diff --git a/Physics_Thesis_Template/bib-refs.bib b/Physics_Thesis_Template/bib-refs.bib index 44fcc23..012b0c5 100644 --- a/Physics_Thesis_Template/bib-refs.bib +++ b/Physics_Thesis_Template/bib-refs.bib @@ -1,3 +1,21 @@ +@misc{koidr25, + +doi = {10.26133/NEA5}, + +url = {https://catcopy.ipac.caltech.edu/dois/doi.php?id=10.26133/NEA19}, + +author = {{NASA Exoplanet Archive}}, + +title = {Kepler Objects of Interest DR25}, + +publisher = {NExScI-Caltech/IPAC}, + +version = {Version: YYYY-MM-DD HH:MM}, + +year = {YYYY} + +} + @INPROCEEDINGS{flare_study_2, author = {{Maehara}, Hiroyuki and {Notsu}, Yuta and {Notsu}, Shota and {Namekata}, Kousuke and {Ikuta}, Kai and {Honda}, Satoshi and {Nogami}, Daisaku and {Shibata}, Kazunari}, title = "{Starspots on late-type stars and their correlation with flare activity}", @@ -631,7 +649,7 @@ archivePrefix = {arXiv}, } @MISC{vizier, - author = { Ochsenbein F. et. al}, + author = {{Ochsenbein F. et. al}}, title = "{ The VizieR database of astronomical catalogues }", doi = {10.26093/cds/vizier}, } diff --git a/Physics_Thesis_Template/content/appendixA.tex b/Physics_Thesis_Template/content/appendixA.tex index 08afb61..d3c1482 100644 --- a/Physics_Thesis_Template/content/appendixA.tex +++ b/Physics_Thesis_Template/content/appendixA.tex @@ -2,17 +2,17 @@ { \centering -\tabcolsep=8pt -\begin{longtable}{llll} -\caption{Table containing all stars used in this study of spectral type M. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The list is sorted first by spectral type, and then by main identifier.} +\tabcolsep=5pt +\begin{longtable}{lclll} +\caption{Table containing all stars of spectra type M for which flares have been found. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The fit type column specifies the used fit types which were found to work best for the lightcurves. The list is sorted first by spectral type, and then by main identifier.} \label{apA:list_of_m_stars}\\ \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endfirsthead \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endhead @@ -21,201 +21,71 @@ \hline\hline \endlastfoot -2MASS J18460555+4332131 & M & TIC 123317330 & KIC 7800087 \\ -2MASS J18472701+4348011 & M & TIC 123410529 & KIC 8007234 \\ -2MASS J18491356+4619042 & M & TIC 123447780 & KIC 9631548 \\ -2MASS J18511354+4227227 & M & TIC 164411695 & KIC 6925256 \\ -2MASS J18511902+4837594 & M & TIC 48216443 & KIC 11069034 \\ -2MASS J18512069+4846013 & M & TIC 48216303 & KIC 11122350 \\ -2MASS J18524238+4828368 & M & TIC 48304549 & KIC 10960823 \\ -2MASS J18525314+4818044 & M & TIC 48304703 & KIC 10905192 \\ -2MASS J18525455+4634012 & M & TIC 164457389 & KIC 9754582 \\ -2MASS J18531060+4050093 & M & TIC 237158804 & KIC 5597695 \\ -2MASS J18535987+4741070 & M & TIC 164525174 & KIC 10452840 \\ -2MASS J18541728+4305206 & M & TIC 164529739 & KIC 7422811 \\ -2MASS J18545269+4107528 & M & TIC 350987684 & KIC 5855808 \\ -2MASS J18561787+4457391 & M & TIC 164670879 & KIC 8737443 \\ -2MASS J18565158+4448162 & M & TIC 164671055 & KIC 8673358 \\ -2MASS J18570619+4516101 & M & TIC 164677934 & KIC 8935942 \\ -2MASS J18572876+4035369 & M & TIC 120251682 & KIC 5342558 \\ -2MASS J18574689+4115593 & M & TIC 120254207 & KIC 5941226 \\ -2MASS J18592859+4351465 & M & TIC 164786997 & KIC 8012943 \\ -2MASS J19000393+4109460 & M & TIC 120419969 & KIC 5858361 \\ -2MASS J19001025+4045358 & M & TIC 120422710 & KIC 5515142 \\ -2MASS J19005916+4400190 & M & TIC 164889286 & KIC 8150479 \\ -2MASS J19011064+4206175 & M & TIC 164886887 & KIC 6672948 \\ -2MASS J19011256+4152067 & M & TIC 399822429 & KIC 6425989 \\ -2MASS J19020142+4110533 & M & TIC 120576193 & KIC 5859365 \\ -2MASS J19023480+4539052 & M & TIC 352013620 & KIC 9205855 \\ -2MASS J19024516+4429007 & M & TIC 352012319 & KIC 8417053 \\ -2MASS J19030585+4046008 & M & TIC 120579026 & KIC 5516671 \\ -2MASS J19033576+3941263 & M & TIC 120684614 & KIC 4544623 \\ -2MASS J19034709+4317208 & M & TIC 158166384 & KIC 7592133 \\ -2MASS J19035284+4338273 & M & TIC 158165866 & KIC 7877209 \\ -2MASS J19041026+4530403 & M & TIC 158172860 & KIC 9142714 \\ -2MASS J19053703+4235308 & M & TIC 158218091 & KIC 7018323 \\ -2MASS J19061507+5029221 & M & TIC 399825094 & KIC 12004872 \\ -2MASS J19061662+4502422 & M & TIC 158274889 & KIC 8807085 \\ -2MASS J19063685+4928043 & M & TIC 399825963 & KIC 11498106 \\ -2MASS J19064350+5020087 & M & TIC 399825217 & KIC 11955208 \\ -2MASS J19064648+4931162 & M & TIC 399825921 & KIC 11550428 \\ -2MASS J19074075+3752413 & M & TIC 121022434 & KIC 2557669 \\ -2MASS J19081745+3902346 & M & TIC 121085753 & KIC 3940372 \\ -2MASS J19083962+4221137 & M & TIC 158388172 & KIC 6849112 \\ -2MASS J19085407+4320395 & M & TIC 158423632 & KIC 7670700 \\ -2MASS J19103260+4322147 & M & TIC 158551504 & KIC 7671594 \\ -2MASS J19104382+4039368 & M & TIC 121329525 & KIC 5435958 \\ -2MASS J19110814+4024571 & M & TIC 121333779 & KIC 5262561 \\ -2MASS J19114749+4048205 & M & TIC 121461193 & KIC 5608002 \\ -2MASS J19130891+5127421 & M & TIC 298961665 & KIC 12505054 \\ -2MASS J19135561+4319299 & M & TIC 158725435 & KIC 7673428 \\ -2MASS J19141052+4559479 & M & TIC 158787568 & KIC 9396972 \\ -2MASS J19143720+4243450 & M & TIC 158795349 & KIC 7190459 \\ -2MASS J19152845+5001374 & M & TIC 299088298 & KIC 11808734 \\ -2MASS J19160242+4726491 & M & TIC 158983853 & KIC 10332732 \\ -2MASS J19170322+4953087 & M & TIC 299159305 & KIC 11708034 \\ -2MASS J19200001+3844383 & M & TIC 122225323 & KIC 3640527 \\ -2MASS J19200978+4954168 & M & TIC 267747418 & KIC 11760021 \\ -2MASS J19205088+5018194 & M & TIC 406950619 & KIC 11961075 \\ -2MASS J19210354+4523201 & M & TIC 159303166 & KIC 9017693 \\ -2MASS J19213187+4459115 & M & TIC 159387244 & KIC 8749769 \\ -2MASS J19230963+3739397 & M & TIC 122672447 & KIC 2300039 \\ -2MASS J19232149+5107053 & M & TIC 417655942 & KIC 12356051 \\ -2MASS J19233077+5035350 & M & TIC 417656504 & KIC 12060710 \\ -2MASS J19233788+4518061 & M & TIC 159520226 & KIC 9019435 \\ -2MASS J19240851+3747169 & M & TIC 122781970 & KIC 2441562 \\ -2MASS J19242752+5106364 & M & TIC 350738203 & KIC 12356489 \\ -2MASS J19255059+4532219 & M & TIC 159761686 & KIC 9153754 \\ -2MASS J19291103+4821243 & M & TIC 424864617 & KIC 10921009 \\ -2MASS J19304396+4112528 & M & TIC 137759349 & KIC 5962956 \\ -2MASS J19304840+4142454 & M & TIC 137758161 & KIC 6366739 \\ -2MASS J19335656+4010546 & M & - & KIC 5016904 \\ -2MASS J19343395+4137235 & M & TIC 138222062 & KIC 6290811 \\ -2MASS J19353467+3943573 & M & TIC 138436033 & KIC 4662431 \\ -2MASS J19353874+4708324 & M & TIC 270790828 & KIC 10146539 \\ -2MASS J19365745+4628121 & M & TIC 270957843 & KIC 9716117 \\ -2MASS J19374745+4341098 & M & TIC 271047224 & KIC 7898781 \\ -2MASS J19421615+4928069 & M & TIC 27531488 & KIC 11515276 \\ -2MASS J19423900+5108356 & M & TIC 27639064 & KIC 12365719 \\ -2MASS J19433653+4758149 & M & TIC 27645448 & KIC 10676126 \\ -2MASS J19443380+4843497 & M & TIC 27770198 & KIC 11147271 \\ -2MASS J19444493+4720327 & M & TIC 272279258 & KIC 10285642 \\ -2MASS J19450930+4754591 & M & TIC 27771932 & KIC 10677397 \\ -2MASS J19451164+4345265 & M & TIC 272270363 & KIC 7973675 \\ -2MASS J19454134+3906345 & M & TIC 184471264 & KIC 4077867 \\ -2MASS J19471875+4123248 & M & TIC 239228371 & KIC 6060845 \\ -2MASS J19471987+4747258 & M & TIC 272841049 & KIC 10548508 \\ -2MASS J19480997+4310160 & M & TIC 272943707 & KIC 7547969 \\ -2MASS J19503771+4705359 & M & TIC 273378083 & KIC 10091786 \\ -2MASS J19503804+4041450 & M & TIC 169816129 & KIC 5471468 \\ -2MASS J19505785+4630250 & M & TIC 273379615 & KIC 9786877 \\ -2MASS J19510637+4505045 & M & TIC 273383619 & KIC 8836388 \\ -2MASS J19525571+4743328 & M & TIC 273874034 & KIC 10553513 \\ -2MASS J19542833+4420425 & M & TIC 268158580 & KIC 8387621 \\ -2MASS J19543981+4814406 & M & TIC 264508845 & KIC 10880514 \\ -2MASS J19550625+4009192 & M & TIC 171101426 & KIC 5041192 \\ -2MASS J19553603+4805356 & M & TIC 416528859 & KIC 10753072 \\ -2MASS J19561258+4335485 & M & TIC 268485803 & KIC 7847566 \\ -2MASS J19584764+4711122 & M & TIC 269029909 & KIC 10165815 \\ -2MASS J20000387+4531405 & M & TIC 239234887 & KIC 9179906 \\ -ATO J285.1153+45.7850 & M & TIC 164882037 & KIC 9267818 \\ -KOI-1654 & M & TIC 48355200 & KIC 11546211 \\ -UCAC4 639-062929 & M & TIC 120963868 & KIC 2284919 \\ -UCAC4 643-073385 & M & TIC 138647610 & KIC 3454793 \\ -UCAC4 651-066418 & M & TIC 120354289 & KIC 4904647 \\ -UCAC4 661-082974 & M & TIC 268288304 & KIC 6720765 \\ -UCAC4 664-071715 & M & TIC 158430593 & KIC 7104739 \\ -UCAC4 668-073165 & M & TIC 158432884 & KIC 7741987 \\ -UCAC4 683-066189 & M & TIC 351897570 & KIC 9692206 \\ -UCAC4 707-062317 & M & TIC 299097784 & KIC 12403318 \\ -1RXS J060224.9-163451 & M0 & TIC 95328477 & - \\ -V* MY Tau & M0.5e & TIC 348638763 & - \\ -WOH S 209 & M0: & TIC 179038379 & - \\ -Kepler-210 & M0V & TIC 63283780 & KIC 7447200 \\ -MCC 428 & M0V & TIC 434136638 & - \\ -V* HK Aqr & M0Ve & TIC 5656273 & - \\ -HG 7-26 & M1 & TIC 345454031 & - \\ -V* OT Ser & M1.0V & TIC 355793860 & - \\ -V* V631 Tau & M1.5 & TIC 348638813 & - \\ -2MASS J18563342+4513481 & M1.5V & TIC 164670606 & KIC 8935655 \\ -G 6-33 & M1.5V & TIC 434160946 & - \\ -V* FF And & M1Ve+M1Ve & TIC 267802440 & - \\ -HD 197481 & M1VeBa1 & TIC 441420236 & - \\ -{[LM84]} 3-13 & M2 & TIC 165124012 & - \\ -V* AX Cnc & M2.0 & TIC 175233993 & - \\ -2MASS J19412234+5104273 & M2.1 & TIC 27454242 & KIC 12314646 \\ -1RXS J004211.1-425245 & M2.2 & TIC 80427281 & - \\ -2MASS J04133314-5231586 & M2.4 & TIC 219229275 & - \\ -PM J19399+3950 & M2.5 & TIC 138893136 & KIC 4758595 \\ -UCAC4 647-065171 & M2.5 & TIC 121215155 & KIC 4142890 \\ -G 10-29 & M2.5V & TIC 396951485 & - \\ -LP 474-124 & M2.5V & TIC 348663808 & - \\ -2MASS J19130537+5020559 & M2.5Ve & TIC 298962893 & KIC 11957647 \\ -ASAS J232857-6802.4 & M2.5Ve & TIC 229807000 & - \\ -2MASS J19324802+4200580 & M2.7 & TIC 275496670 & KIC 6610837 \\ -2MASS J19445931+4812415 & M2.8 & TIC 27772498 & KIC 10872868 \\ -V* V497 Tau & M2.9 & TIC 258032026 & - \\ -CD-51 13128 & M2Ve & TIC 140045538 & - \\ -2MASS J19183060+4153031 & M3 & TIC 122067236 & KIC 6436291 \\ -{[PS78]} 219 & M3+ & TIC 11652986 & - \\ -UCAC4 698-065839 & M3.0 & TIC 48504458 & KIC 11495571 \\ -G 9-11 & M3.0V & TIC 21246336 & - \\ -UCAC4 673-078334 & M3.0Ve & TIC 272272592 & KIC 8507979 \\ -G 209-3 & M3.4 & TIC 28231379 & KIC 10877432 \\ -V* LT Tau & M3.5 & TIC 258067389 & - \\ -BD-15 6290 & M3.5V & TIC 188580272 & - \\ -LP 426-35 & M3.5V & TIC 197247983 & - \\ -LP 737-14 & M3.5V & TIC 335628483 & - \\ -2MASS J22371494-2622332 & M3.5Ve & TIC 326446019 & - \\ -BD+16 2708 & M3V & TIC 258105174 & - \\ -KOI-256 & M3V & TIC 48528261 & KIC 11548140 \\ -LAMOST J192817.82+410412.2 & M3V & TIC 137410897 & KIC 5791720 \\ -2MASS J18535530+4310389 & M3Ve & TIC 164529625 & KIC 7505644 \\ -2MASS J18592696+4548446 & M3Ve & TIC 164784762 & KIC 9328653 \\ -2MASS J19015564+4134218 & M3Ve & TIC 120576760 & KIC 6187812 \\ -CD-43 9546 & M3Ve & TIC 334524122 & - \\ -CD-56 1032A & M3Ve & TIC 220433363 & - \\ -2MASS J04534379-5836247 & M3e & TIC 220432563 & - \\ -2MASS J22534969-1721358 & M4 & TIC 188586529 & - \\ -LP 873-37 & M4 & TIC 99566892 & - \\ -1RXS J185504.7+425952 & M4.0V & TIC 164644375 & KIC 7341653 \\ -HG 8-80 & M4.0V & TIC 435916078 & - \\ -V* EV Lac & M4.0Ve & TIC 154101678 & - \\ -2MASS J01275875-6032243 & M4.2 & TIC 237910557 & - \\ -2MASS J19150930+5101139 & M4.5V & TIC 299089441 & KIC 12302994 \\ -2MASS J19573917+4554182 & M4.5V & TIC 268711231 & KIC 9426508 \\ -G 6-7 & M4.5V & TIC 456938518 & - \\ -UCAC4 683-069625 & M4.5V & TIC 159171299 & KIC 9705079 \\ -2MASS J18432784+4727325 & M4Ve & TIC 123205792 & KIC 10318386 \\ -2MASS J18474286+4218039 & M4Ve & TIC 123408865 & KIC 6837702 \\ -2MASS J18535193+4327449 & M4Ve & TIC 164529313 & KIC 7734382 \\ -2MASS J19005766+4428279 & M4Ve & TIC 164889852 & KIC 8416220 \\ -2MASS J19045588+3738361 & M4Ve & TIC 120825083 & KIC 2283749 \\ -CD-56 1032B & M4Ve & TIC 220433364 & - \\ -Kepler-1646 & M4Ve & TIC 158552258 & KIC 7350067 \\ -2MASS J21484123-4736506 & M5 & TIC 147421845 & - \\ -UCAC3 53-724 & M5.5V & TIC 425937691 & - \\ -G 205-40 & M5V & TIC 164458193 & KIC 9201463 \\ -LP 357-206 & M5e & TIC 14079970 & - \\ -LP 760-3 & M6.5V & - & - \\ -2MASS J19202351+5037161 & M6Ve & TIC 267746625 & KIC 12108566 \\ -V* V692 Tau & M: & TIC 149923415 & - \\ +2MASS J18565158+4448162 & M & TIC 164671055 & KIC 8673358 & sine \\ +2MASS J18570619+4516101 & M & TIC 164677934 & KIC 8935942 & sine \\ +2MASS J18572876+4035369 & M & TIC 120251682 & KIC 5342558 & sine \\ +2MASS J19023480+4539052 & M & TIC 352013620 & KIC 9205855 & sine \\ +2MASS J19061662+4502422 & M & TIC 158274889 & KIC 8807085 & sine \\ +2MASS J19074075+3752413 & M & TIC 121022434 & KIC 2557669 & sine \\ +2MASS J19230963+3739397 & M & TIC 122672447 & KIC 2300039 & sine \\ +2MASS J19255059+4532219 & M & TIC 159761686 & KIC 9153754 & sine \\ +2MASS J19421615+4928069 & M & TIC 27531488 & KIC 11515276 & sine \\ +UCAC4 643-073385 & M & TIC 138647610 & KIC 3454793 & sine \\ +1RXS J060224.9-163451 & M0 & TIC 95328477 & - & sine \\ +V* MY Tau & M0.5e & TIC 348638763 & - & sine \\ +WOH S 209 & M0: & TIC 179038379 & - & sine \\ +V* HK Aqr & M0Ve & TIC 5656273 & - & sine \\ +V* OT Ser & M1.0V & TIC 355793860 & - & sine, poly \\ +V* V631 Tau & M1.5 & TIC 348638813 & - & sine \\ +2MASS J18563342+4513481 & M1.5V & TIC 164670606 & KIC 8935655 & sine \\ +V* FF And & M1Ve+M1Ve & TIC 267802440 & - & sine \\ +{[LM84]} 3-13 & M2 & TIC 165124012 & - & sine \\ +V* AX Cnc & M2.0 & TIC 175233993 & - & sine, poly \\ +1RXS J004211.1-425245 & M2.2 & TIC 80427281 & - & sine \\ +2MASS J04133314-5231586 & M2.4 & TIC 219229275 & - & sine \\ +G 10-29 & M2.5V & TIC 396951485 & - & sine \\ +ASAS J232857-6802.4 & M2.5Ve & TIC 229807000 & - & sine \\ +V* V497 Tau & M2.9 & TIC 258032026 & - & sine \\ +CD-51 13128 & M2Ve & TIC 140045538 & - & sine \\ +UCAC4 698-065839 & M3.0 & TIC 48504458 & KIC 11495571 & sine \\ +G 9-11 & M3.0V & TIC 21246336 & - & sine \\ +G 209-3 & M3.4 & TIC 28231379 & KIC 10877432 & sine \\ +V* LT Tau & M3.5 & TIC 258067389 & - & sine \\ +BD-15 6290 & M3.5V & TIC 188580272 & - & sine \\ +2MASS J22371494-2622332 & M3.5Ve & TIC 326446019 & - & sine \\ +KOI-256 & M3V & TIC 48528261 & KIC 11548140 & sine \\ +LAMOST J192817.82+410412.2 & M3V & TIC 137410897 & KIC 5791720 & sine \\ +CD-56 1032A & M3Ve & TIC 220433363 & - & sine \\ +2MASS J04534379-5836247 & M3e & TIC 220432563 & - & sine \\ +1RXS J185504.7+425952 & M4.0V & TIC 164644375 & KIC 7341653 & sine \\ +HG 8-80 & M4.0V & TIC 435916078 & - & sine \\ +V* EV Lac & M4.0Ve & TIC 154101678 & - & sine \\ +2MASS J01275875-6032243 & M4.2 & TIC 237910557 & - & sine \\ +G 6-7 & M4.5V & TIC 456938518 & - & sine \\ +2MASS J19005766+4428279 & M4Ve & TIC 164889852 & KIC 8416220 & sine \\ +CD-56 1032B & M4Ve & TIC 220433364 & - & sine \\ +Kepler-1646 & M4Ve & TIC 158552258 & KIC 7350067 & sine \\ +2MASS J21484123-4736506 & M5 & TIC 147421845 & - & sine \\ +UCAC3 53-724 & M5.5V & TIC 425937691 & - & sine \\ +G 205-40 & M5V & TIC 164458193 & KIC 9201463 & sine \\ +LP 357-206 & M5e & TIC 14079970 & - & sine \\ +V* V692 Tau & M: & TIC 149923415 & - & sine \\ \end{longtable} } { \centering -\tabcolsep=8pt -\begin{longtable}{llll} -\caption{Table containing all stars used in this study of spectral type K. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The list is sorted first by spectral type, and then by main identifier.} +\tabcolsep=5pt +\begin{longtable}{lclll} +\caption{Table containing all stars of spectra type K for which flares have been found. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The fit type column specifies the used fit types which were found to work best for the lightcurves. The list is sorted first by spectral type, and then by main identifier.} \label{apA:list_of_k_stars}\\ \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endfirsthead \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endhead @@ -224,61 +94,43 @@ V* V692 Tau & M: & TIC 149923415 & - \\ \hline\hline \endlastfoot -1RXS J064643.6-770027 & K & TIC 177255827 & - \\ -2MASS J18524052+4156057 & K & - & KIC 6500181 \\ -2MASS J18534407+4208274 & K & - & KIC 6668646 \\ -2MASS J18535462+4135227 & K & - & KIC 6183672 \\ -2MASS J19004200+3903124 & K & TIC 399794444 & KIC 3935803 \\ -2MASS J19082791+4337114 & K & TIC 158389986 & KIC 7879384 \\ -2MASS J19324909+4229041 & K & TIC 275495685 & KIC 6953069 \\ -2MASS J19404949+5046469 & K & TIC 27398219 & KIC 12166457 \\ -ATO J296.1841+42.6311 & K & TIC 272184059 & KIC 7133807 \\ -CPD-19 878 & K & TIC 93125144 & - \\ -KOI-7449 & K & TIC 279918401 & KIC 11495989 \\ -KOI-8047 & K & TIC 290034561 & KIC 11294822 \\ -Kepler-1259 & K & TIC 273592350 & KIC 10028535 \\ -Kepler-1782 & K & TIC 123202646 & KIC 8142942 \\ -Kepler-1856 & K & TIC 27687265 & KIC 12469800 \\ -Kepler-1966 & K & TIC 137627194 & KIC 5962262 \\ -Kepler-246 & K & TIC 272484980 & KIC 7134976 \\ -Kepler-693 & K & TIC 237159318 & KIC 5164255 \\ -PM J07058-5848 & K & TIC 279615427 & - \\ -TYC 1360-957-1 & K & TIC 247117382 & - \\ -HD 245924 & K0IV & TIC 19934471 & - \\ -2MASS J19200703+4335050 & K0V & TIC 159220196 & KIC 7816999 \\ -BD+41 3306 & K0V & TIC 394172596 & KIC 6278762 \\ -CD-26 1578 & K0V & TIC 44797824 & - \\ -TYC 553-33-1 & K0V:e & TIC 405405298 & - \\ -RX J1925.0+4429 & K1V & TIC 159721038 & KIC 8429280 \\ -V* V4371 Sgr & K1V & TIC 151839506 & - \\ -HD 215341 & K1Ve & TIC 145752454 & - \\ -TYC 582-114-1 & K1Ve & TIC 344163180 & - \\ -V* LQ Hya & K1Vp & TIC 46907042 & - \\ -Kepler-1558 & K2 & TIC 158322085 & KIC 10000941 \\ -HD 283750 & K2.5Ve & TIC 125838647 & - \\ -CD-52 381 & K2V(e) & TIC 229151691 & - \\ -V* V471 Tau & K2V+DA & TIC 456863710 & - \\ -Kepler-411 & K3V & TIC 399954349 & KIC 11551692 \\ -BD-13 6131 & K3Ve & TIC 437696706 & - \\ -V* BY Dra & K4Ve+K7.5Ve & TIC 47579336 & - \\ -2MASS J19400800+4923036 & K5 & TIC 27390487 & KIC 11461764 \\ -V* CC Eri & K7V & TIC 142206123 & - \\ +1RXS J064643.6-770027 & K & TIC 177255827 & - & sine \\ +2MASS J19404949+5046469 & K & TIC 27398219 & KIC 12166457 & sine \\ +CPD-19 878 & K & TIC 93125144 & - & sine \\ +Kepler-693 & K & TIC 237159318 & KIC 5164255 & sine \\ +PM J07058-5848 & K & TIC 279615427 & - & sine \\ +TYC 1360-957-1 & K & TIC 247117382 & - & sine \\ +HD 245924 & K0IV & TIC 19934471 & - & sine \\ +CD-26 1578 & K0V & TIC 44797824 & - & sine \\ +TYC 553-33-1 & K0V:e & TIC 405405298 & - & sine \\ +RX J1925.0+4429 & K1V & TIC 159721038 & KIC 8429280 & sine \\ +HD 215341 & K1Ve & TIC 145752454 & - & sine \\ +TYC 582-114-1 & K1Ve & TIC 344163180 & - & sine \\ +V* LQ Hya & K1Vp & TIC 46907042 & - & sine \\ +Kepler-1558 & K2 & TIC 158322085 & KIC 10000941 & sine \\ +HD 283750 & K2.5Ve & TIC 125838647 & - & sine \\ +CD-52 381 & K2V(e) & TIC 229151691 & - & sine \\ +V* V471 Tau & K2V+DA & TIC 456863710 & - & sine \\ +Kepler-411 & K3V & TIC 399954349 & KIC 11551692 & sine \\ +BD-13 6131 & K3Ve & TIC 437696706 & - & sine \\ +V* BY Dra & K4Ve+K7.5Ve & TIC 47579336 & - & sine \\ +V* CC Eri & K7V & TIC 142206123 & - & sine \\ \end{longtable} } { \centering -\tabcolsep=8pt -\begin{longtable}{llll} -\caption{Table containing all stars used in this study of spectral type G. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The list is sorted first by spectral type, and then by main identifier.} +\tabcolsep=5pt +\begin{longtable}{lclll} +\caption{Table containing all stars of spectra type G for which flares have been found. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The fit type column specifies the used fit types which were found to work best for the lightcurves. The list is sorted first by spectral type, and then by main identifier.} \label{apA:list_of_g_stars}\\ \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endfirsthead \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endhead @@ -287,100 +139,43 @@ V* CC Eri & K7V & TIC 142206123 & - \\ \hline\hline \endlastfoot -2MASS J18425375+4345336 & G & TIC 123198563 & KIC 7936748 \\ -2MASS J18495232+4309276 & G & TIC 123489639 & KIC 7503439 \\ -2MASS J18525868+4530560 & G & TIC 164458315 & KIC 9137611 \\ -2MASS J18582492+4446498 & G & TIC 164779298 & KIC 8609289 \\ -2MASS J19012927+4104159 & G & TIC 120496415 & KIC 5773205 \\ -2MASS J19043346+4427484 & G & TIC 158171605 & KIC 8417863 \\ -2MASS J19061691+4654395 & G & TIC 158272786 & KIC 10000509 \\ -2MASS J19065549+3937268 & G & TIC 121012476 & KIC 4546541 \\ -2MASS J19080680+4450500 & G & TIC 158391683 & KIC 8678334 \\ -2MASS J19100183+4257041 & G & TIC 158552191 & KIC 7350021 \\ -2MASS J19182441+4439465 & G & TIC 159097797 & KIC 8554173 \\ -2MASS J19184939+4418233 & G & TIC 159107064 & KIC 8359762 \\ -2MASS J19185028+4633324 & G & TIC 159171504 & KIC 9765670 \\ -2MASS J19250540+3734332 & G & TIC 137097085 & KIC 2159377 \\ -2MASS J19280249+3911165 & G & TIC 137402956 & KIC 4058829 \\ -2MASS J19283146+3837123 & G & TIC 137484235 & KIC 3547283 \\ -2MASS J19313155+4628249 & G & TIC 63452929 & KIC 9712781 \\ -2MASS J19320792+3933052 & G & TIC 137972488 & KIC 4469481 \\ -2MASS J19350077+4608423 & G & TIC 270698467 & KIC 9531002 \\ -2MASS J19354814+4118464 & G & TIC 138431713 & KIC 6049426 \\ -2MASS J19354900+4623499 & G & TIC 270789534 & KIC 9654338 \\ -2MASS J19364457+4403341 & G & TIC 270859571 & KIC 8172597 \\ -2MASS J19370439+4626209 & G & TIC 270957778 & KIC 9716208 \\ -2MASS J19390861+4046149 & G & TIC 138725759 & KIC 5544024 \\ -2MASS J19395042+4622296 & G & TIC 271354512 & KIC 9657062 \\ -2MASS J19415575+4522369 & G & TIC 271664690 & KIC 9032578 \\ -2MASS J19450785+5108395 & G & TIC 27778260 & KIC 12367153 \\ -2MASS J19484658+5002007 & G & TIC 28084005 & KIC 11825619 \\ -2MASS J19491761+4638356 & G & TIC 273131067 & KIC 9845711 \\ -2MASS J19535154+4211197 & G & TIC 274119294 & KIC 6719122 \\ -2MASS J19551628+4145582 & G & TIC 171093514 & KIC 6390935 \\ -2MASS J19553242+4737586 & G & TIC 268382866 & KIC 10491422 \\ -2MASS J19562459+4408276 & G & TIC 268606798 & KIC 8257716 \\ -2MASS J19572618+4520510 & G & TIC 268712881 & KIC 9048032 \\ -2MASS J19583564+4352320 & G & TIC 269121724 & KIC 8055957 \\ -2MASS J20060991+4417004 & G & TIC 185335830 & KIC 8332459 \\ -ATO J285.5682+44.5725 & G & TIC 352012409 & KIC 8481574 \\ -BD-08 995 & G & TIC 43472154 & - \\ -KOI-1747 & G & TIC 159717069 & KIC 7032421 \\ -KOI-2324 & G & TIC 159105557 & KIC 7746958 \\ -KOI-5796 & G & TIC 63070665 & KIC 10470779 \\ -KOI-5810 & G & TIC 123494489 & KIC 10581308 \\ -KOI-5825 & G & TIC 27183790 & KIC 10737437 \\ -KOI-5952 & G & TIC 27845077 & KIC 12071775 \\ -KOI-741 & G & TIC 272840512 & KIC 10418797 \\ -Kepler-1060 & G & TIC 120691237 & KIC 4544907 \\ -Kepler-1198 & G & TIC 158843826 & KIC 8681734 \\ -Kepler-1839 & G & TIC 27082730 & KIC 11818607 \\ -Kepler-513 & G & TIC 48503953 & KIC 11802615 \\ -Kepler-725 & G & TIC 164652841 & KIC 8672910 \\ -Kepler-739 & G & TIC 159225155 & KIC 9766437 \\ -TYC 4595-107-1 & G & TIC 394030788 & - \\ -UCAC4 640-067417 & G & TIC 122517231 & KIC 2709412 \\ -UCAC4 686-075120 & G & TIC 269030397 & KIC 10098932 \\ -V* V452 Lyr & G & - & KIC 7742289 \\ -BD-01 2318 & G0 & TIC 78234015 & - \\ -HD 295290 & G0 & TIC 53417036 & - \\ -TYC 3560-458-1 & G0 & TIC 26815845 & KIC 10922836 \\ -TYC 3557-1509-1 & G0.5V & TIC 273379797 & KIC 9726613 \\ -TYC 3139-951-1 & G0V & TIC 138215507 & KIC 4660797 \\ -Kepler-1424 & G1.5Vb & TIC 122706631 & KIC 5096590 \\ -KOI-6202 & G1V & TIC 164669854 & KIC 9389245 \\ -Kepler-400 & G2V & TIC 122707140 & KIC 5272233 \\ -TYC 3131-2137-1 & G2V & TIC 164460243 & KIC 7871914 \\ -TYC 3146-672-1 & G2V & TIC 159448893 & KIC 7523785 \\ -TYC 3545-2661-1 & G2V & TIC 399827121 & KIC 10850420 \\ -HD 183473 & G5 & TIC 63120335 & KIC 7201012 \\ -HD 214261 & G5 & TIC 200501090 & - \\ -KOI-644 & G5 & TIC 122138452 & KIC 5356593 \\ -TYC 3550-241-1 & G5 & TIC 299088815 & KIC 12008308 \\ -HD 23524 & G5V & TIC 428761512 & - \\ -TYC 3562-2088-1 & G5V & TIC 273872314 & KIC 10093680 \\ -V* AG Lep & G5V & TIC 92845906 & - \\ -HD 222259A & G6V & TIC 410214986 & - \\ -Kepler-605 & G7 & TIC 158423850 & KIC 7595157 \\ -TYC 3128-2312-1 & G8V & TIC 120686876 & KIC 5944209 \\ -HD 180445 & G8V(e) & TIC 97914505 & - \\ -HD 220186 & G9Ve & TIC 49619607 & - \\ +2MASS J18425375+4345336 & G & TIC 123198563 & KIC 7936748 & sine \\ +2MASS J19061691+4654395 & G & TIC 158272786 & KIC 10000509 & sine \\ +2MASS J19320792+3933052 & G & TIC 137972488 & KIC 4469481 & sine \\ +2MASS J19553242+4737586 & G & TIC 268382866 & KIC 10491422 & sine \\ +2MASS J20060991+4417004 & G & TIC 185335830 & KIC 8332459 & sine \\ +ATO J285.5682+44.5725 & G & TIC 352012409 & KIC 8481574 & sine \\ +BD-08 995 & G & TIC 43472154 & - & sine \\ +Kepler-725 & G & TIC 164652841 & KIC 8672910 & sine \\ +TYC 4595-107-1 & G & TIC 394030788 & - & sine \\ +V* V452 Lyr & G & - & KIC 7742289 & sine \\ +BD-01 2318 & G0 & TIC 78234015 & - & sine \\ +HD 295290 & G0 & TIC 53417036 & - & sine \\ +TYC 3146-672-1 & G2V & TIC 159448893 & KIC 7523785 & sine \\ +HD 214261 & G5 & TIC 200501090 & - & sine \\ +KOI-644 & G5 & TIC 122138452 & KIC 5356593 & sine \\ +HD 23524 & G5V & TIC 428761512 & - & sine \\ +V* AG Lep & G5V & TIC 92845906 & - & sine \\ +HD 222259A & G6V & TIC 410214986 & - & sine \\ +Kepler-605 & G7 & TIC 158423850 & KIC 7595157 & sine, poly \\ +HD 180445 & G8V(e) & TIC 97914505 & - & sine \\ +HD 220186 & G9Ve & TIC 49619607 & - & sine \\ \end{longtable} } { \centering -\tabcolsep=8pt -\begin{longtable}{llll} -\caption{Table containing all stars used in this study of spectral type F. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The list is sorted first by spectral type, and then by main identifier.} +\tabcolsep=5pt +\begin{longtable}{lclll} +\caption{Table containing all stars of spectra type F for which flares have been found. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The fit type column specifies the used fit types which were found to work best for the lightcurves. The list is sorted first by spectral type, and then by main identifier.} \label{apA:list_of_f_stars}\\ \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endfirsthead \hline\hline -\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Spectral Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} \\ +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ \hline \endhead @@ -389,18 +184,614 @@ HD 220186 & G9Ve & TIC 49619607 & - \\ \hline\hline \endlastfoot -2MASS J18491671+4410445 & F & TIC 123449867 & KIC 8212826 \\ -KOI-4698 & F & TIC 159643077 & KIC 10663738 \\ -Kepler-1271 & F & TIC 120825510 & KIC 1996180 \\ -Kepler-1443 & F & TIC 164525743 & KIC 10057494 \\ -Kepler-380 & F & TIC 48132154 & KIC 11121752 \\ -Kepler-494 & F & TIC 169176556 & KIC 6305192 \\ -TYC 3134-301-1 & F & TIC 137483286 & KIC 3852772 \\ -KOI-19 & F3/F5V & TIC 123201406 & KIC 7255336 \\ -TYC 3557-727-1 & F3/F5V & TIC 273684688 & KIC 9788113 \\ -TYC 3140-1658-1 & F5 & TIC 138967825 & KIC 5802601 \\ -TYC 3557-1501-1 & F6IV & TIC 273043859 & KIC 9724820 \\ -KOI-44 & F7IV & TIC 239276046 & KIC 8845026 \\ -Kepler-1084 & F8V & TIC 267749737 & KIC 10857519 \\ +Kepler-380 & F & TIC 48132154 & KIC 11121752 & sine \\ +KOI-19 & F3/F5V & TIC 123201406 & KIC 7255336 & sine \\ +TYC 3557-1501-1 & F6IV & TIC 273043859 & KIC 9724820 & sine \\ +Kepler-1084 & F8V & TIC 267749737 & KIC 10857519 & sine \\ +\end{longtable} +} + +{ +\centering +\tabcolsep=5pt +\begin{longtable}{lclll} +\caption{Table containing all stars which where analysed. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The list is sorted first by spectral type, and then by main identifier.} +\label{apA:list_of_unused_stars}\\ +\hline\hline +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ +\hline +\endfirsthead + +\hline\hline +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ +\hline +\endhead + +\hline +\endfoot + +\hline\hline +\endlastfoot +HD 225391 & A & TIC 139156518 & KIC 5632093 & sine \\ +HD 226712 & A & TIC 171882897 & KIC 5905878 & sine \\ +TYC 3125-2237-1 & A & TIC 121274152 & KIC 4641547 & sine \\ +HD 187141 & A0 & TIC 360021868 & KIC 6381306 & sine \\ +HD 188360 & A0 & TIC 28359846 & KIC 10815604 & sine \\ +HD 177982 & A2 & TIC 120821069 & KIC 4995049 & sine \\ +HD 225493 & A4V & TIC 184163024 & KIC 5201872 & sine \\ +TYC 3551-561-1 & A5IV & TIC 26418553 & KIC 11296464 & sine \\ +HD 225333 & A5V & TIC 139037071 & KIC 3458671 & sine \\ +AG+46 1529 & A7III & TIC 273380253 & KIC 9604762 & sine \\ +TYC 3560-1923-1 & A9IV–V & TIC 271167267 & KIC 10281360 & sine \\ +TYC 3565-514-1 & A9V & TIC 27458214 & KIC 11197934 & sine \\ +KOI-3818 & B9.5Vn & TIC 159102838 & KIC 6515722 & sine \\ +2MASS J18491671+4410445 & F & TIC 123449867 & KIC 8212826 & sine \\ +KOI-4698 & F & TIC 159643077 & KIC 10663738 & sine \\ +Kepler-1271 & F & TIC 120825510 & KIC 1996180 & sine \\ +Kepler-1443 & F & TIC 164525743 & KIC 10057494 & sine \\ +Kepler-494 & F & TIC 169176556 & KIC 6305192 & sine \\ +TYC 3134-301-1 & F & TIC 137483286 & KIC 3852772 & sine \\ +TYC 3557-727-1 & F3/F5V & TIC 273684688 & KIC 9788113 & sine \\ +TYC 3140-1658-1 & F5 & TIC 138967825 & KIC 5802601 & sine \\ +KOI-44 & F7IV & TIC 239276046 & KIC 8845026 & sine \\ +2MASS J18495232+4309276 & G & TIC 123489639 & KIC 7503439 & \\ +2MASS J18525868+4530560 & G & TIC 164458315 & KIC 9137611 & sine \\ +2MASS J18582492+4446498 & G & TIC 164779298 & KIC 8609289 & sine \\ +2MASS J19012927+4104159 & G & TIC 120496415 & KIC 5773205 & sine \\ +2MASS J19043346+4427484 & G & TIC 158171605 & KIC 8417863 & sine \\ +2MASS J19065549+3937268 & G & TIC 121012476 & KIC 4546541 & sine \\ +2MASS J19080680+4450500 & G & TIC 158391683 & KIC 8678334 & sine \\ +2MASS J19100183+4257041 & G & TIC 158552191 & KIC 7350021 & sine \\ +2MASS J19182441+4439465 & G & TIC 159097797 & KIC 8554173 & sine \\ +2MASS J19184939+4418233 & G & TIC 159107064 & KIC 8359762 & sine \\ +2MASS J19185028+4633324 & G & TIC 159171504 & KIC 9765670 & sine \\ +2MASS J19250540+3734332 & G & TIC 137097085 & KIC 2159377 & sine \\ +2MASS J19280249+3911165 & G & TIC 137402956 & KIC 4058829 & sine, poly \\ +2MASS J19283146+3837123 & G & TIC 137484235 & KIC 3547283 & sine \\ +2MASS J19313155+4628249 & G & TIC 63452929 & KIC 9712781 & sine \\ +2MASS J19350077+4608423 & G & TIC 270698467 & KIC 9531002 & sine \\ +2MASS J19354814+4118464 & G & TIC 138431713 & KIC 6049426 & sine \\ +2MASS J19354900+4623499 & G & TIC 270789534 & KIC 9654338 & sine \\ +2MASS J19364457+4403341 & G & TIC 270859571 & KIC 8172597 & sine \\ +2MASS J19370439+4626209 & G & TIC 270957778 & KIC 9716208 & sine \\ +2MASS J19390861+4046149 & G & TIC 138725759 & KIC 5544024 & sine \\ +2MASS J19395042+4622296 & G & TIC 271354512 & KIC 9657062 & sine \\ +2MASS J19415575+4522369 & G & TIC 271664690 & KIC 9032578 & sine \\ +2MASS J19450785+5108395 & G & TIC 27778260 & KIC 12367153 & sine \\ +2MASS J19484658+5002007 & G & TIC 28084005 & KIC 11825619 & sine \\ +2MASS J19491761+4638356 & G & TIC 273131067 & KIC 9845711 & sine \\ +2MASS J19535154+4211197 & G & TIC 274119294 & KIC 6719122 & sine \\ +2MASS J19551628+4145582 & G & TIC 171093514 & KIC 6390935 & sine \\ +2MASS J19562459+4408276 & G & TIC 268606798 & KIC 8257716 & sine \\ +2MASS J19572618+4520510 & G & TIC 268712881 & KIC 9048032 & sine \\ +2MASS J19583564+4352320 & G & TIC 269121724 & KIC 8055957 & sine \\ +KOI-1747 & G & TIC 159717069 & KIC 7032421 & sine \\ +KOI-2324 & G & TIC 159105557 & KIC 7746958 & poly \\ +KOI-5796 & G & TIC 63070665 & KIC 10470779 & sine \\ +KOI-5810 & G & TIC 123494489 & KIC 10581308 & sine \\ +KOI-5825 & G & TIC 27183790 & KIC 10737437 & sine \\ +KOI-5952 & G & TIC 27845077 & KIC 12071775 & sine \\ +KOI-741 & G & TIC 272840512 & KIC 10418797 & sine \\ +Kepler-1060 & G & TIC 120691237 & KIC 4544907 & \\ +Kepler-1198 & G & TIC 158843826 & KIC 8681734 & sine \\ +Kepler-1839 & G & TIC 27082730 & KIC 11818607 & sine \\ +Kepler-513 & G & TIC 48503953 & KIC 11802615 & sine \\ +Kepler-739 & G & TIC 159225155 & KIC 9766437 & \\ +UCAC4 640-067417 & G & TIC 122517231 & KIC 2709412 & sine \\ +UCAC4 686-075120 & G & TIC 269030397 & KIC 10098932 & sine \\ +TYC 3560-458-1 & G0 & TIC 26815845 & KIC 10922836 & sine \\ +TYC 3557-1509-1 & G0.5V & TIC 273379797 & KIC 9726613 & sine \\ +TYC 3139-951-1 & G0V & TIC 138215507 & KIC 4660797 & sine \\ +Kepler-1424 & G1.5Vb & TIC 122706631 & KIC 5096590 & sine \\ +KOI-6202 & G1V & TIC 164669854 & KIC 9389245 & sine \\ +Kepler-400 & G2V & TIC 122707140 & KIC 5272233 & sine \\ +TYC 3131-2137-1 & G2V & TIC 164460243 & KIC 7871914 & sine \\ +TYC 3545-2661-1 & G2V & TIC 399827121 & KIC 10850420 & sine \\ +HD 183473 & G5 & TIC 63120335 & KIC 7201012 & sine, poly \\ +TYC 3550-241-1 & G5 & TIC 299088815 & KIC 12008308 & sine \\ +TYC 3562-2088-1 & G5V & TIC 273872314 & KIC 10093680 & sine \\ +TYC 3128-2312-1 & G8V & TIC 120686876 & KIC 5944209 & sine \\ +2MASS J18524052+4156057 & K & - & KIC 6500181 & sine \\ +2MASS J18534407+4208274 & K & - & KIC 6668646 & sine \\ +2MASS J18535462+4135227 & K & - & KIC 6183672 & sine \\ +2MASS J19004200+3903124 & K & TIC 399794444 & KIC 3935803 & sine \\ +2MASS J19082791+4337114 & K & TIC 158389986 & KIC 7879384 & sine \\ +2MASS J19324909+4229041 & K & TIC 275495685 & KIC 6953069 & sine \\ +ATO J296.1841+42.6311 & K & TIC 272184059 & KIC 7133807 & sine \\ +KOI-7449 & K & TIC 279918401 & KIC 11495989 & sine \\ +KOI-8047 & K & TIC 290034561 & KIC 11294822 & sine \\ +Kepler-1259 & K & TIC 273592350 & KIC 10028535 & sine \\ +Kepler-1782 & K & TIC 123202646 & KIC 8142942 & sine \\ +Kepler-1856 & K & TIC 27687265 & KIC 12469800 & sine \\ +Kepler-1966 & K & TIC 137627194 & KIC 5962262 & sine \\ +Kepler-246 & K & TIC 272484980 & KIC 7134976 & sine \\ +2MASS J19200703+4335050 & K0V & TIC 159220196 & KIC 7816999 & sine \\ +BD+41 3306 & K0V & TIC 394172596 & KIC 6278762 & sine, poly \\ +V* V4371 Sgr & K1V & TIC 151839506 & - & poly \\ +2MASS J19400800+4923036 & K5 & TIC 27390487 & KIC 11461764 & sine \\ +2MASS J18460555+4332131 & M & TIC 123317330 & KIC 7800087 & \\ +2MASS J18472701+4348011 & M & TIC 123410529 & KIC 8007234 & sine \\ +2MASS J18491356+4619042 & M & TIC 123447780 & KIC 9631548 & sine \\ +2MASS J18511354+4227227 & M & TIC 164411695 & KIC 6925256 & sine \\ +2MASS J18511902+4837594 & M & TIC 48216443 & KIC 11069034 & sine \\ +2MASS J18512069+4846013 & M & TIC 48216303 & KIC 11122350 & sine \\ +2MASS J18524238+4828368 & M & TIC 48304549 & KIC 10960823 & sine \\ +2MASS J18525314+4818044 & M & TIC 48304703 & KIC 10905192 & sine \\ +2MASS J18525455+4634012 & M & TIC 164457389 & KIC 9754582 & sine \\ +2MASS J18531060+4050093 & M & TIC 237158804 & KIC 5597695 & sine \\ +2MASS J18535987+4741070 & M & TIC 164525174 & KIC 10452840 & sine \\ +2MASS J18541728+4305206 & M & TIC 164529739 & KIC 7422811 & sine \\ +2MASS J18545269+4107528 & M & TIC 350987684 & KIC 5855808 & sine \\ +2MASS J18561787+4457391 & M & TIC 164670879 & KIC 8737443 & sine \\ +2MASS J18574689+4115593 & M & TIC 120254207 & KIC 5941226 & sine \\ +2MASS J18592859+4351465 & M & TIC 164786997 & KIC 8012943 & sine \\ +2MASS J19000393+4109460 & M & TIC 120419969 & KIC 5858361 & sine \\ +2MASS J19001025+4045358 & M & TIC 120422710 & KIC 5515142 & sine \\ +2MASS J19005916+4400190 & M & TIC 164889286 & KIC 8150479 & sine \\ +2MASS J19011064+4206175 & M & TIC 164886887 & KIC 6672948 & sine \\ +2MASS J19011256+4152067 & M & TIC 399822429 & KIC 6425989 & sine \\ +2MASS J19020142+4110533 & M & TIC 120576193 & KIC 5859365 & sine \\ +2MASS J19024516+4429007 & M & TIC 352012319 & KIC 8417053 & \\ +2MASS J19030585+4046008 & M & TIC 120579026 & KIC 5516671 & sine \\ +2MASS J19033576+3941263 & M & TIC 120684614 & KIC 4544623 & sine \\ +2MASS J19034709+4317208 & M & TIC 158166384 & KIC 7592133 & sine \\ +2MASS J19035284+4338273 & M & TIC 158165866 & KIC 7877209 & sine \\ +2MASS J19041026+4530403 & M & TIC 158172860 & KIC 9142714 & sine \\ +2MASS J19053703+4235308 & M & TIC 158218091 & KIC 7018323 & sine \\ +2MASS J19061507+5029221 & M & TIC 399825094 & KIC 12004872 & sine \\ +2MASS J19063685+4928043 & M & TIC 399825963 & KIC 11498106 & sine \\ +2MASS J19064350+5020087 & M & TIC 399825217 & KIC 11955208 & sine \\ +2MASS J19064648+4931162 & M & TIC 399825921 & KIC 11550428 & sine \\ +2MASS J19081745+3902346 & M & TIC 121085753 & KIC 3940372 & sine \\ +2MASS J19083962+4221137 & M & TIC 158388172 & KIC 6849112 & sine \\ +2MASS J19085407+4320395 & M & TIC 158423632 & KIC 7670700 & sine \\ +2MASS J19103260+4322147 & M & TIC 158551504 & KIC 7671594 & sine \\ +2MASS J19104382+4039368 & M & TIC 121329525 & KIC 5435958 & sine \\ +2MASS J19110814+4024571 & M & TIC 121333779 & KIC 5262561 & sine \\ +2MASS J19114749+4048205 & M & TIC 121461193 & KIC 5608002 & sine \\ +2MASS J19130891+5127421 & M & TIC 298961665 & KIC 12505054 & sine \\ +2MASS J19135561+4319299 & M & TIC 158725435 & KIC 7673428 & sine \\ +2MASS J19141052+4559479 & M & TIC 158787568 & KIC 9396972 & sine \\ +2MASS J19143720+4243450 & M & TIC 158795349 & KIC 7190459 & \\ +2MASS J19152845+5001374 & M & TIC 299088298 & KIC 11808734 & sine \\ +2MASS J19160242+4726491 & M & TIC 158983853 & KIC 10332732 & sine \\ +2MASS J19170322+4953087 & M & TIC 299159305 & KIC 11708034 & sine \\ +2MASS J19200001+3844383 & M & TIC 122225323 & KIC 3640527 & sine \\ +2MASS J19200978+4954168 & M & TIC 267747418 & KIC 11760021 & sine \\ +2MASS J19205088+5018194 & M & TIC 406950619 & KIC 11961075 & sine \\ +2MASS J19210354+4523201 & M & TIC 159303166 & KIC 9017693 & sine \\ +2MASS J19213187+4459115 & M & TIC 159387244 & KIC 8749769 & sine \\ +2MASS J19232149+5107053 & M & TIC 417655942 & KIC 12356051 & sine \\ +2MASS J19233077+5035350 & M & TIC 417656504 & KIC 12060710 & sine \\ +2MASS J19233788+4518061 & M & TIC 159520226 & KIC 9019435 & sine \\ +2MASS J19240851+3747169 & M & TIC 122781970 & KIC 2441562 & sine \\ +2MASS J19242752+5106364 & M & TIC 350738203 & KIC 12356489 & sine \\ +2MASS J19291103+4821243 & M & TIC 424864617 & KIC 10921009 & sine \\ +2MASS J19304396+4112528 & M & TIC 137759349 & KIC 5962956 & sine \\ +2MASS J19304840+4142454 & M & TIC 137758161 & KIC 6366739 & sine \\ +2MASS J19335656+4010546 & M & - & KIC 5016904 & sine, poly \\ +2MASS J19343395+4137235 & M & TIC 138222062 & KIC 6290811 & sine \\ +2MASS J19353467+3943573 & M & TIC 138436033 & KIC 4662431 & sine \\ +2MASS J19353874+4708324 & M & TIC 270790828 & KIC 10146539 & \\ +2MASS J19365745+4628121 & M & TIC 270957843 & KIC 9716117 & sine \\ +2MASS J19374745+4341098 & M & TIC 271047224 & KIC 7898781 & sine \\ +2MASS J19423900+5108356 & M & TIC 27639064 & KIC 12365719 & sine \\ +2MASS J19433653+4758149 & M & TIC 27645448 & KIC 10676126 & sine \\ +2MASS J19443380+4843497 & M & TIC 27770198 & KIC 11147271 & sine \\ +2MASS J19444493+4720327 & M & TIC 272279258 & KIC 10285642 & sine \\ +2MASS J19450930+4754591 & M & TIC 27771932 & KIC 10677397 & sine \\ +2MASS J19451164+4345265 & M & TIC 272270363 & KIC 7973675 & sine \\ +2MASS J19454134+3906345 & M & TIC 184471264 & KIC 4077867 & sine \\ +2MASS J19471875+4123248 & M & TIC 239228371 & KIC 6060845 & sine \\ +2MASS J19471987+4747258 & M & TIC 272841049 & KIC 10548508 & sine \\ +2MASS J19480997+4310160 & M & TIC 272943707 & KIC 7547969 & sine \\ +2MASS J19503771+4705359 & M & TIC 273378083 & KIC 10091786 & sine \\ +2MASS J19503804+4041450 & M & TIC 169816129 & KIC 5471468 & sine \\ +2MASS J19505785+4630250 & M & TIC 273379615 & KIC 9786877 & sine \\ +2MASS J19510637+4505045 & M & TIC 273383619 & KIC 8836388 & sine \\ +2MASS J19525571+4743328 & M & TIC 273874034 & KIC 10553513 & sine \\ +2MASS J19542833+4420425 & M & TIC 268158580 & KIC 8387621 & sine \\ +2MASS J19543981+4814406 & M & TIC 264508845 & KIC 10880514 & sine \\ +2MASS J19550625+4009192 & M & TIC 171101426 & KIC 5041192 & sine \\ +2MASS J19553603+4805356 & M & TIC 416528859 & KIC 10753072 & sine \\ +2MASS J19561258+4335485 & M & TIC 268485803 & KIC 7847566 & sine \\ +2MASS J19584764+4711122 & M & TIC 269029909 & KIC 10165815 & sine \\ +2MASS J20000387+4531405 & M & TIC 239234887 & KIC 9179906 & sine \\ +ATO J285.1153+45.7850 & M & TIC 164882037 & KIC 9267818 & sine \\ +KOI-1654 & M & TIC 48355200 & KIC 11546211 & sine \\ +UCAC4 639-062929 & M & TIC 120963868 & KIC 2284919 & sine \\ +UCAC4 651-066418 & M & TIC 120354289 & KIC 4904647 & sine \\ +UCAC4 661-082974 & M & TIC 268288304 & KIC 6720765 & sine \\ +UCAC4 664-071715 & M & TIC 158430593 & KIC 7104739 & sine \\ +UCAC4 668-073165 & M & TIC 158432884 & KIC 7741987 & sine \\ +UCAC4 683-066189 & M & TIC 351897570 & KIC 9692206 & sine \\ +UCAC4 707-062317 & M & TIC 299097784 & KIC 12403318 & sine \\ +Kepler-210 & M0V & TIC 63283780 & KIC 7447200 & poly \\ +MCC 428 & M0V & TIC 434136638 & - & \\ +HG 7-26 & M1 & TIC 345454031 & - & \\ +G 6-33 & M1.5V & TIC 434160946 & - & sine \\ +HD 197481 & M1VeBa1 & TIC 441420236 & - & poly \\ +2MASS J19412234+5104273 & M2.1 & TIC 27454242 & KIC 12314646 & sine \\ +PM J19399+3950 & M2.5 & TIC 138893136 & KIC 4758595 & sine \\ +UCAC4 647-065171 & M2.5 & TIC 121215155 & KIC 4142890 & sine \\ +LP 474-124 & M2.5V & TIC 348663808 & - & \\ +2MASS J19130537+5020559 & M2.5Ve & TIC 298962893 & KIC 11957647 & sine \\ +2MASS J19324802+4200580 & M2.7 & TIC 275496670 & KIC 6610837 & sine \\ +2MASS J19445931+4812415 & M2.8 & TIC 27772498 & KIC 10872868 & sine \\ +2MASS J19183060+4153031 & M3 & TIC 122067236 & KIC 6436291 & sine \\ +{[PS78]} 219 & M3+ & TIC 11652986 & - & \\ +UCAC4 673-078334 & M3.0Ve & TIC 272272592 & KIC 8507979 & sine \\ +LP 426-35 & M3.5V & TIC 197247983 & - & \\ +LP 737-14 & M3.5V & TIC 335628483 & - & \\ +BD+16 2708 & M3V & TIC 258105174 & - & \\ +2MASS J18535530+4310389 & M3Ve & TIC 164529625 & KIC 7505644 & sine \\ +2MASS J18592696+4548446 & M3Ve & TIC 164784762 & KIC 9328653 & sine \\ +2MASS J19015564+4134218 & M3Ve & TIC 120576760 & KIC 6187812 & sine \\ +CD-43 9546 & M3Ve & TIC 334524122 & - & poly \\ +2MASS J22534969-1721358 & M4 & TIC 188586529 & - & \\ +LP 873-37 & M4 & TIC 99566892 & - & \\ +2MASS J19150930+5101139 & M4.5V & TIC 299089441 & KIC 12302994 & \\ +2MASS J19573917+4554182 & M4.5V & TIC 268711231 & KIC 9426508 & sine \\ +UCAC4 683-069625 & M4.5V & TIC 159171299 & KIC 9705079 & sine \\ +2MASS J18432784+4727325 & M4Ve & TIC 123205792 & KIC 10318386 & sine \\ +2MASS J18474286+4218039 & M4Ve & TIC 123408865 & KIC 6837702 & sine \\ +2MASS J18535193+4327449 & M4Ve & TIC 164529313 & KIC 7734382 & sine \\ +2MASS J19045588+3738361 & M4Ve & TIC 120825083 & KIC 2283749 & sine \\ +LP 760-3 & M6.5V & - & - & \\ +2MASS J19202351+5037161 & M6Ve & TIC 267746625 & KIC 12108566 & sine \\ +L 762-51 & dM3.5 & TIC 286942673 & - & \\ +GALEX J184242.4+440405 & sdB & TIC 123198279 & KIC 8142623 & sine \\ +GALEX J191612.1+474915 & sdB+F/G & TIC 158984345 & KIC 10593239 & sine \\ +SDSS J192715.88+380808.2 & sdB+dM & - & KIC 2991403 & sine \\ +\end{longtable} +} + +{ +\centering +\tabcolsep=5pt +\begin{longtable}{lclll} +\caption{Table containing all stars which where analysed. The first column (Main Identifier) is matched with SIMBADs "MAIN\_ID" value for the star. The second column specifies the spectral type of the star according to SIMBAD (with the exception of the stars mentioned in section \ref{sec:data:sptype_identification}, which use the method described in that section). The TIC and KIC columns represent the TESS and Kepler Input Catalogues respectively. The list is sorted first by spectral type, and then by main identifier.} +\label{apA:list_of_all_stars}\\ +\hline\hline +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ +\hline +\endfirsthead + +\hline\hline +\multicolumn{1}{c}{Main Identifier} & \multicolumn{1}{c}{Sp. Type} & \multicolumn{1}{c}{TIC} & \multicolumn{1}{c}{KIC} & \multicolumn{1}{c}{Fit Type} \\ +\hline +\endhead + +\hline +\endfoot + +\hline\hline +\endlastfoot +HD 225391 & A & TIC 139156518 & KIC 5632093 & sine \\ +HD 226712 & A & TIC 171882897 & KIC 5905878 & sine \\ +TYC 3125-2237-1 & A & TIC 121274152 & KIC 4641547 & sine \\ +HD 187141 & A0 & TIC 360021868 & KIC 6381306 & sine \\ +HD 188360 & A0 & TIC 28359846 & KIC 10815604 & sine \\ +HD 177982 & A2 & TIC 120821069 & KIC 4995049 & sine \\ +HD 225493 & A4V & TIC 184163024 & KIC 5201872 & sine \\ +TYC 3551-561-1 & A5IV & TIC 26418553 & KIC 11296464 & sine \\ +HD 225333 & A5V & TIC 139037071 & KIC 3458671 & sine \\ +AG+46 1529 & A7III & TIC 273380253 & KIC 9604762 & sine \\ +TYC 3560-1923-1 & A9IV–V & TIC 271167267 & KIC 10281360 & sine \\ +TYC 3565-514-1 & A9V & TIC 27458214 & KIC 11197934 & sine \\ +KOI-3818 & B9.5Vn & TIC 159102838 & KIC 6515722 & sine \\ +2MASS J18491671+4410445 & F & TIC 123449867 & KIC 8212826 & sine \\ +KOI-4698 & F & TIC 159643077 & KIC 10663738 & sine \\ +Kepler-1271 & F & TIC 120825510 & KIC 1996180 & sine \\ +Kepler-1443 & F & TIC 164525743 & KIC 10057494 & sine \\ +Kepler-380 & F & TIC 48132154 & KIC 11121752 & sine \\ +Kepler-494 & F & TIC 169176556 & KIC 6305192 & sine \\ +TYC 3134-301-1 & F & TIC 137483286 & KIC 3852772 & sine \\ +KOI-19 & F3/F5V & TIC 123201406 & KIC 7255336 & sine \\ +TYC 3557-727-1 & F3/F5V & TIC 273684688 & KIC 9788113 & sine \\ +TYC 3140-1658-1 & F5 & TIC 138967825 & KIC 5802601 & sine \\ +TYC 3557-1501-1 & F6IV & TIC 273043859 & KIC 9724820 & sine \\ +KOI-44 & F7IV & TIC 239276046 & KIC 8845026 & sine \\ +Kepler-1084 & F8V & TIC 267749737 & KIC 10857519 & sine \\ +2MASS J18425375+4345336 & G & TIC 123198563 & KIC 7936748 & sine \\ +2MASS J18495232+4309276 & G & TIC 123489639 & KIC 7503439 & \\ +2MASS J18525868+4530560 & G & TIC 164458315 & KIC 9137611 & sine \\ +2MASS J18582492+4446498 & G & TIC 164779298 & KIC 8609289 & sine \\ +2MASS J19012927+4104159 & G & TIC 120496415 & KIC 5773205 & sine \\ +2MASS J19043346+4427484 & G & TIC 158171605 & KIC 8417863 & sine \\ +2MASS J19061691+4654395 & G & TIC 158272786 & KIC 10000509 & sine \\ +2MASS J19065549+3937268 & G & TIC 121012476 & KIC 4546541 & sine \\ +2MASS J19080680+4450500 & G & TIC 158391683 & KIC 8678334 & sine \\ +2MASS J19100183+4257041 & G & TIC 158552191 & KIC 7350021 & sine \\ +2MASS J19182441+4439465 & G & TIC 159097797 & KIC 8554173 & sine \\ +2MASS J19184939+4418233 & G & TIC 159107064 & KIC 8359762 & sine \\ +2MASS J19185028+4633324 & G & TIC 159171504 & KIC 9765670 & sine \\ +2MASS J19250540+3734332 & G & TIC 137097085 & KIC 2159377 & sine \\ +2MASS J19280249+3911165 & G & TIC 137402956 & KIC 4058829 & sine, poly \\ +2MASS J19283146+3837123 & G & TIC 137484235 & KIC 3547283 & sine \\ +2MASS J19313155+4628249 & G & TIC 63452929 & KIC 9712781 & sine \\ +2MASS J19320792+3933052 & G & TIC 137972488 & KIC 4469481 & sine \\ +2MASS J19350077+4608423 & G & TIC 270698467 & KIC 9531002 & sine \\ +2MASS J19354814+4118464 & G & TIC 138431713 & KIC 6049426 & sine \\ +2MASS J19354900+4623499 & G & TIC 270789534 & KIC 9654338 & sine \\ +2MASS J19364457+4403341 & G & TIC 270859571 & KIC 8172597 & sine \\ +2MASS J19370439+4626209 & G & TIC 270957778 & KIC 9716208 & sine \\ +2MASS J19390861+4046149 & G & TIC 138725759 & KIC 5544024 & sine \\ +2MASS J19395042+4622296 & G & TIC 271354512 & KIC 9657062 & sine \\ +2MASS J19415575+4522369 & G & TIC 271664690 & KIC 9032578 & sine \\ +2MASS J19450785+5108395 & G & TIC 27778260 & KIC 12367153 & sine \\ +2MASS J19484658+5002007 & G & TIC 28084005 & KIC 11825619 & sine \\ +2MASS J19491761+4638356 & G & TIC 273131067 & KIC 9845711 & sine \\ +2MASS J19535154+4211197 & G & TIC 274119294 & KIC 6719122 & sine \\ +2MASS J19551628+4145582 & G & TIC 171093514 & KIC 6390935 & sine \\ +2MASS J19553242+4737586 & G & TIC 268382866 & KIC 10491422 & sine \\ +2MASS J19562459+4408276 & G & TIC 268606798 & KIC 8257716 & sine \\ +2MASS J19572618+4520510 & G & TIC 268712881 & KIC 9048032 & sine \\ +2MASS J19583564+4352320 & G & TIC 269121724 & KIC 8055957 & sine \\ +2MASS J20060991+4417004 & G & TIC 185335830 & KIC 8332459 & sine \\ +ATO J285.5682+44.5725 & G & TIC 352012409 & KIC 8481574 & sine \\ +BD-08 995 & G & TIC 43472154 & - & sine \\ +KOI-1747 & G & TIC 159717069 & KIC 7032421 & sine \\ +KOI-2324 & G & TIC 159105557 & KIC 7746958 & poly \\ +KOI-5796 & G & TIC 63070665 & KIC 10470779 & sine \\ +KOI-5810 & G & TIC 123494489 & KIC 10581308 & sine \\ +KOI-5825 & G & TIC 27183790 & KIC 10737437 & sine \\ +KOI-5952 & G & TIC 27845077 & KIC 12071775 & sine \\ +KOI-741 & G & TIC 272840512 & KIC 10418797 & sine \\ +Kepler-1060 & G & TIC 120691237 & KIC 4544907 & \\ +Kepler-1198 & G & TIC 158843826 & KIC 8681734 & sine \\ +Kepler-1839 & G & TIC 27082730 & KIC 11818607 & sine \\ +Kepler-513 & G & TIC 48503953 & KIC 11802615 & sine \\ +Kepler-725 & G & TIC 164652841 & KIC 8672910 & sine \\ +Kepler-739 & G & TIC 159225155 & KIC 9766437 & \\ +TYC 4595-107-1 & G & TIC 394030788 & - & sine \\ +UCAC4 640-067417 & G & TIC 122517231 & KIC 2709412 & sine \\ +UCAC4 686-075120 & G & TIC 269030397 & KIC 10098932 & sine \\ +V* V452 Lyr & G & - & KIC 7742289 & sine \\ +BD-01 2318 & G0 & TIC 78234015 & - & sine \\ +HD 295290 & G0 & TIC 53417036 & - & sine \\ +TYC 3560-458-1 & G0 & TIC 26815845 & KIC 10922836 & sine \\ +TYC 3557-1509-1 & G0.5V & TIC 273379797 & KIC 9726613 & sine \\ +TYC 3139-951-1 & G0V & TIC 138215507 & KIC 4660797 & sine \\ +Kepler-1424 & G1.5Vb & TIC 122706631 & KIC 5096590 & sine \\ +KOI-6202 & G1V & TIC 164669854 & KIC 9389245 & sine \\ +Kepler-400 & G2V & TIC 122707140 & KIC 5272233 & sine \\ +TYC 3131-2137-1 & G2V & TIC 164460243 & KIC 7871914 & sine \\ +TYC 3146-672-1 & G2V & TIC 159448893 & KIC 7523785 & sine \\ +TYC 3545-2661-1 & G2V & TIC 399827121 & KIC 10850420 & sine \\ +HD 183473 & G5 & TIC 63120335 & KIC 7201012 & sine, poly \\ +HD 214261 & G5 & TIC 200501090 & - & sine \\ +KOI-644 & G5 & TIC 122138452 & KIC 5356593 & sine \\ +TYC 3550-241-1 & G5 & TIC 299088815 & KIC 12008308 & sine \\ +HD 23524 & G5V & TIC 428761512 & - & sine \\ +TYC 3562-2088-1 & G5V & TIC 273872314 & KIC 10093680 & sine \\ +V* AG Lep & G5V & TIC 92845906 & - & sine \\ +HD 222259A & G6V & TIC 410214986 & - & sine \\ +Kepler-605 & G7 & TIC 158423850 & KIC 7595157 & sine, poly \\ +TYC 3128-2312-1 & G8V & TIC 120686876 & KIC 5944209 & sine \\ +HD 180445 & G8V(e) & TIC 97914505 & - & sine \\ +HD 220186 & G9Ve & TIC 49619607 & - & sine \\ +1RXS J064643.6-770027 & K & TIC 177255827 & - & sine \\ +2MASS J18524052+4156057 & K & - & KIC 6500181 & sine \\ +2MASS J18534407+4208274 & K & - & KIC 6668646 & sine \\ +2MASS J18535462+4135227 & K & - & KIC 6183672 & sine \\ +2MASS J19004200+3903124 & K & TIC 399794444 & KIC 3935803 & sine \\ +2MASS J19082791+4337114 & K & TIC 158389986 & KIC 7879384 & sine \\ +2MASS J19324909+4229041 & K & TIC 275495685 & KIC 6953069 & sine \\ +2MASS J19404949+5046469 & K & TIC 27398219 & KIC 12166457 & sine \\ +ATO J296.1841+42.6311 & K & TIC 272184059 & KIC 7133807 & sine \\ +CPD-19 878 & K & TIC 93125144 & - & sine \\ +KOI-7449 & K & TIC 279918401 & KIC 11495989 & sine \\ +KOI-8047 & K & TIC 290034561 & KIC 11294822 & sine \\ +Kepler-1259 & K & TIC 273592350 & KIC 10028535 & sine \\ +Kepler-1782 & K & TIC 123202646 & KIC 8142942 & sine \\ +Kepler-1856 & K & TIC 27687265 & KIC 12469800 & sine \\ +Kepler-1966 & K & TIC 137627194 & KIC 5962262 & sine \\ +Kepler-246 & K & TIC 272484980 & KIC 7134976 & sine \\ +Kepler-693 & K & TIC 237159318 & KIC 5164255 & sine \\ +PM J07058-5848 & K & TIC 279615427 & - & sine \\ +TYC 1360-957-1 & K & TIC 247117382 & - & sine \\ +HD 245924 & K0IV & TIC 19934471 & - & sine \\ +2MASS J19200703+4335050 & K0V & TIC 159220196 & KIC 7816999 & sine \\ +BD+41 3306 & K0V & TIC 394172596 & KIC 6278762 & sine, poly \\ +CD-26 1578 & K0V & TIC 44797824 & - & sine \\ +TYC 553-33-1 & K0V:e & TIC 405405298 & - & sine \\ +RX J1925.0+4429 & K1V & TIC 159721038 & KIC 8429280 & sine \\ +V* V4371 Sgr & K1V & TIC 151839506 & - & poly \\ +HD 215341 & K1Ve & TIC 145752454 & - & sine \\ +TYC 582-114-1 & K1Ve & TIC 344163180 & - & sine \\ +V* LQ Hya & K1Vp & TIC 46907042 & - & sine \\ +Kepler-1558 & K2 & TIC 158322085 & KIC 10000941 & sine \\ +HD 283750 & K2.5Ve & TIC 125838647 & - & sine \\ +CD-52 381 & K2V(e) & TIC 229151691 & - & sine \\ +V* V471 Tau & K2V+DA & TIC 456863710 & - & sine \\ +Kepler-411 & K3V & TIC 399954349 & KIC 11551692 & sine \\ +BD-13 6131 & K3Ve & TIC 437696706 & - & sine \\ +V* BY Dra & K4Ve+K7.5Ve & TIC 47579336 & - & sine \\ +2MASS J19400800+4923036 & K5 & TIC 27390487 & KIC 11461764 & sine \\ +V* CC Eri & K7V & TIC 142206123 & - & sine \\ +2MASS J18460555+4332131 & M & TIC 123317330 & KIC 7800087 & \\ +2MASS J18472701+4348011 & M & TIC 123410529 & KIC 8007234 & sine \\ +2MASS J18491356+4619042 & M & TIC 123447780 & KIC 9631548 & sine \\ +2MASS J18511354+4227227 & M & TIC 164411695 & KIC 6925256 & sine \\ +2MASS J18511902+4837594 & M & TIC 48216443 & KIC 11069034 & sine \\ +2MASS J18512069+4846013 & M & TIC 48216303 & KIC 11122350 & sine \\ +2MASS J18524238+4828368 & M & TIC 48304549 & KIC 10960823 & sine \\ +2MASS J18525314+4818044 & M & TIC 48304703 & KIC 10905192 & sine \\ +2MASS J18525455+4634012 & M & TIC 164457389 & KIC 9754582 & sine \\ +2MASS J18531060+4050093 & M & TIC 237158804 & KIC 5597695 & sine \\ +2MASS J18535987+4741070 & M & TIC 164525174 & KIC 10452840 & sine \\ +2MASS J18541728+4305206 & M & TIC 164529739 & KIC 7422811 & sine \\ +2MASS J18545269+4107528 & M & TIC 350987684 & KIC 5855808 & sine \\ +2MASS J18561787+4457391 & M & TIC 164670879 & KIC 8737443 & sine \\ +2MASS J18565158+4448162 & M & TIC 164671055 & KIC 8673358 & sine \\ +2MASS J18570619+4516101 & M & TIC 164677934 & KIC 8935942 & sine \\ +2MASS J18572876+4035369 & M & TIC 120251682 & KIC 5342558 & sine \\ +2MASS J18574689+4115593 & M & TIC 120254207 & KIC 5941226 & sine \\ +2MASS J18592859+4351465 & M & TIC 164786997 & KIC 8012943 & sine \\ +2MASS J19000393+4109460 & M & TIC 120419969 & KIC 5858361 & sine \\ +2MASS J19001025+4045358 & M & TIC 120422710 & KIC 5515142 & sine \\ +2MASS J19005916+4400190 & M & TIC 164889286 & KIC 8150479 & sine \\ +2MASS J19011064+4206175 & M & TIC 164886887 & KIC 6672948 & sine \\ +2MASS J19011256+4152067 & M & TIC 399822429 & KIC 6425989 & sine \\ +2MASS J19020142+4110533 & M & TIC 120576193 & KIC 5859365 & sine \\ +2MASS J19023480+4539052 & M & TIC 352013620 & KIC 9205855 & sine \\ +2MASS J19024516+4429007 & M & TIC 352012319 & KIC 8417053 & \\ +2MASS J19030585+4046008 & M & TIC 120579026 & KIC 5516671 & sine \\ +2MASS J19033576+3941263 & M & TIC 120684614 & KIC 4544623 & sine \\ +2MASS J19034709+4317208 & M & TIC 158166384 & KIC 7592133 & sine \\ +2MASS J19035284+4338273 & M & TIC 158165866 & KIC 7877209 & sine \\ +2MASS J19041026+4530403 & M & TIC 158172860 & KIC 9142714 & sine \\ +2MASS J19053703+4235308 & M & TIC 158218091 & KIC 7018323 & sine \\ +2MASS J19061507+5029221 & M & TIC 399825094 & KIC 12004872 & sine \\ +2MASS J19061662+4502422 & M & TIC 158274889 & KIC 8807085 & sine \\ +2MASS J19063685+4928043 & M & TIC 399825963 & KIC 11498106 & sine \\ +2MASS J19064350+5020087 & M & TIC 399825217 & KIC 11955208 & sine \\ +2MASS J19064648+4931162 & M & TIC 399825921 & KIC 11550428 & sine \\ +2MASS J19074075+3752413 & M & TIC 121022434 & KIC 2557669 & sine \\ +2MASS J19081745+3902346 & M & TIC 121085753 & KIC 3940372 & sine \\ +2MASS J19083962+4221137 & M & TIC 158388172 & KIC 6849112 & sine \\ +2MASS J19085407+4320395 & M & TIC 158423632 & KIC 7670700 & sine \\ +2MASS J19103260+4322147 & M & TIC 158551504 & KIC 7671594 & sine \\ +2MASS J19104382+4039368 & M & TIC 121329525 & KIC 5435958 & sine \\ +2MASS J19110814+4024571 & M & TIC 121333779 & KIC 5262561 & sine \\ +2MASS J19114749+4048205 & M & TIC 121461193 & KIC 5608002 & sine \\ +2MASS J19130891+5127421 & M & TIC 298961665 & KIC 12505054 & sine \\ +2MASS J19135561+4319299 & M & TIC 158725435 & KIC 7673428 & sine \\ +2MASS J19141052+4559479 & M & TIC 158787568 & KIC 9396972 & sine \\ +2MASS J19143720+4243450 & M & TIC 158795349 & KIC 7190459 & \\ +2MASS J19152845+5001374 & M & TIC 299088298 & KIC 11808734 & sine \\ +2MASS J19160242+4726491 & M & TIC 158983853 & KIC 10332732 & sine \\ +2MASS J19170322+4953087 & M & TIC 299159305 & KIC 11708034 & sine \\ +2MASS J19200001+3844383 & M & TIC 122225323 & KIC 3640527 & sine \\ +2MASS J19200978+4954168 & M & TIC 267747418 & KIC 11760021 & sine \\ +2MASS J19205088+5018194 & M & TIC 406950619 & KIC 11961075 & sine \\ +2MASS J19210354+4523201 & M & TIC 159303166 & KIC 9017693 & sine \\ +2MASS J19213187+4459115 & M & TIC 159387244 & KIC 8749769 & sine \\ +2MASS J19230963+3739397 & M & TIC 122672447 & KIC 2300039 & sine \\ +2MASS J19232149+5107053 & M & TIC 417655942 & KIC 12356051 & sine \\ +2MASS J19233077+5035350 & M & TIC 417656504 & KIC 12060710 & sine \\ +2MASS J19233788+4518061 & M & TIC 159520226 & KIC 9019435 & sine \\ +2MASS J19240851+3747169 & M & TIC 122781970 & KIC 2441562 & sine \\ +2MASS J19242752+5106364 & M & TIC 350738203 & KIC 12356489 & sine \\ +2MASS J19255059+4532219 & M & TIC 159761686 & KIC 9153754 & sine \\ +2MASS J19291103+4821243 & M & TIC 424864617 & KIC 10921009 & sine \\ +2MASS J19304396+4112528 & M & TIC 137759349 & KIC 5962956 & sine \\ +2MASS J19304840+4142454 & M & TIC 137758161 & KIC 6366739 & sine \\ +2MASS J19335656+4010546 & M & - & KIC 5016904 & sine, poly \\ +2MASS J19343395+4137235 & M & TIC 138222062 & KIC 6290811 & sine \\ +2MASS J19353467+3943573 & M & TIC 138436033 & KIC 4662431 & sine \\ +2MASS J19353874+4708324 & M & TIC 270790828 & KIC 10146539 & \\ +2MASS J19365745+4628121 & M & TIC 270957843 & KIC 9716117 & sine \\ +2MASS J19374745+4341098 & M & TIC 271047224 & KIC 7898781 & sine \\ +2MASS J19421615+4928069 & M & TIC 27531488 & KIC 11515276 & sine \\ +2MASS J19423900+5108356 & M & TIC 27639064 & KIC 12365719 & sine \\ +2MASS J19433653+4758149 & M & TIC 27645448 & KIC 10676126 & sine \\ +2MASS J19443380+4843497 & M & TIC 27770198 & KIC 11147271 & sine \\ +2MASS J19444493+4720327 & M & TIC 272279258 & KIC 10285642 & sine \\ +2MASS J19450930+4754591 & M & TIC 27771932 & KIC 10677397 & sine \\ +2MASS J19451164+4345265 & M & TIC 272270363 & KIC 7973675 & sine \\ +2MASS J19454134+3906345 & M & TIC 184471264 & KIC 4077867 & sine \\ +2MASS J19471875+4123248 & M & TIC 239228371 & KIC 6060845 & sine \\ +2MASS J19471987+4747258 & M & TIC 272841049 & KIC 10548508 & sine \\ +2MASS J19480997+4310160 & M & TIC 272943707 & KIC 7547969 & sine \\ +2MASS J19503771+4705359 & M & TIC 273378083 & KIC 10091786 & sine \\ +2MASS J19503804+4041450 & M & TIC 169816129 & KIC 5471468 & sine \\ +2MASS J19505785+4630250 & M & TIC 273379615 & KIC 9786877 & sine \\ +2MASS J19510637+4505045 & M & TIC 273383619 & KIC 8836388 & sine \\ +2MASS J19525571+4743328 & M & TIC 273874034 & KIC 10553513 & sine \\ +2MASS J19542833+4420425 & M & TIC 268158580 & KIC 8387621 & sine \\ +2MASS J19543981+4814406 & M & TIC 264508845 & KIC 10880514 & sine \\ +2MASS J19550625+4009192 & M & TIC 171101426 & KIC 5041192 & sine \\ +2MASS J19553603+4805356 & M & TIC 416528859 & KIC 10753072 & sine \\ +2MASS J19561258+4335485 & M & TIC 268485803 & KIC 7847566 & sine \\ +2MASS J19584764+4711122 & M & TIC 269029909 & KIC 10165815 & sine \\ +2MASS J20000387+4531405 & M & TIC 239234887 & KIC 9179906 & sine \\ +ATO J285.1153+45.7850 & M & TIC 164882037 & KIC 9267818 & sine \\ +KOI-1654 & M & TIC 48355200 & KIC 11546211 & sine \\ +UCAC4 639-062929 & M & TIC 120963868 & KIC 2284919 & sine \\ +UCAC4 643-073385 & M & TIC 138647610 & KIC 3454793 & sine \\ +UCAC4 651-066418 & M & TIC 120354289 & KIC 4904647 & sine \\ +UCAC4 661-082974 & M & TIC 268288304 & KIC 6720765 & sine \\ +UCAC4 664-071715 & M & TIC 158430593 & KIC 7104739 & sine \\ +UCAC4 668-073165 & M & TIC 158432884 & KIC 7741987 & sine \\ +UCAC4 683-066189 & M & TIC 351897570 & KIC 9692206 & sine \\ +UCAC4 707-062317 & M & TIC 299097784 & KIC 12403318 & sine \\ +1RXS J060224.9-163451 & M0 & TIC 95328477 & - & sine \\ +V* MY Tau & M0.5e & TIC 348638763 & - & sine \\ +WOH S 209 & M0: & TIC 179038379 & - & sine \\ +Kepler-210 & M0V & TIC 63283780 & KIC 7447200 & poly \\ +MCC 428 & M0V & TIC 434136638 & - & \\ +V* HK Aqr & M0Ve & TIC 5656273 & - & sine \\ +HG 7-26 & M1 & TIC 345454031 & - & \\ +V* OT Ser & M1.0V & TIC 355793860 & - & sine, poly \\ +V* V631 Tau & M1.5 & TIC 348638813 & - & sine \\ +2MASS J18563342+4513481 & M1.5V & TIC 164670606 & KIC 8935655 & sine \\ +G 6-33 & M1.5V & TIC 434160946 & - & sine \\ +V* FF And & M1Ve+M1Ve & TIC 267802440 & - & sine \\ +HD 197481 & M1VeBa1 & TIC 441420236 & - & poly \\ +{[LM84]} 3-13 & M2 & TIC 165124012 & - & sine \\ +V* AX Cnc & M2.0 & TIC 175233993 & - & sine, poly \\ +2MASS J19412234+5104273 & M2.1 & TIC 27454242 & KIC 12314646 & sine \\ +1RXS J004211.1-425245 & M2.2 & TIC 80427281 & - & sine \\ +2MASS J04133314-5231586 & M2.4 & TIC 219229275 & - & sine \\ +PM J19399+3950 & M2.5 & TIC 138893136 & KIC 4758595 & sine \\ +UCAC4 647-065171 & M2.5 & TIC 121215155 & KIC 4142890 & sine \\ +G 10-29 & M2.5V & TIC 396951485 & - & sine \\ +LP 474-124 & M2.5V & TIC 348663808 & - & \\ +2MASS J19130537+5020559 & M2.5Ve & TIC 298962893 & KIC 11957647 & sine \\ +ASAS J232857-6802.4 & M2.5Ve & TIC 229807000 & - & sine \\ +2MASS J19324802+4200580 & M2.7 & TIC 275496670 & KIC 6610837 & sine \\ +2MASS J19445931+4812415 & M2.8 & TIC 27772498 & KIC 10872868 & sine \\ +V* V497 Tau & M2.9 & TIC 258032026 & - & sine \\ +CD-51 13128 & M2Ve & TIC 140045538 & - & sine \\ +2MASS J19183060+4153031 & M3 & TIC 122067236 & KIC 6436291 & sine \\ +{[PS78]} 219 & M3+ & TIC 11652986 & - & \\ +UCAC4 698-065839 & M3.0 & TIC 48504458 & KIC 11495571 & sine \\ +G 9-11 & M3.0V & TIC 21246336 & - & sine \\ +UCAC4 673-078334 & M3.0Ve & TIC 272272592 & KIC 8507979 & sine \\ +G 209-3 & M3.4 & TIC 28231379 & KIC 10877432 & sine \\ +V* LT Tau & M3.5 & TIC 258067389 & - & sine \\ +BD-15 6290 & M3.5V & TIC 188580272 & - & sine \\ +LP 426-35 & M3.5V & TIC 197247983 & - & \\ +LP 737-14 & M3.5V & TIC 335628483 & - & \\ +2MASS J22371494-2622332 & M3.5Ve & TIC 326446019 & - & sine \\ +BD+16 2708 & M3V & TIC 258105174 & - & \\ +KOI-256 & M3V & TIC 48528261 & KIC 11548140 & sine \\ +LAMOST J192817.82+410412.2 & M3V & TIC 137410897 & KIC 5791720 & sine \\ +2MASS J18535530+4310389 & M3Ve & TIC 164529625 & KIC 7505644 & sine \\ +2MASS J18592696+4548446 & M3Ve & TIC 164784762 & KIC 9328653 & sine \\ +2MASS J19015564+4134218 & M3Ve & TIC 120576760 & KIC 6187812 & sine \\ +CD-43 9546 & M3Ve & TIC 334524122 & - & poly \\ +CD-56 1032A & M3Ve & TIC 220433363 & - & sine \\ +2MASS J04534379-5836247 & M3e & TIC 220432563 & - & sine \\ +2MASS J22534969-1721358 & M4 & TIC 188586529 & - & \\ +LP 873-37 & M4 & TIC 99566892 & - & \\ +1RXS J185504.7+425952 & M4.0V & TIC 164644375 & KIC 7341653 & sine \\ +HG 8-80 & M4.0V & TIC 435916078 & - & sine \\ +V* EV Lac & M4.0Ve & TIC 154101678 & - & sine \\ +2MASS J01275875-6032243 & M4.2 & TIC 237910557 & - & sine \\ +2MASS J19150930+5101139 & M4.5V & TIC 299089441 & KIC 12302994 & \\ +2MASS J19573917+4554182 & M4.5V & TIC 268711231 & KIC 9426508 & sine \\ +G 6-7 & M4.5V & TIC 456938518 & - & sine \\ +UCAC4 683-069625 & M4.5V & TIC 159171299 & KIC 9705079 & sine \\ +2MASS J18432784+4727325 & M4Ve & TIC 123205792 & KIC 10318386 & sine \\ +2MASS J18474286+4218039 & M4Ve & TIC 123408865 & KIC 6837702 & sine \\ +2MASS J18535193+4327449 & M4Ve & TIC 164529313 & KIC 7734382 & sine \\ +2MASS J19005766+4428279 & M4Ve & TIC 164889852 & KIC 8416220 & sine \\ +2MASS J19045588+3738361 & M4Ve & TIC 120825083 & KIC 2283749 & sine \\ +CD-56 1032B & M4Ve & TIC 220433364 & - & sine \\ +Kepler-1646 & M4Ve & TIC 158552258 & KIC 7350067 & sine \\ +2MASS J21484123-4736506 & M5 & TIC 147421845 & - & sine \\ +UCAC3 53-724 & M5.5V & TIC 425937691 & - & sine \\ +G 205-40 & M5V & TIC 164458193 & KIC 9201463 & sine \\ +LP 357-206 & M5e & TIC 14079970 & - & sine \\ +LP 760-3 & M6.5V & - & - & \\ +2MASS J19202351+5037161 & M6Ve & TIC 267746625 & KIC 12108566 & sine \\ +V* V692 Tau & M: & TIC 149923415 & - & sine \\ +L 762-51 & dM3.5 & TIC 286942673 & - & \\ +GALEX J184242.4+440405 & sdB & TIC 123198279 & KIC 8142623 & sine \\ +GALEX J191612.1+474915 & sdB+F/G & TIC 158984345 & KIC 10593239 & sine \\ +SDSS J192715.88+380808.2 & sdB+dM & - & KIC 2991403 & sine \\ \end{longtable} } \ No newline at end of file diff --git a/Physics_Thesis_Template/content/appendixB.tex b/Physics_Thesis_Template/content/appendixB.tex index f35e144..9476ea7 100644 --- a/Physics_Thesis_Template/content/appendixB.tex +++ b/Physics_Thesis_Template/content/appendixB.tex @@ -1,3 +1,231 @@ \chapter{Additional folded lightcurves \label{chap:apB}} +\section{KOI-256 \label{apB:KOI-256}} + + \section{TYC 4595-107-1 \label{apB:TYC_4595-107-1}} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-14-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 14} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-18-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 18} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-19-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 19} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-24-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 24} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-25-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 25} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-26-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 26} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-40-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 40} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-41-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 41} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-47-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 47} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-51-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 51} + \end{subfigure} + \caption{Folded lightcurves for TYC 4595-107-1.} + \label{apB:fig:TYC_4595-107-1-TESS_foldedLC1} +\end{figure} +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-52-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 52} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-53-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 53} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-54-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 54} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-58-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 58} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-59-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 59} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-60-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 60} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-73-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 73} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1_TESS-74-foldedLC-marked_fit_flares.png} + \caption{TESS Sector 74} + \end{subfigure} + \caption{Folded lightcurves for TYC 4595-107-1.} + \label{apB:fig:TYC_4595-107-1-TESS_foldedLC2} +\end{figure} + +\FloatBarrier +\section{V471 Tau \label{apB:V471_tau}} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/V471Tau/V_star_ V471 Tau_TESS-42-periodFoldedLC-marked_fit_flares.png} + \caption{TESS Sector 42} + \label{apB:fig:V471Tau-TESS42} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/V471Tau/V_star_ V471 Tau_TESS-43-periodFoldedLC-marked_fit_flares.png} + \caption{TESS Sector 43} + \label{apB:fig:V471Tau-TESS43} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/V471Tau/V_star_ V471 Tau_TESS-44-periodFoldedLC-marked_fit_flares.png} + \caption{TESS Sector 44} + \label{apB:fig:V471Tau-TESS44} + \end{subfigure} + \caption{Folded lightcurves for V* V471 Tau.} + \label{apB:fig:V471Tau-TESS_foldedLC} +\end{figure} + +\FloatBarrier +\section{KOI-256 \label{apB:koi-256}} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-35-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 35} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-36-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 36} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-37-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 37} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-38-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 38} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-39-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 39} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-40-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 40} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-69-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 69} + \end{subfigure} + \caption{Folded Kepler lightcurves for KOI-256.} + \label{apB:fig:KOI-256-Kepler_foldedLC} +\end{figure} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-37-periodFoldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 37} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_Kepler-38-periodFoldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 38} + \end{subfigure} + \caption{Folded Kepler lightcurves for KOI-256 by rotational period.} + \label{apB:fig:KOI-256-Kepler_periodfoldedLC} +\end{figure} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_TESS-53-foldedLC-marked_fit_flares.png} + \caption{TESS sector 53} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_TESS-75-foldedLC-marked_fit_flares.png} + \caption{TESS sector 75} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_TESS-80-foldedLC-marked_fit_flares.png} + \caption{TESS sector 80} + \end{subfigure} + \caption{Folded TESS lightcurves for KOI-256.} + \label{apB:fig:KOI-256-TESS_foldedLC} +\end{figure} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_TESS-53-periodFoldedLC-marked_fit_flares.png} + \caption{TESS sector 53} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/KOI-256/KOI-256_TESS-80-periodFoldedLC-marked_fit_flares.png} + \caption{TESS sector 80} + \end{subfigure} + \caption{Folded TESS lightcurves for KOI-256 by rotational period.} + \label{apB:fig:KOI-256-TESS_periodfoldedLC} +\end{figure} diff --git a/Physics_Thesis_Template/content/appendixC.tex b/Physics_Thesis_Template/content/appendixC.tex index ccd27f4..6d1230a 100644 --- a/Physics_Thesis_Template/content/appendixC.tex +++ b/Physics_Thesis_Template/content/appendixC.tex @@ -1 +1,57 @@ -\chapter{Appendix C} \ No newline at end of file +\chapter{Miscellaneous lightcurves} +\label{apC} + +Appendix for miscellaneous lightcurves that can not be attributed to any of the topics, but are still noteworthy. + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.98\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/KOI-6423/2MASS J19033576+3941263_TESS-40-lc.png} + \caption{TESS Sector 40} + \label{apC:fig:KOI-6423-TESS40} + \end{subfigure} + \begin{subfigure}[b]{.98\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/KOI-6423/2MASS J19033576+3941263_TESS-41-lc.png} + \caption{TESS Sector 41} + \label{apC:fig:KOI-6423-TESS41} + \end{subfigure} + \caption{Lightcurves for 2MASS J19033576+3941263, also known as KOI-6423.} + \label{apC:fig:KOI-6423-TESS_lightcurves1} +\end{figure} +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.98\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/KOI-6423/2MASS J19033576+3941263_TESS-53-lc.png} + \caption{TESS Sector 53} + \label{apC:fig:KOI-6423-TESS53} + \end{subfigure} + \begin{subfigure}[b]{.98\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/KOI-6423/2MASS J19033576+3941263_TESS-54-lc.png} + \caption{TESS Sector 54} + \label{apC:fig:KOI-6423-TESS54} + \end{subfigure} + \caption{Lightcurves for 2MASS J19033576+3941263, also known as KOI-6423.} + \label{apC:fig:KOI-6423-TESS_lightcurves2} +\end{figure} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.98\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/V452Lyr/V_star_ V452 Lyr_Kepler-55-lc-marked_flares.png} + \caption{Kepler target table ID 55, normalized lightcurve} + \label{apC:fig:V452Lyr-Kepler55_lc} + \end{subfigure} + \begin{subfigure}[b]{.98\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/V452Lyr/V_star_ V452 Lyr_Kepler-55-flattened_lc-marked_flares.png} + \caption{Kepler target table ID 55, flattened lightcurve} + \label{apC:fig:V452Lyr-Kepler55_flattenedlc} + \end{subfigure} + \caption{Lightcurves for 2MASS J19033576+3941263, also known as KOI-6423.} + \label{apC:fig:V452Lyr-Kepler_lightcurves} +\end{figure} \ No newline at end of file diff --git a/Physics_Thesis_Template/content/chapter-conclusion.tex b/Physics_Thesis_Template/content/chapter-conclusion.tex index 3b0d235..7ee8cb5 100644 --- a/Physics_Thesis_Template/content/chapter-conclusion.tex +++ b/Physics_Thesis_Template/content/chapter-conclusion.tex @@ -1,3 +1,3 @@ \chapter{Conclusion and Outlook \label{sec:conclusion}} - +% better algorithms, handle edge cases better, analyse more stars, take kepler/k2 long cadence into consideration for more data, create plots for flare peaks between x and y diff --git a/Physics_Thesis_Template/content/chapter-data.tex b/Physics_Thesis_Template/content/chapter-data.tex index bff4a15..e5c360a 100644 --- a/Physics_Thesis_Template/content/chapter-data.tex +++ b/Physics_Thesis_Template/content/chapter-data.tex @@ -17,14 +17,16 @@ The initial dataset was taken from a list of well known flaring stars from \cite This chapter explains the methods used in this study, split into the algorithms for flare detection and folding lightcurves. Everything, like the GUI discussed in chapter \ref{sec:gui}, was written in python 3 (\cite{10.5555/1593511}). It also makes extensive use of the python packages astropy (\cite{astropy:2018}), numpy (\cite{numpy}), scipy (\cite{scipy}), pandas (\cite{pandas}) and lightkurve (\cite{lightkurve}). The focus of this chapter lays in the description of the method used to create the final output, which is less customizable than the GUI, which exposes most parameters offered in the functions of the lightkurve API. Unless stated otherwise, the default parameters are used. Furthermore for the final output only PDCSAP\_FLUX is used, which is set as the default flux in the lightkurve $LightCurve$ objects after reading the fit file. The methods are the same for both $KeplerLightCurve$ and $TessLightCurve$ subclasses. \subsection{Flare detection} +\label{sec:data:data_reduction:flare_detection} The first step is to normalize the lightcurve. This is done to apply the same thresholds to all files in later steps. An example of this is shown in figure \ref{fig:full_gui_normal_selection_normalize_options} in chapter \ref{sec:gui:data_display}. The normalization is done via the $normalize()$ function of the $LightCurve$ class of the lightkurve api. Afterwards the lightcurves are flattened by called $flatten()$ of the $LightCurve$ objects. The resulting object is then used as the base for the detection of flares. This removes all longterm trends like brightness changes due to spot modulation or similar, while retaining short term events like flares or transits. A similar approach was used by \cite{au_mic_flaring_spi}.\\ The next step is then to call $calculateFlareFitsForLightcurve()$ with the flattened lightcurve as well as the normalized lightcurve as parameters. It returns two lists of dictionaries with the data for the flare peak as well as a fit which is described in the following paragraphs. -It parses the flattened lightcurve with the scipy $find_peaks$ function. This function returns local maxima, which can be further filtered by their minimum height as well as the minimum distance of datapoints they need to be apart. The minimum distance between points is set to 1 with no minimum required height. Afterwards the found peaks are sorted by height, and the highest 100 are returned. This was found to be a good amount as the most flares per fits file found in this study were around 70 for CD-56 1032A and B.\\ +It parses the flattened lightcurve with the scipy $find\_peaks$ function. This function returns local maxima, which can be further filtered by their minimum height as well as the minimum distance of datapoints they need to be apart. The minimum distance between points is set to 1 with no minimum required height. Afterwards the found peaks are sorted by height, and the highest 100 are returned. This was found to be a good amount as the most flares per fits file found in this study were around 70 for CD-56 1032A and B.\\ Afterwards each individual peak is checked. For this purpose every datapoint of the normalized flattened lightcurve is subtracted by 1 to move the average from 1 to 0. Additionally the star and end point of the flare are estimated. This is done by checking the datapoints before and after the peak. If it finds that the flux delta is below 0.005 for three consecutive datapoints, it stops, and assumes that the last checked point is the start/end of the flare. In the case it finds an infinite or NaN value (which can happen if there are gaps in the lightcurve data), or it reaches 100 datapoints before/after it will stop. This was found to cover most flares detected and provides enough datapoints for the following steps.\\ Afterwards multiple checks are done. The first checking if the 1 datapoint before the peak, and 1 after the peak are above a threshold of 0.003, or if 2 datapoint after the peak after above the same threshold (which is a similar approach to \cite{kepler_411_study}). Afterwards it is checked if the datapoint at two indices before the peak is larger than the datapoint right before the registered peak. While this eliminates the positive detection of 2 flares in they case of them appearing very shortly after another, it was by visual inspection found to eliminate more false positives. Shortly after another appearing flares are still allowed, if the criteria are met, and theres atleast one more datapoint between the peaks. Then a fit of the flare is generated. The first half of the fit, till the peak, is that of a gaussian function, with the second half being an exponential decay (similar approach to \cite{au_mic_flaring_spi} and \cite{doyle_2018}). Then the residual sum of squares (RSS) between the fit and the flux of the flare, as well as the total sum of squares (TSS) are calculated. Afterwards R-squared is calculated, and if it is below 0.8, the flare is rejected as the flare would not have the typical form. In the last step, the location of the flare in the normalized and flattened lightcurve are compared. This step has been introduced, as in some rare cases the flattening algorithm can produce a large spike (values of 10 or higher when normalized). \subsection{Lightcurve folding} +\label{sec:data:data_reduction:lightcurve_folding} This section will mainly describe how the $getOptimizedFold()$ function works. It takes the normalized lightcurve as well as a fit type as parameters. The fit type can either be "sine" for a sine fit, "poly" for a polynomlial fit, or "linear" for a linear fit. The default value is "sine", but can be changed for each individual star in the GUI. The function at first generates two periodograms with the lightkurve function $to\_periodogram$. The first one uses the lombscargle algorithm, while the second one uses the boxleastsquares algorithm. Afterwards the 4 highest peaks of each are taken and converted into periods (unit in days). diff --git a/Physics_Thesis_Template/content/chapter-discussion.tex b/Physics_Thesis_Template/content/chapter-discussion.tex index 1bd532f..1829cfe 100644 --- a/Physics_Thesis_Template/content/chapter-discussion.tex +++ b/Physics_Thesis_Template/content/chapter-discussion.tex @@ -1,10 +1,14 @@ \chapter{Discussion \label{sec:discussion}} +The flare to spot correlation in this study is based on a large sample of known active stars, which were observed by the Kepler/K2 and TESS missions. To also catch shorter events, short-cadence data was used for Kepler/K2. Not all stars analysed were used though to generate the plots in the results section (see table \ref{apA:list_of_unused_stars}). This list contains stars that either did not match the spectral types which were analysed in this study (e.g. some A type stars from the list of stars by \cite{althukair_starlist}), could not produce valid fits (reached 30 tries during the fit optimization for folded lightcurves) or no consistent period was found. The full list of stars analyzed can be found in table \ref{apA:list_of_all_stars}.\\ +The analysis was done with a self written python program (discussed in chapter \ref{sec:gui}). The reason a GUI was made was for ease of management of the data (e.g. easily looking up parameters of a star), as well as checking individual results in a fast and easy way during the development stage. This also allowed to quickly compare the outputs of the algorithms between different fits files of the same star as well as between different stars fits files. The algorithms are based on the approaches of \cite{kepler_411_study}, \cite{au_mic_flaring_spi} and \cite{doyle_2018}. The thresholds described in section \ref{sec:data:data_reduction:flare_detection} for the flare detection algorithm have been set by trial and visual inspection of the lightcurves of multiple stars/fits files. The last step for flare detection, which was introduced to prevent failures of the flattening algorithm to be detected as (massive) flares, was introduced due to the results for the stars 2MASS J19033576+3941263 (TESS sectors 40, 41 and 53), 2MASS J19370439+4626209 (TESS sector 54) and V* V452 Lyr (Kepler target table ID 55). 2MASS J19033576+3941263, also known by KOI-6423 or KIC 4544623 shows regular dips in its lightcurve, which could indicate one or multiple transiting planets. It has currently been marked as a false positive candidate in the NASA Exoplanet Archive (\cite{koidr25}, \href{https://exoplanetarchive.ipac.caltech.edu/overview/KOI-6423}{https://exoplanetarchive.ipac.caltech.edu/overview/KOI-6423}). The TESS lightcurves for KOI-6423 can be found in appendix \ref{apC} in figures \ref{apC:fig:KOI-6423-TESS_lightcurves1} and \ref{apC:fig:KOI-6423-TESS_lightcurves2}. While there are no noteworthy dips upon manual inspection in the lightcurve for 2MASS J19370439+4626209, flattening it still generates peaks of over 800 on a normalized lightcurve. V* V452 Lyr was observed in multiple Kepler target table IDs, with the only detected flares (4 total) in target table ID 55. The lightcurve itself is very flat (see figure \ref{apC:fig:V452Lyr-Kepler_lightcurves} in appendix \ref{apC}). Further to notice, the flare detection can only distinguish high and low flare peaks, but it does not calculate the flare energy.\\ +While the folding algorithm (see section \ref{sec:data:data_reduction:lightcurve_folding}) works on most stars/fits files, it has its limitations in edge cases like V* HK Aqr or KOI-256 as described in sections \ref{results:hk_aqr} and \ref{results:koi_256}. It is set to check for an additional periodicity signal if the fit for the folded lightcurve has two peaks which are further than 10\% of the total phase from the edge. While it is expected to find two peaks when folding and fitting a sine function due to marging of error of the fitting parameters, there has to be set a limit for when to search for additional periodicity. A well working (and near perfect) example is V471 Tau. It shows additional periodicity in the TESS lightcurves 42, 32 and 44 (see figure \ref{apB:fig:V471Tau-TESS_foldedLC} in appendix \ref{chap:apB}), but not 70 and 71. Additionally the shift by the difference of the fit minimum to the (currently used) epoch for the fold is necessary to generate reliable results, as otherwise it has been found the minimum of the fit/folded lightcurve can vary by up to \textasciitilde25\% depending on which first minimum is detected in the lightcurve.\\\\ +Out of a total of \textasciitilde160 M dwarfs in the list of stars to be analyzed, flares could only be detected on 49 stars. This could be due to a not sensitive enough algorithm or instruments, too noisy data or it could be that there were just no flares during the observation time. For the remaining 49 stars, a total of \textasciitilde3500 flares were detected. Using all available flares, there was no significant spot dependency detected in the histogram with 10 bins. In the third bin there were \textasciitilde50 flares less detected compared to other bins. This bin is located in the transition from the phase maxima to minima. While not being significant, the 6th bin has the most flares detected, which would be at the phase minimum. This could show a possible dependency with more available data. The data also contains the detected flares from KOI-256 and V* HK Aqr, which were not folded correctly. Manually comparing the results for V* HK Aqr (figures \ref{fig:HKAqr-Flarecount-10_Bins} and \ref{fig:HKAqr-Flarecount-10_Bins_Period}), as well as the folded lightcurves shows that for TESS sector 29 the detected minimum ($\pm$ quarter of the phase) the amount of detected flares flipped. While more flares should be counted in the minimum (see figure \ref{fig:HKAqr-TESS29_foldedLC_Period}) compared to the maximum (see figure \ref{fig:HKAqr-TESS29_foldedLC}), the opposite is the case. Similarly for TESS sector 42. Overall these changes make the spot dependence of flares on V* HK Aqr more clear, as the histogram (10 bins) with only the rotational period folded lightcurves indicates a spot dependency. There are significantly more flares counted around the minimum compared to the phase maximum. The flares with the highest peaks V* HK Aqr were also detected during the phase minimum in TESS sector 29 with a normalized peak of up to 1.8. KOI-256 shows a similar behaviour, showing a clear spot dependence when using only period folded lightcurves for the histogram, while having more spread out peaks around the phase minimum when using all spot modulation folded lightcurves.\\ +2MASS J19230963+3739397 on the other hand is a star, which shows an inverted spot dependency. This could be an indication that similarly to what \cite{kepler_411_210_comparison} found, the spot area is not the only important parameter.\\ +Limiting the flare by maximum flare peak height indicates a dependency of flares on spots. While no flare energies were calculated in this study, this could be parameters to look at in the future. Limiting the flare peak to 1\% above the flux shows a higher count in the phase maxima compared to he phase minima. The same dip as with all flares can be seen here already too. Increasing the flare peak limit to 5\% above the flux shows a nearly identical histogram (in form) to the one with all flares. A noteworthy difference here is the peak in the bin at the phase minimum at $1 \pi$. \cite{connection_starspots_flares_ms_kepler} found an increase of flares in M and K dwarfs at phase minimum with flares which had a flux increase at their peaks between 1\% and 5\%. The differences could be due to a different set of stars and flare detection methods. -%methods: lombscargle generally finds lower periods with higher peaks (e.g. halfs of rotational period), which boxleastsquares does not always detect within the 4 highest - - +% 14 - 10; 10 - 14 %M dwarfs, all data, no significant dependency of flare appearance on phase using 10 bins. %30 bins -> either 2 dips during the transition minima <-> maxima or increase of flare occurance during minima and maxima. %Looking at stronger flares only (min 1.25/1.5 flare peak) peaks during minima, stronger peak during phase maxima, in both 10 and 30 bin histograms. @@ -12,16 +16,28 @@ %Limit to max 1.05, nearly identical histograms to all data. (different result to \cite{connection_starspots_flares_ms_kepler}) %\\\\ +Out of a total of \textasciitilde40 K dwarfs in the list of stars to be analyzed, flares could only be detected on 37 stars. This could be due to a not sensitive enough algorithm or instruments, too noisy data or it could be that there were just no flares during the observation time. Overall the results for the flare distribution on K dwarfs is similar to those of M dwarfs. There is no real dependence on spots visible, with the exception of the bin (bins for the histogram with 30 bins) around the phase minimum. One of the causes for this is V* V471 Tau (see section \ref{results:v471_tau}), which is in close orbit with a white dwarf (\cite{v471tau_revised}, \cite{V471tau_magnetic_activity}). This can lead to magnetic interactions between the K dwarf and the white dwarf (\cite{V471tau_magnetic_activity}), which could lead to the increased flarecount seen.\\ +Limiting the flare peaks to greater than 5\% of the flux shows two peaks around the center bin, with one higher bin being at the maximum at phase $0 \pi$. While the two peaks around the phase minimum could indicate a dependency on spots, it is not the only relevant bin found. +Limiting the flare peaks to a maximum of 1\% above the flux shows an interesting pattern. There is a larger count of flares found during the phase minimum, but also during the phase maximum, while less flares have been detected in the transition between phase miminum/maximum. Increasing the allowed flare peak to 5\% above the flux shows a similar pattern, but the gaps between peaks/dips closes and is already very similar to the histogram with all flares. + % K dwarfs, all data, siginificant peak at phase minimum, peak dominated by V471 Tau (discussed later). Slightly more flares from maximum to minimum than minimum to maximum in 10 bins. 30 bins larger dips but also larger peaks in second half of phase compared to first half. % limiting to min 1.05 -> three peaks, dip after maximum and on at phase 1 $\pi$. gradual decrease after minimum. V471 Taus peaks at right before and right after phase minimum. % limiting to <1.01 and 1.05, makes histogram look more and more like with all data, similarly to \cite{connection_starspots_flares_ms_kepler} peak in center (compared to their M/K plot), but additionally also peak at phase maximum. % max 1.05 already most flares, very similar to with all data. +Out of a total of \textasciitilde80 G dwarfs in the list of stars to be analyzed, flares could only be detected on 21 stars. This could be due to a not sensitive enough algorithm or instruments, too noisy data or it could be that there were just no flares during the observation time. Most of the flares detected had a peak below 5\% above the flux, but as \cite{solar_like_superflares} found, flares with a flux increase between 0.1 to 1\% would already be categorized as superflares. For the flares found in this study for G type stars, there appears to be a spot dependency, as the flare count peaks around the phase minimum. Unlike the other results, there is a gradual fall off to each sides till the phase maximum is reached.\\ +Limiting the flare peaks to a minimum of 1.05 shows three major peaks. The highest being at the phase minimum, while the other two are in the transition between maximum and miminum and minimum and maximum. This does not indicate a pure spot dependency, and a more detailed look at the individual events is necessary.\\ +BD-08 995, which seems to be a late G type star, reflects this trend well. It shows the same bell curve style histogram. Additionally though it also shows a slight increase in flares around the phase maximum. Its highest flare peak was detected around the phase maximum though. The maximum flare count for TYC 4595-107-1 on the other hand is slightly offset to before the phase minimum. It also shows a slight increase of flares around the maximum. Its highest flare peak was detected in the same bin as the highest flare count. + % G dwarfs, significant results, increase of flare appearance during phase minimum. Most flares are <1.05 (flares on solar like stars that increase brightness by 0.1\% to 1\% already superflares, \cite{solar_like_superflares}) -> most/all detected flares superflares. Overall dependency on phase/spot appearance. % Limiting to flares >1.05 -> flares during minima and transitions between minima <-> maxima, increasing bins -> more data would be required. +Out of a total of \textasciitilde13 F dwarfs in the list of stars to be analyzed, flares could only be detected on 4 stars. This could be due to a not sensitive enough algorithm or instruments, too noisy data or it could be that there were just no flares during the observation time. While all flares detected are centered around the phase minimum, the total of 5 flares detected is not a large enough sample to come to a conclusion if there exists a flare spot dependency for these stars. + % For F dwarfs, overall too little data, but the not siginificant amount detected all during phase minimum, could be similar to G dwarfs? +Looking at all results together, there appears to be a slight flare dependence, which is mostly influenced by the results for K and G stars. The dip in the otherwise seemingly stable histogram for the results of M dwarfs propagates for the overall results. + % All data combined, peak at phase minimum dominated by G/K dwarfs, dip in transition maxima -> minima dominated by dip from M dwarf results. % Individual star results (subset taken): diff --git a/Physics_Thesis_Template/content/chapter-introduction.tex b/Physics_Thesis_Template/content/chapter-introduction.tex index 6cac9a5..8b727b8 100644 --- a/Physics_Thesis_Template/content/chapter-introduction.tex +++ b/Physics_Thesis_Template/content/chapter-introduction.tex @@ -7,12 +7,12 @@ This chapter gives an introduction to the goals of this study. Afterwards there \section{Goals and current knowledge \label{sec:intro:goals}} The goal of this study is to relate flares/superflares to the appearance of spots on the surfaces of stars of various spectral types. Flares are well studied for the sun (\cite{solar_flares_1}, \cite{solar_flares_2}, \cite{solar_flares_3}) as well as its impact on earths magnetic field (\cite{solar_flare_mag_field}). While the first stellar flares were discovered in middle of the last century (\cite{early_stellar_flares1}, \cite{early_stellar_flares2}), the topic gained a lot of traction with the launch of the likes of Kepler and the Transiting Exoplanet Survey Satellite (TESS). They allowed the survey of thousands of stars. With this, studies of flares and superflares on a large number of stars have been conducted (e.g. \cite{flare_study_1}, \cite{flare_study_2}, \cite{connection_starspots_flares_ms_kepler}, \cite{flare_occurance_periodicity}), but the origin of superflares (flares with an energy above $10^{33}$ erg) is still not clear. So far no superflare has been observed on our sun, but there have been studies focusing on the possible origin on superflares and their likelyhood to happen on our sun (\cite{superflares_on_sun}). They found that superflares on our sun would be rare events (every \textasciitilde800 years for superflares with $10^{34}$ erg).\\ -A few proposed caused could be star-planet interaction (SPI) (\cite{au_mic_flaring_spi}, \cite{SPI_1}, \cite{SPI_2}), or just being scaled up version of normal flares which we see from our sun coming from large spots (\cite{superflares_1}, \cite{superflares_2}).\\ -\cite{kepler_411_study} focused on Kepler-411 by investigating the relation between superflares and star spots on that star. They found a positive correlation between the energy of flares and the area of star spots (\cite{kepler_411_study}) on Kepler-411. They then compared their results for Kepler-411, which produced multiple superflares, with Kepler-210, which did not produce superflares while having the same number of spots (\cite{kepler_411_210_comparison}). They found the spots on Kepler-210 to be larger, warmer and therefor being magnetically weaker/less complex compared to Kepler-411 and concluded that the area of starspots is not the only relevant parameter for superflare occurance (\cite{kepler_411_210_comparison}).\\ -\cite{doyle_2018} studied 34 M dwarfs from the K2 mission, using short cadence observational data. They confirmed that stars with a rotational period of less than 10 days showed more flares, which was already shown previously (\cite{faster_rot_stars_more_flares1}, \cite{faster_rot_stars_more_flares2}). Furthermore they found no star with a preference for when flares occured during the rotational phase (\cite{doyle_2018}). A similar study using TESS 2 minute cadence data has been conducted by \cite{doyle_2019}. In this study they used data of 167 M dwarfs and found a total of 1834 flares. Similar to the study on K2 data, they found no preference for roational phase (\cite{doyle_2019}).\\ -Another possible cause for a periodic increase in flares is star-planet interaction (SPI), which is studied by \cite{au_mic_flaring_spi} for the star AU Mic. While they found a signal in their used TESS lightcurves correlating with the orbital period of AU Mic b, they require more observation time to get a $>3\sigma$ detection (\cite{au_mic_flaring_spi}).\\ +A few proposed causes could be star-planet interaction (SPI) (\cite{au_mic_flaring_spi}, \cite{SPI_1}, \cite{SPI_2}), or just being scaled up version of normal flares which we see from our sun coming from large spots (\cite{superflares_1}, \cite{superflares_2}).\\ +\cite{doyle_2018} studied 34 M dwarfs from the K2 mission, using short cadence observational data. They confirmed that the stars in their dataset with a rotational period of less than 10 days showed more flares, which was already shown previously (\cite{faster_rot_stars_more_flares1}, \cite{faster_rot_stars_more_flares2}). Furthermore they found no star with a preference for when flares occured during the rotational phase (\cite{doyle_2018}). A similar study using TESS 2 minute cadence data has been conducted by \cite{doyle_2019}. In this study they used data of 167 M dwarfs and found a total of 1834 flares. Similar to the study on K2 data, they found no preference for roational phase (\cite{doyle_2019}).\\ Further analysis on periodic flare occurance was done by \cite{flare_occurance_periodicity}, who studied lightcurves of 284 M dwarfs. They found three targets (TIC 80427281, TIC 95328477, TIC 220432563) with a confirmed flare periodicity, which correlates to their rotational period or half of it.\\ -\cite{connection_starspots_flares_ms_kepler} investigated a sample of 119 stars from spectral types M to F. They found that flares which increase the stellar flux by 1\% to 5\% appear more often while larger starspots are visible, while flares which increase the flux by more that 5\% do not seem to have this dependency (\cite{connection_starspots_flares_ms_kepler}). +\cite{connection_starspots_flares_ms_kepler} investigated a sample of 119 stars from spectral types M to F. They found that flares which increase the stellar flux by 1\% to 5\% appear more often while larger starspots are visible, while flares which increase the flux by more that 5\% do not seem to have this dependency (\cite{connection_starspots_flares_ms_kepler}).\\ +There have also been studies on individual stars, for example \cite{kepler_411_study} focused on Kepler-411 by investigating the relation between superflares and star spots on that star. They found a positive correlation between the energy of flares and the area of star spots (\cite{kepler_411_study}) on Kepler-411. They then compared their results for Kepler-411, which produced multiple superflares, with Kepler-210, which did not produce superflares while having the same number of spots (\cite{kepler_411_210_comparison}). They found the spots on Kepler-210 to be larger, warmer and therefor being magnetically weaker/less complex compared to Kepler-411 and concluded that the area of starspots is not the only relevant parameter for superflare occurance (\cite{kepler_411_210_comparison}). Star-planet interaction is studied by \cite{au_mic_flaring_spi} for the star AU Mic. While they found a signal in their used TESS lightcurves correlating with the orbital period of AU Mic b, they require more observation time to get a $>3\sigma$ detection (\cite{au_mic_flaring_spi}).\\ +In coclusion, many flares and superflares have been found on stars, but the origin of the later is still not clear. There are a few ongoing possible origins like star-planet interaction (or interactions with other close companions) or them coming from larger, more complex starspots. \section{Spectral Types \label{sec:intro:spectral_types}} @@ -40,7 +40,7 @@ The spectral types are a way to classify the vast amount of stars into various t % Different Spectral Types -\section{Flares and Starspots \label{sec:intro:flares_and_spots}} +\section{Flares and Spots \label{sec:intro:flares_and_spots}} % Stellar Activity, @@ -48,6 +48,14 @@ The spectral types are a way to classify the vast amount of stars into various t % TESS, Kepler/K2 +\subsection{Kepler} + + +\subsection{K2} + + +\subsection{TESS} + %\section{Current knowledge \label{sec:intro:current_knowledge}} diff --git a/Physics_Thesis_Template/content/chapter-results.tex b/Physics_Thesis_Template/content/chapter-results.tex index b07f97d..7542b6e 100644 --- a/Physics_Thesis_Template/content/chapter-results.tex +++ b/Physics_Thesis_Template/content/chapter-results.tex @@ -6,7 +6,7 @@ The results also only contain the data of folded lightcurves which could be fitt \section{M dwarfs \label{sec:results:m_dwarfs}} -This section shows the results for all 144 M dwarfs in this study. The list of stars can be found in table \ref{apA:list_of_m_stars}.\\ +This section shows the results for 49 M dwarfs for which flares could be detected. The list of stars can be found in table \ref{apA:list_of_m_stars}.\\ Figures \ref{fig:M-Flarecount-10_Bins} and \ref{fig:M-Flarecount-30_Bins} show histograms, with 10 and 30 bins respectively, of the amount of flares during the normalized phase.\\ Looking at figure \ref{fig:M-Flarecount-10_Bins} there is an even distribution within error of flares across the normalized phase, with the excepion of the bin at phase $0.5 \pi$. The bin at phase $0.5 \pi$ shows a significant dip of roughly twice the error below the surrounding bins.\\ Looking at the same data, just with 30 instead of 10 bins (figure \ref{fig:M-Flarecount-30_Bins}), the same dip is visible. In this figure the dip spans 3 bins. Additionally there are additional dips at around phase $0.7 \pi$, $1.3 \pi$ and $1.4 \pi$. Including the error, the major dip (which was already visible in figure \ref{fig:M-Flarecount-10_Bins}) is still below the average. Similar for the dips at phases $0.7 \pi$ and $1.3 \pi$. The dip at phase $1.4 \pi$ on the other hand overlaps with its error with the errorbars of the bins at phase \textasciitilde$1.7 \pi$ and and onward, which are good assumption for an average value. Due to the dips surrounding the center, it may look like there is an increased number of flares in the center. If we look at the errorbars, it is clear that only the bin at phase \textasciitilde$1.25 \pi$ is above the average. @@ -25,7 +25,7 @@ Looking at the same data, just with 30 instead of 10 bins (figure \ref{fig:M-Fla \caption{30 bins} \label{fig:M-Flarecount-30_Bins} \end{subfigure} - \caption{Histogram showing the amount of flares per phase for all 144 M dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:M-Flarecount-10_Bins})/30 bins (\subref{fig:M-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histogram showing the amount of flares per phase of 49 M dwarfs for which flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:M-Flarecount-10_Bins})/30 bins (\subref{fig:M-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:M-Flarecount} \end{figure} @@ -50,7 +50,7 @@ Increasing the bin count to 30 (see figure \ref{fig:M-Flarecount-30_Bins_1.5_pea \caption{30 bins} \label{fig:M-Flarecount-30_Bins_1.25_peak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.25 per phase for all 144 M dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.25_peak}) /30 (\subref{fig:M-Flarecount-30_Bins_1.25_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.25 per phase of 27 M dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.25_peak}) /30 (\subref{fig:M-Flarecount-30_Bins_1.25_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:M-Flarecount-peaks_1.25_peak} \end{figure} \begin{figure}[pt!] @@ -67,7 +67,7 @@ Increasing the bin count to 30 (see figure \ref{fig:M-Flarecount-30_Bins_1.5_pea \caption{30 bins} \label{fig:M-Flarecount-30_Bins_1.5_peak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.5 per phase for all 144 M dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.5_peak})/30 (\subref{fig:M-Flarecount-30_Bins_1.5_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.5 per phase for 20 M dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.5_peak})/30 (\subref{fig:M-Flarecount-30_Bins_1.5_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:M-Flarecount-peaks_1.5_peak} \end{figure} @@ -90,7 +90,7 @@ The difference becomes less obvious when increasing the bin size 30 (figure \ref \caption{30 bins} \label{fig:M-Flarecount-30_Bins_1.01_maxpeak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of less than 1.01 per phase for all 144 M dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.01_maxpeak})/30 (\subref{fig:M-Flarecount-30_Bins_1.01_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of less than 1.01 per phase of 17 M dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.01_maxpeak})/30 (\subref{fig:M-Flarecount-30_Bins_1.01_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:M-Flarecount-peaks_1.01_maxpeak} \end{figure} @@ -108,14 +108,14 @@ The difference becomes less obvious when increasing the bin size 30 (figure \ref \caption{30 bins} \label{fig:M-Flarecount-30_Bins_1.05_maxpeak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of less than 1.05 per phase for all 144 M dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.05_maxpeak})/30 (\subref{fig:M-Flarecount-30_Bins_1.05_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of less than 1.05 per phase of 32 M dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:M-Flarecount-10_Bins_1.05_maxpeak})/30 (\subref{fig:M-Flarecount-30_Bins_1.05_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:M-Flarecount-peaks_1.05_maxpeak} \end{figure} \FloatBarrier \section{K dwarfs \label{sec:results:k_dwarfs}} -This section shows the results for all 37 K dwarfs in this study. A full list of the stars used can be found in table \ref{apA:list_of_k_stars}.\\ +This section shows the results for 37 K dwarfs for which flares could be detected. A full list of the stars used can be found in table \ref{apA:list_of_k_stars}.\\ Figure \ref{fig:K-Flarecount-10_Bins} shows the amount of flares per phase with 10 bins of 37 K type dwarfs in used in this study. Overall the distribution is even within error, with a slight increase in flares when going from the maximum to the minimum of the lightcurve at phase $0.5 \pi$, and a slight decrease when going from minimum to maximum at phase $1.5 \pi$. There is also a peak at around $1 \pi$ with around 95 flares compared to the 60-80 flares per bin in the rest of the histogram. This peak is dominated by $V*~V471~Tau$. The individual results for this star are visible in section \ref{sec:results:individual}.\\ Looking at the same dataset with 30 bins for the histogram (figure \ref{fig:K-Flarecount-30_Bins}), the peak in the phase minimum at $1 \pi$ is still visible. Additionally there appear more peaks at phase $>1.3 \pi$ ($1.3,~1.6,~1.9 \pi$), while the amount of flares between phase $0 \pi$ and $1 \pi$ shows a slight trend to more flares with dips inbetween and a larger dip right before and after the big peak at phase $1 \pi$ which was also visible in figure \ref{fig:K-Flarecount-10_Bins} with 10 bins. The major dips at phase $0.7 \pi$, $1.3 \pi$, $1.6 \pi$ and $1.9 \pi$ are all well outside the errorbars of the surrounding peak bins, while the smaller ones between phase $0 \pi$ and $1 \pi$ overlap with their errorbars with their surrounding bins. @@ -133,7 +133,7 @@ Looking at the same dataset with 30 bins for the histogram (figure \ref{fig:K-Fl \caption{30 bins} \label{fig:K-Flarecount-30_Bins} \end{subfigure} - \caption{Histogram showing the amount of flares per phase for all 37 K dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:K-Flarecount-10_Bins})/30 bins (\subref{fig:K-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histogram showing the amount of flares per phase of 37 K dwarfs for which flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:K-Flarecount-10_Bins})/30 bins (\subref{fig:K-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:K-Flarecount} \end{figure} @@ -155,7 +155,7 @@ A similar picture forms when increasing the bin count to 30 (figure \ref{fig:K-F \caption{30 bins} \label{fig:K-Flarecount-30_Bins_1.05_peak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.05 per phase for all 37 K dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:K-Flarecount-10_Bins_1.05_peak})/30 (\subref{fig:K-Flarecount-30_Bins_1.05_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.05 per phase of 13 K dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:K-Flarecount-10_Bins_1.05_peak})/30 (\subref{fig:K-Flarecount-30_Bins_1.05_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:K-Flarecount-peaks_1.5_peak} \end{figure} @@ -178,7 +178,7 @@ Increasing the bins to 30 (figure \ref{fig:K-Flarecount-30_Bins_1.05_maxpeak}) s \caption{30 bins} \label{fig:K-Flarecount-30_Bins_1.01_maxpeak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of less than 1.01 per phase for all 37 K dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:K-Flarecount-10_Bins_1.01_maxpeak})/30 (\subref{fig:K-Flarecount-30_Bins_1.01_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of less than 1.01 per phase of 20 K dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:K-Flarecount-10_Bins_1.01_maxpeak})/30 (\subref{fig:K-Flarecount-30_Bins_1.01_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:K-Flarecount-peaks_1.01_maxpeak} \end{figure} @@ -198,14 +198,14 @@ Increasing the bins to 30 (figure \ref{fig:K-Flarecount-30_Bins_1.05_maxpeak}) s \caption{30 bins} \label{fig:K-Flarecount-30_Bins_1.05_maxpeak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of less than 1.05 per phase for all 37 K dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:K-Flarecount-10_Bins_1.05_maxpeak})/30 (\subref{fig:K-Flarecount-30_Bins_1.05_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of less than 1.05 per phase of 20 K dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:K-Flarecount-10_Bins_1.05_maxpeak})/30 (\subref{fig:K-Flarecount-30_Bins_1.05_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:K-Flarecount-peaks_1.05_maxpeak} \end{figure} \FloatBarrier \section{G dwarfs \label{sec:results:g_dwarfs}} -This section shows the results for 71 G dwarfs in this study. Table \ref{apA:list_of_g_stars} contains a list of all G type stars used.\\ +This section shows the results for 21 G dwarfs for which flares could be detected. Table \ref{apA:list_of_g_stars} contains a list of all G type stars used.\\ The first histogram over all data of G type dwarfs with 10 bins in figure \ref{fig:G-Flarecount-10_Bins} shows a significant increase of occuring flares well outside the errorbar range in the lightcurve minima at around phase $1 \pi$ compared to the maxima at phase $0 \pi$/$2 \pi$. The rise in flare occurances from maxima to minima (phase $0 \pi$ to $1 \pi$) seems to be gradual, while there is a steep fall off after the sixth bin at phase $1.1 \pi$.\\ Due to the lower number of detected flares on G type stars, the error bars in figure \ref{fig:G-Flarecount-30_Bins} are rather large. The increase of flares in the minima of the folded lightcurve from the previous figure is now splint into two peaks at phase $0.6 \pi$ and $1 \pi$. An additional peak bin appears at around phase $0.25 \pi$ in this figure. This peaks errorbar does not overlap with its surrounding bins errorbars. Right before this peak is a significant dip visible at phase $0.2 \pi$. On the other half of the phase after the peak at phase $1 \pi$, the near even distribution of figure \ref{fig:G-Flarecount-10_Bins} becomes more noisy, even though its still well within error.\\ Limiting the flare peaks to <1.05 (figure \ref{fig:G-Flarecount-peaks_1.05_maxpeak}) does not change the resulting histograms much. There are only miniscule differences, mainly the bin at phase $1.1 \pi$ is now slightly smaller relative to the two prior bins in figure \ref{fig:G-Flarecount-10_Bins_1.05_maxpeak} compared to figure \ref{fig:G-Flarecount-10_Bins} with all flares. @@ -224,7 +224,7 @@ Limiting the flare peaks to <1.05 (figure \ref{fig:G-Flarecount-peaks_1.05_maxpe \caption{30 bins} \label{fig:G-Flarecount-30_Bins} \end{subfigure} - \caption{Histogram showing the amount of flares per phase for all 71 G dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:G-Flarecount-10_Bins})/30 bins (\subref{fig:G-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histogram showing the amount of flares per phase of 21 G dwarfs for which flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:G-Flarecount-10_Bins})/30 bins (\subref{fig:G-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:G-Flarecount} \end{figure} @@ -245,7 +245,7 @@ Increasing the bins to 30, which is seen in figure \ref{fig:G-Flarecount-30_Bins \caption{30 bins} \label{fig:G-Flarecount-30_Bins_1.05_maxpeak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of less than 1.05 per phase for all 37 K dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:G-Flarecount-10_Bins_1.05_maxpeak})/30 (\subref{fig:G-Flarecount-30_Bins_1.05_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of less than 1.05 per phase of 16 G dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:G-Flarecount-10_Bins_1.05_maxpeak})/30 (\subref{fig:G-Flarecount-30_Bins_1.05_maxpeak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:G-Flarecount-peaks_1.05_maxpeak} \end{figure} @@ -263,14 +263,14 @@ Increasing the bins to 30, which is seen in figure \ref{fig:G-Flarecount-30_Bins \caption{30 bins} \label{fig:G-Flarecount-30_Bins_1.05_peak} \end{subfigure} - \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.05 per phase for all 71 G dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:G-Flarecount-10_Bins_1.05_peak})/30 (\subref{fig:G-Flarecount-30_Bins_1.05_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares with a normalized peak of greater than 1.05 per phase of 13 G dwarfs for which such flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 (\subref{fig:G-Flarecount-10_Bins_1.05_peak})/30 (\subref{fig:G-Flarecount-30_Bins_1.05_peak}) bins of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:G-Flarecount-peaks_1.5_peak} \end{figure} \FloatBarrier \section{F dwarfs \label{sec:results:f_dwarfs}} -This section shows the results for all 13 F dwarfs in this study. The list of F type stars can be found in table \ref{apA:list_of_f_stars}.\\ +This section shows the results for 4 F dwarfs for which flares could be detected. The list of F type stars can be found in table \ref{apA:list_of_f_stars}.\\ Due to the low number of F type stars in this study, and the difficulty to detect flares on them, the detected number of flares in figures \ref{fig:F-Flarecount-10_Bins} and \ref{fig:F-Flarecount-30_Bins} is very low which causes the errorbars of the histogram to grow very large. Nontheless all detected flares were around the minimum of the lightcurves. \begin{figure}[pt!] @@ -287,14 +287,14 @@ Due to the low number of F type stars in this study, and the difficulty to detec \caption{30 bins} \label{fig:F-Flarecount-30_Bins} \end{subfigure} - \caption{Histogram showing the amount of flares per phase for all 13 F dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:F-Flarecount-10_Bins})/30 bins (\subref{fig:F-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histogram showing the amount of flares per phase of 4 F dwarfs for which flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:F-Flarecount-10_Bins})/30 bins (\subref{fig:F-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:F-Flarecount} \end{figure} \FloatBarrier \section{Combined results \label{sec:results:combined}} -The results for all 265 stars in the study are shown in this chapter. This includes the stars from tables \ref{apA:list_of_m_stars} to \ref{apA:list_of_f_stars}. The histograms in figure \ref{fig:MKGF-Flarecount-10_Bins} and \ref{fig:MKGF-Flarecount-30_Bins} are stacked histograms. The flare amount of the individual stars are per bin are stacked on top of each other resulting in the final value.\\ +The results for all 95 stars in the study for which flares could be detected. This includes the stars from tables \ref{apA:list_of_m_stars} to \ref{apA:list_of_f_stars}. The histograms in figure \ref{fig:MKGF-Flarecount-10_Bins} and \ref{fig:MKGF-Flarecount-30_Bins} are stacked histograms. The flare amount of the individual stars are per bin are stacked on top of each other resulting in the final value.\\ The dip at phase $0.5 \pi$ which was present in the histogram for the M type stars (see figure \ref{fig:M-Flarecount-10_Bins} in section \ref{sec:results:m_dwarfs}) propagates and casues the dip to be also visible in figure \ref{fig:MKGF-Flarecount-10_Bins}. The peak at phase $1 \pi$ is also a result of propagation, but from the K and G type star data. Due to the large number of overall flares, the errorbars are small and the errorbars of the peak in the center at phase $1 \pi$ does not overlap with the other errorbars.\\ Looking at the same data with 30 bins over the phase in figure \ref{fig:MKGF-Flarecount-30_Bins}, the propagation of the variation in the data of the M type stars is clearly visible with the dip around phase $0.5 \pi$ and $1.4 \pi$. Additionally the peaks from the data of K (figure \ref{fig:K-Flarecount-30_Bins}) and G (figure \ref{fig:G-Flarecount-30_Bins}) type stars cause a wider peak at around phase $1 \pi$. Additionally there are also smaller, especially less wide peaks at around phases $0.4 \pi$, $0.7 \pi$ and $1.5 \pi$. @@ -312,7 +312,7 @@ Looking at the same data with 30 bins over the phase in figure \ref{fig:MKGF-Fla \caption{30 bins} \label{fig:MKGF-Flarecount-30_Bins} \end{subfigure} - \caption{Histograms showing the amount of flares per phase for all 265 dwarfs used in this study. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:MKGF-Flarecount-10_Bins})/30 bins (\subref{fig:MKGF-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The colors show the individual amount for each spectral type with the amount being stacked ontop of each other. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} + \caption{Histograms showing the amount of flares per phase for all 95 dwarfs for which flares could be detected. The x-axis represents the normalized phase of the folded lightcurves. There are 10 bins (\subref{fig:MKGF-Flarecount-10_Bins})/30 bins (\subref{fig:MKGF-Flarecount-30_Bins}) of the phase, showing the number of flares per bin. The colors show the individual amount for each spectral type with the amount being stacked ontop of each other. The error bar shows the standard deviation for the histogram. The blue line indicates an idialized phase (sine curve), with the maximum at phase $0 \pi$/$2 \pi$ and the minimum at phase $1 \pi$.} \label{fig:MKGF-Flarecount} \end{figure} @@ -323,7 +323,7 @@ This section contains a selection of results for individual stars. The results f \subsection{BD-08 995} -BD-08 995, also known by TIC 43472154, is a G type star with a surface temperature of 5231.2 K, which is \textasciitilde87 pc away. It is a very active solar like star, producing over 200 superflares per year (\cite{tess_1st_year_superflares}). It has a rotational period of 2.8 days (\cite{tess_1st_year_superflares}). There are two TESS lightcurves available, sectors 5 and 32.\\ +BD-08 995, also known by TIC 43472154, is a G type star with a surface temperature of 5316 K (\cite{revised_tess_input_catalogue}), which is \textasciitilde87 pc away (\cite{simbad}). It is a very active solar like star, producing over 200 superflares per year (\cite{tess_1st_year_superflares}). It has a rotational period of 2.8 days (\cite{tess_1st_year_superflares}). There are two TESS lightcurves available, sectors 5 and 32.\\ Looking at figure \ref{fig:BD-08_995-Flarecount-10_Bins}, which shows the flare distribution across the normalized phase of the folded lightcurves with 10 bins, it shows a clear peak of flares appearance in the lightcurve minima at phase $1 \pi$. The errorbars of this wide peak only overlap with the first bin of the plot at phase $0 \pi$. This bin belong to the phase maxima which also shows slight increase in flare activity at phase $0/2 \pi$ compared to the transition regions at around phase $0.5 \pi$ (maxima to minima) and $1.5 \pi$ (minima to maxima). Considering errors for this, the errorbars of the bins at the phase maxima overlap with those of the transition regions.\\ Figure \ref{fig:BD-08_995-Flarecount-30_Bins} shows the same data just with 30 bins instead of 10. Ignoring the errorbars, it shows a similar picture as the previous figure. But due to the low number of total detected flares, and a the relatively large bin count, the errorbars become large compared to the individual bins. Due to this, the errorbars of most bins overlap with each other, with the exceptions of the the first bin at phase $0 \pi$ and the bin at phase \textasciitilde$1.1 \pi$, whichs erorbars only overlap with other higher bins like the ones at phase \textasciitilde$0.9 \pi$ and \textasciitilde$1.4 \pi$. @@ -460,7 +460,8 @@ The histogram with 30 bins (figure \ref{fig:TYC_4595-107-1-Flarecount-30_Bins}) \label{fig:TYC_4595-107-1-Flarecount} \end{figure} -The flare peak at normalized phase distribution can be seen in figure \ref{fig:TYC_4595-107-1-flarepeaks_1.27}. The strongest flare was detected at normalized phase \textasciitilde$0.8 \pi$. Two sligthly higher flare peaks have been detected at phases $0.5 \pi$ and $2 \pi$ respectively, but otherwise there does not seem to be any pattern. +The flare peak at normalized phase distribution can be seen in figure \ref{fig:TYC_4595-107-1-flarepeaks_1.27}. The strongest flare was detected at normalized phase \textasciitilde$0.8 \pi$. Two sligthly higher flare peaks have been detected at phases $0.5 \pi$ and $2 \pi$ respectively, but otherwise there does not seem to be any pattern.\\ +All of the folded lightcurves of TYC 4595-107-1 can be found in appendix \ref{apB:TYC_4595-107-1}, figures \ref{apB:fig:TYC_4595-107-1-TESS_foldedLC1} and \ref{apB:fig:TYC_4595-107-1-TESS_foldedLC2}. \begin{figure}[pt!] \includegraphics[width=.95\textwidth]{plots/sine/TYC_4595-107-1/TYC 4595-107-1-Flarepeaks_maxY-1.2782052782832685.png} @@ -470,6 +471,7 @@ The flare peak at normalized phase distribution can be seen in figure \ref{fig:T \FloatBarrier \subsection{V* V471 Tau} +\label{results:v471_tau} V471 Tau is a post-common envelope binary system consiting of a K2 type dwarf and a white dwarf (\cite{v471tau_revised}). The K2 dwarf has a always present dominant spot, which faces the white dwarf (\cite{V471tau_magnetic_activity}). Figures \ref{fig:V471Tau-Flarecount-10_Bins} and \ref{fig:V471Tau-Flarecount-30_Bins} show the histograms of 5 TESS folded lightcurves for V471 Tau with 10 and 30 bins respectively. The TESS lightcurves used are of sectors 42, 43, 44, 70 and 71. The lightcurve of K2 target table ID 80 was rejected by the algorithm. Due to the lightcurve spanning 90 days, and the variability in spots, the folding and fitting algorithm could not produce a reliable output. @@ -533,6 +535,7 @@ Figure \ref{fig:V471Tau-flarepeaks_1.053} shows the normalized phase and peak of \FloatBarrier \subsection{V* HK Aqr} +\label{results:hk_aqr} HK Aqr is a M dwarf with a mass of 0.57 $M_\odot$, a radius of 0.53 $R_\odot$ and is around 22.3 pc away from our solar system. Its effective temperature is aroun 3800 K (\cite{conch_shell_m_dwarfs}). It was observed in four TESS sectors. HK Aqr is mentioned here, as it is a star, for which the optimize fold algorithm partially broke. This happened for its lightcurves for the sectors 29 and 42. The algorithm found for both periodograms a second signal for a possible period. This resulted in the folded lightcurves seen in figures \ref{fig:HKAqr-TESS29_foldedLC} and \ref{fig:HKAqr-TESS42_foldedLC}. Figures \ref{fig:HKAqr-Flarecount-10_Bins} and \ref{fig:HKAqr-Flarecount-30_Bins} were created with this dataset.\\ @@ -632,6 +635,7 @@ The flare count in figure \ref{fig:HKAqr-Flarecount-30_Bins_Period} is very low. \FloatBarrier \subsection{KOI-256} +\label{results:koi_256} KOI-256 is, similarly to V471 Tau, a binary system consisting of a M dwarf and a white dwarf (\cite{eclipsing_binaries_koi_256}, \cite{koi_256_effects_of_magnetic}). It has a mass of 0.51 M$_\odot$, a radius of 0.540 R$_\odot$ and an effective temperature of 3450 K (\cite{eclipsing_binaries_koi_256}). Similarly to HK Aqr, a second periodicity was detected, which was the used to fold for spot modulation. This happened for Kepler target table ids 37, 38, 53 and TESS sector 80.\\ Figure \ref{fig:KOI-256-Flarecount-10_Bins} shows the histogram with 10 bins for KOI-256 with all detected spot modulations, including the mentioned ones that were wrongfully detected. This figure shows a increase in flare count around phase $1 \pi$, which peaks at phases $0.7 \pi$ and around $1.4 \pi$. Additionally there appears a peak at phase $1.7 \pi$. @@ -656,7 +660,7 @@ Increasing the bins to 30 (figure \ref{fig:KOI-256-Flarecount-30_Bins}) shows cl \label{fig:KOI-256-Flarecount} \end{figure} -Figures \ref{fig:KOI-256-Flarecount-10_Bins_Period} and \ref{fig:KOI-256-Flarecount-30_Bins_Period} show the histograms based on the, by the optimized fold algorithm determined, period folded lightcurves. Therefor only the period folded lightcurves from Kepler target table id 37, 38, 53 and TESS sector 80 were used. +Figures \ref{fig:KOI-256-Flarecount-10_Bins_Period} and \ref{fig:KOI-256-Flarecount-30_Bins_Period} show the histograms based on the, by the optimized fold algorithm determined, period folded lightcurves. Therefor only the period folded lightcurves from Kepler target table id 37, 38, 53 and TESS sector 80 were used. The folded lightcurves can be found in appendix \ref{apB:koi-256}, figures \ref{apB:fig:KOI-256-Kepler_foldedLC} and \ref{apB:fig:KOI-256-TESS_foldedLC}. In figure \ref{fig:KOI-256-Flarecount-10_Bins_Period}, which shows a histogram with 10 bins for the flare distribution across the normalized phase, there is a clear increase of flares seen around the minima at phase $1 \pi$. The distribution nearly reminds one of a normal distribution, with the exception that the last two bins around phase $1.8 \pi$ to $2 \pi$ do not fall off as much as the first bin at phase $0 \pi$ does compared to the bins in the center.\\ Looking at figure \ref{fig:KOI-256-Flarecount-30_Bins_Period} which shows the same data, just with 30 bins, the peak at the phase minimum at $1 \pi$ is still present. Additionally there are three more peaks visible at around phases $0.3 \pi$, $1.4 \pi$ and $2 \pi$. These three peaks are only 1 bin wide and stand out far from their surrounding by around 1.5 times the errorbar. The peak in the center on the otherhand has gradual increases/descreases before and after, with the exception of the dip in the bin right before at around phase $0.9 \pi$. @@ -678,7 +682,7 @@ Looking at figure \ref{fig:KOI-256-Flarecount-30_Bins_Period} which shows the sa \label{fig:KOI-256-Flarecount_Period} \end{figure} -Comparing the results of the flare peak distributions across the normalized phases of the two datasets in figure \ref{fig:KOI-256-flarepeaks} shows that the highest normalized flare peaks of up to 1.7 were detected in the lightcurves with proper period detection. Comparing flare peaks which exist in both data sample, one can see that the highest peak of \subref{fig:KOI-256-flarepeaks_1.3_period} at around phase $0.8 \pi$ and a normalized peak of \textasciitilde1.3 was moved to around phase $0.4 \pi$ in figure \subref{fig:KOI-256-flarepeaks_1.7_spot} due to the additional found periodicity. +Comparing the results of the flare peak distributions across the normalized phases of the two datasets in figure \ref{fig:KOI-256-flarepeaks} shows that the highest normalized flare peaks of up to 1.7 were detected in the lightcurves with proper period detection (folded lightcurves in appendix \ref{apB:koi-256}, figures \ref{apB:fig:KOI-256-Kepler_periodfoldedLC} and \ref{apB:fig:KOI-256-TESS_periodfoldedLC}). Comparing flare peaks which exist in both data sample, one can see that the highest peak of \subref{fig:KOI-256-flarepeaks_1.3_period} at around phase $0.8 \pi$ and a normalized peak of \textasciitilde1.3 was moved to around phase $0.4 \pi$ in figure \subref{fig:KOI-256-flarepeaks_1.7_spot} due to the additional found periodicity. \begin{figure}[pt!] \centering @@ -694,6 +698,54 @@ Comparing the results of the flare peak distributions across the normalized phas \caption{Period folded} \label{fig:KOI-256-flarepeaks_1.3_period} \end{subfigure} - \caption{Distribution of flare peaks in relation to the normalized phase at which they occured. Y-Axis shows the flare peak and is limited to the value of the highest peak detected. The x-axis shows the normalized phase.} + \caption{Distribution of flare peaks for KOI-256 in relation to the normalized phase at which they occured. Y-Axis shows the flare peak and is limited to the value of the highest peak detected. The x-axis shows the normalized phase.} \label{fig:KOI-256-flarepeaks} +\end{figure} + +\FloatBarrier +\subsection{2MASS J19230963+3739397} +\label{results:2MASS_J19230963p3739397} + +2MASS J19230963+3739397, also known as KIC 2300039 or TIC 122672447, is a M dwarf around 213 pc away from our solar system (\cite{simbad}). It was observed in 3 Kepler target table IDs as well as 4 TESS sectors. The results for its flare distributions can be seen in figure \ref{fig:2MASS_J19230963p3739397-Flarecount}. It was selected as an example as it shows quite the opposite of what was expected. As seen in the histogram with 10 bins (figure \ref{fig:2MASS_J19230963p3739397-Flarecount-10_Bins}) it shows an increased flare occurance during the transition between phase minimum and maximum and during the maximum (phase $1.3 \pi$ to $2 \pi$). An additional significant peak is seen in the second bin. The flare count during the phase minimum at phase $1 \pi$ is at a minimum. Increasing the bin count to 30 (see figure \ref{fig:2MASS_J19230963p3739397-Flarecount-30_Bins}) creates a similarly shaped histogram. The errorbars increase in size relatively though, and makes the individual less accurate. The folded lightcurves for the Kepler target table IDs 47, 48 and 49 can be seen in figure \ref{fig:2MASS_J19230963p3739397-Kepler_foldedLCs}. There were no flares detected in the TESS lightcurves. As seen in the Kepler lightcurves, flare peaks as high as 1.5 have been detected, all around the phase maxima. + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/2MASS J19230963+3739397/2MASS J19230963+3739397-Flarecount-10_Bins.png} + \caption{10 bins} + \label{fig:2MASS_J19230963p3739397-Flarecount-10_Bins} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/2MASS J19230963+3739397/2MASS J19230963+3739397-Flarecount-30_Bins.png} + \caption{30 bins} + \label{fig:2MASS_J19230963p3739397-Flarecount-30_Bins} + \end{subfigure} + \caption{Histograms of 2MASS J19230963+3739397 across the phase showing the number of flares in each bin. The error bar shows the standard deviation for the histogram. The blue lines show the various fits for the folded lightcurves used to generate the data, with the phase minimum at $1 \pi$ and phase maximum at $0 \pi$/$2 \pi$.} + \label{fig:2MASS_J19230963p3739397-Flarecount} +\end{figure} + +\begin{figure}[pt!] + \centering + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/2MASS J19230963+3739397/2MASS J19230963+3739397_Kepler-47-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 47} + \label{fig:2MASS_J19230963p3739397-Kepler47_foldedLC} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/2MASS J19230963+3739397/2MASS J19230963+3739397_Kepler-48-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 48} + \label{fig:2MASS_J19230963p3739397-Kepler48_foldedLC} + \end{subfigure} + \begin{subfigure}[b]{.49\textwidth} + \centering + \includegraphics[width=\linewidth]{plots/sine/2MASS J19230963+3739397/2MASS J19230963+3739397_Kepler-49-foldedLC-marked_fit_flares.png} + \caption{Kepler target table ID 48} + \label{fig:2MASS_J19230963p3739397-Kepler48_foldedLC} + \end{subfigure} + \caption{Folded lightcurves for 2MASS J19230963+3739397. The blue lines shows the sine fits calculated. The red crosses indicate the detected flare peaks.} + \label{fig:2MASS_J19230963p3739397-Kepler_foldedLCs} \end{figure} \ No newline at end of file diff --git a/Physics_Thesis_Template/main.bbl-SAVE-ERROR b/Physics_Thesis_Template/main.bbl-SAVE-ERROR new file mode 100644 index 0000000..158abdf --- /dev/null +++ b/Physics_Thesis_Template/main.bbl-SAVE-ERROR @@ -0,0 +1,4850 @@ +% $ biblatex auxiliary file $ +% $ biblatex bbl format version 3.3 $ +% Do not modify the above lines! +% +% This is an auxiliary file used by the 'biblatex' package. +% This file may safely be deleted. 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G\bibinitperiod}}}% + {{hash=2722c01dac261bf1d524b958eab2af7d}{% + family={{Brammer}}, + familyi={B\bibinitperiod}, + given={G.\bibnamedelimi B.}, + giveni={G\bibinitperiod\bibinitdelim B\bibinitperiod}}}% + {{hash=95380ba92c465b793d9b3f8825aceaf7}{% + family={{Bray}}, + familyi={B\bibinitperiod}, + given={E.\bibnamedelimi M.}, + giveni={E\bibinitperiod\bibinitdelim M\bibinitperiod}}}% + {{hash=1ecf457786b281f30abea8eee755c65d}{% + family={{Breytenbach}}, + familyi={B\bibinitperiod}, + given={H.}, + giveni={H\bibinitperiod}}}% + {{hash=30ec18253b77891af5142e05b5a63d3f}{% + family={{Buddelmeijer}}, + familyi={B\bibinitperiod}, + given={H.}, + giveni={H\bibinitperiod}}}% + {{hash=6ed08ed8409909aceb18d6df7f4fe8d8}{% + family={{Burke}}, + familyi={B\bibinitperiod}, + given={D.\bibnamedelimi J.}, + giveni={D\bibinitperiod\bibinitdelim J\bibinitperiod}}}% + {{hash=32f8af8d58679a067cf285b3bb536c82}{% + family={{Calderone}}, + familyi={C\bibinitperiod}, + given={G.}, + giveni={G\bibinitperiod}}}% + {{hash=2f5d9c0b542c29660f2071fd662428df}{% + family={{Cano Rodr{'i}guez}}, + familyi={C\bibinitperiod}, + given={J.\bibnamedelimi L.}, + giveni={J\bibinitperiod\bibinitdelim L\bibinitperiod}}}% + {{hash=0263f59533ec5fbabc2713556bba7019}{% + family={{Cara}}, + familyi={C\bibinitperiod}, + given={M.}, + giveni={M\bibinitperiod}}}% + {{hash=e96df0efacb5de716fe6e8aa81319517}{% + family={{Cardoso}}, + familyi={C\bibinitperiod}, + given={J.\bibnamedelimi V.\bibnamedelimi M.}, + giveni={J\bibinitperiod\bibinitdelim V\bibinitperiod\bibinitdelim M\bibinitperiod}}}% + {{hash=b93bc17061cda9aabbec0503a4fdd6e2}{% + family={{Cheedella}}, + familyi={C\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=f5b592bdbfa5171f351701e0ea568f79}{% + family={{Copin}}, + familyi={C\bibinitperiod}, + given={Y.}, + giveni={Y\bibinitperiod}}}% + {{hash=df3eaf8d38f6aaf06e6eec84ba77dd79}{% + family={{Corrales}}, + familyi={C\bibinitperiod}, + given={L.}, + giveni={L\bibinitperiod}}}% + {{hash=c4b6b6607285ed228e8022d28f6a29e9}{% + family={{Crichton}}, + familyi={C\bibinitperiod}, + given={D.}, + giveni={D\bibinitperiod}}}% + {{hash=51b82276257c3def9a31939e231fbbba}{% + family={{D'Avella}}, + familyi={D\bibinitperiod}, + given={D.}, + giveni={D\bibinitperiod}}}% + {{hash=6e98c577c89bbf4fddef54b8e0447a4c}{% + family={{Deil}}, + familyi={D\bibinitperiod}, + given={C.}, + giveni={C\bibinitperiod}}}% + {{hash=2fa09843a54af02287bb67fed60c425d}{% + family={{Depagne}}, + familyi={D\bibinitperiod}, + given={{'E}.}, + giveni={'\bibinitperiod}}}% + {{hash=682fc66b6cd3f151522ca14f0c55992e}{% + family={{Dietrich}}, + familyi={D\bibinitperiod}, + given={J.\bibnamedelimi P.}, + giveni={J\bibinitperiod\bibinitdelim P\bibinitperiod}}}% + {{hash=4f11808f116ad992895dbe66194d67a2}{% + family={{Donath}}, + familyi={D\bibinitperiod}, + given={A.}, + giveni={A\bibinitperiod}}}% + {{hash=99425be38b693432e3c57f2ba278b8a6}{% + family={{Droettboom}}, + 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{{hash=b7a914441090183561ddbe5f7c57af3b}{% + family={{Garrison}}, + familyi={G\bibinitperiod}, + given={L.\bibnamedelimi H.}, + giveni={L\bibinitperiod\bibinitdelim H\bibinitperiod}}}% + {{hash=754e651035a4cd3a51ae18c2314b4dd7}{% + family={{Gibbons}}, + familyi={G\bibinitperiod}, + given={S.\bibnamedelimi L.\bibnamedelimi J.}, + giveni={S\bibinitperiod\bibinitdelim L\bibinitperiod\bibinitdelim J\bibinitperiod}}}% + {{hash=4ba3af2613678e8880846785d4d1bf53}{% + family={{Goldstein}}, + familyi={G\bibinitperiod}, + given={D.\bibnamedelimi A.}, + giveni={D\bibinitperiod\bibinitdelim A\bibinitperiod}}}% + {{hash=c7acd5cd06d4a55f10d56e5066dad94b}{% + family={{Gommers}}, + familyi={G\bibinitperiod}, + given={R.}, + giveni={R\bibinitperiod}}}% + {{hash=fa380b0492c15ee595b903e2802a2897}{% + family={{Greco}}, + familyi={G\bibinitperiod}, + given={J.\bibnamedelimi P.}, + giveni={J\bibinitperiod\bibinitdelim P\bibinitperiod}}}% + {{hash=6fc48cb49c62c12a80e7181d87e5709f}{% + family={{Greenfield}}, + familyi={G\bibinitperiod}, + given={P.}, + giveni={P\bibinitperiod}}}% + {{hash=fac3e63ff2cd60d984abcd019051cdd2}{% + family={{Groener}}, + familyi={G\bibinitperiod}, + given={A.\bibnamedelimi M.}, + giveni={A\bibinitperiod\bibinitdelim M\bibinitperiod}}}% + {{hash=1447c52921e046b8cf9add41bc29d75e}{% + family={{Grollier}}, + familyi={G\bibinitperiod}, + given={F.}, + giveni={F\bibinitperiod}}}% + {{hash=bf83d306b6208203373fd49439b519b8}{% + family={{Hagen}}, + familyi={H\bibinitperiod}, + given={A.}, + giveni={A\bibinitperiod}}}% + {{hash=e485db9d5319ff0e986a25bf4c896a71}{% + family={{Hirst}}, + familyi={H\bibinitperiod}, + given={P.}, + giveni={P\bibinitperiod}}}% + {{hash=4650a93e8d60ee76eee6cc3dc30d274c}{% + family={{Homeier}}, + familyi={H\bibinitperiod}, + given={D.}, + giveni={D\bibinitperiod}}}% + {{hash=58490e162b1e92bb6045a2ec67f8dde2}{% + family={{Horton}}, + familyi={H\bibinitperiod}, + given={A.\bibnamedelimi J.}, + giveni={A\bibinitperiod\bibinitdelim J\bibinitperiod}}}% + {{hash=c4715721668aa0cddc28e228c343a001}{% + family={{Hosseinzadeh}}, + familyi={H\bibinitperiod}, + given={G.}, + giveni={G\bibinitperiod}}}% + {{hash=52ae33def4997fdba78f83e4f5035919}{% + family={{Hu}}, + familyi={H\bibinitperiod}, + given={L.}, + giveni={L\bibinitperiod}}}% + {{hash=fdce7ec5a0c79c4e628fbc8230302d22}{% + family={{Hunkeler}}, + familyi={H\bibinitperiod}, + given={J.\bibnamedelimi S.}, + giveni={J\bibinitperiod\bibinitdelim S\bibinitperiod}}}% + {{hash=813793a6f11cdd4d34784185fbb83834}{% + family={{Ivezi{'c}}}, + familyi={I\bibinitperiod}, + given={{\bibnamedelimb {Z}}.}, + giveni={\bibinitperiod\bibinitdelim Z\bibinitperiod}}}% + {{hash=b8a48184e3794e3037528773cc004bb8}{% + family={{Jain}}, + familyi={J\bibinitperiod}, + given={A.}, + giveni={A\bibinitperiod}}}% + {{hash=fc16cf880e7cfaecac1c3e20ac8c37d9}{% + family={{Jenness}}, + familyi={J\bibinitperiod}, + given={T.}, + giveni={T\bibinitperiod}}}% + {{hash=2828aa94f5bfab6b35e82f288568c5d0}{% + family={{Kanarek}}, + familyi={K\bibinitperiod}, + given={G.}, + giveni={G\bibinitperiod}}}% + {{hash=d059cafd635e0d02391376110804caa5}{% + family={{Kendrew}}, + familyi={K\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=6281763a54fe5e9a884819459338b82f}{% + family={{Kern}}, + familyi={K\bibinitperiod}, + given={N.\bibnamedelimi S.}, + giveni={N\bibinitperiod\bibinitdelim S\bibinitperiod}}}% + {{hash=4aec9dee3cd5ef6a65288ece72f6ea25}{% + family={{Kerzendorf}}, + familyi={K\bibinitperiod}, + given={W.\bibnamedelimi E.}, + giveni={W\bibinitperiod\bibinitdelim E\bibinitperiod}}}% + {{hash=eb477e9c4597a03ff0722fd057d6b91a}{% + family={{Khvalko}}, + familyi={K\bibinitperiod}, + given={A.}, + giveni={A\bibinitperiod}}}% + {{hash=3dd4a04c7b122fd8f1a781cec9c03815}{% + family={{King}}, + familyi={K\bibinitperiod}, + given={J.}, + giveni={J\bibinitperiod}}}% + {{hash=056382f2662d499ac42051b005ab381b}{% + family={{Kirkby}}, + familyi={K\bibinitperiod}, + given={D.}, + giveni={D\bibinitperiod}}}% + {{hash=77a8f3eb81499e306f6801679cb180a8}{% + family={{Kulkarni}}, + familyi={K\bibinitperiod}, + given={A.\bibnamedelimi M.}, + giveni={A\bibinitperiod\bibinitdelim M\bibinitperiod}}}% + {{hash=40faa1bc69980517511d12eb5ab3c8bb}{% + family={{Kumar}}, + familyi={K\bibinitperiod}, + given={A.}, + giveni={A\bibinitperiod}}}% + {{hash=b8e85c5e661557b8a07fe719c2c30bf1}{% + family={{Lee}}, + familyi={L\bibinitperiod}, + given={A.}, + giveni={A\bibinitperiod}}}% + {{hash=d4c52fc874fb9d62c40dacd6348fdc4d}{% + family={{Lenz}}, + familyi={L\bibinitperiod}, + given={D.}, + giveni={D\bibinitperiod}}}% + {{hash=2890071f39e762e10b20580289167fb0}{% + family={{Littlefair}}, + familyi={L\bibinitperiod}, + given={S.\bibnamedelimi P.}, + giveni={S\bibinitperiod\bibinitdelim P\bibinitperiod}}}% + {{hash=fc56c3d085d8042379a2aaa9f0f3e53c}{% + family={{Ma}}, + familyi={M\bibinitperiod}, + given={Z.}, + giveni={Z\bibinitperiod}}}% + {{hash=f761eacc4ec086ab243f35674c0ccab5}{% + family={{Macleod}}, + familyi={M\bibinitperiod}, + given={D.\bibnamedelimi M.}, + giveni={D\bibinitperiod\bibinitdelim M\bibinitperiod}}}% + {{hash=ac9ea97af9d92d511e16f0742462f77e}{% + family={{Mastropietro}}, + familyi={M\bibinitperiod}, + given={M.}, + giveni={M\bibinitperiod}}}% + {{hash=a5e8c5bbc32aff5b136b7be18cea5a9a}{% + family={{McCully}}, + familyi={M\bibinitperiod}, + given={C.}, + giveni={C\bibinitperiod}}}% + {{hash=26d757f57bd901d1266dbd257f1cc8d7}{% + family={{Montagnac}}, + familyi={M\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=fa5b30cc88d5249b2d652ff5d9539151}{% + family={{Morris}}, + familyi={M\bibinitperiod}, + given={B.\bibnamedelimi M.}, + giveni={B\bibinitperiod\bibinitdelim M\bibinitperiod}}}% + {{hash=b7b76fe0a2f07a18d2e4cd1206c44962}{% + family={{Mueller}}, + familyi={M\bibinitperiod}, + given={M.}, + giveni={M\bibinitperiod}}}% + {{hash=ccbd4f9e77c548cf1c0b7220632bc54a}{% + family={{Mumford}}, + familyi={M\bibinitperiod}, + given={S.\bibnamedelimi J.}, + giveni={S\bibinitperiod\bibinitdelim J\bibinitperiod}}}% + {{hash=b2dd6a1e6ac8d3b6aa39f18c69d04dbb}{% + family={{Muna}}, + familyi={M\bibinitperiod}, + given={D.}, + giveni={D\bibinitperiod}}}% + {{hash=6fc1a14a2e5e541c9d7740108dfa1f1e}{% + family={{Murphy}}, + familyi={M\bibinitperiod}, + given={N.\bibnamedelimi A.}, + giveni={N\bibinitperiod\bibinitdelim A\bibinitperiod}}}% + {{hash=6567cf068239f4196799ddb3cdde11f0}{% + family={{Nelson}}, + familyi={N\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=74276f1b3969e188be62321f01eec949}{% + family={{Nguyen}}, + familyi={N\bibinitperiod}, + given={G.\bibnamedelimi H.}, + giveni={G\bibinitperiod\bibinitdelim H\bibinitperiod}}}% + {{hash=3700c16da8e8742baecd01c6ac7d0bcb}{% + family={{Ninan}}, + familyi={N\bibinitperiod}, + given={J.\bibnamedelimi P.}, + giveni={J\bibinitperiod\bibinitdelim P\bibinitperiod}}}% + {{hash=f2e7e8606ffeb85e82858d6c66e303b1}{% + family={{N{"o}the}}, + familyi={N\bibinitperiod}, + given={M.}, + giveni={M\bibinitperiod}}}% + {{hash=d2fe58f347341b2f049d29485aadddc0}{% + family={{Ogaz}}, + familyi={O\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=a252f407739a0e7cce8eba6b55ae7285}{% + family={{Oh}}, + familyi={O\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=efd20712557535453110b49939f2503d}{% + family={{Parejko}}, + familyi={P\bibinitperiod}, + given={J.\bibnamedelimi K.}, + giveni={J\bibinitperiod\bibinitdelim K\bibinitperiod}}}% + {{hash=5a2584f72e9d51eb681d62409b38f9bb}{% + family={{Parley}}, + familyi={P\bibinitperiod}, + given={N.}, + giveni={N\bibinitperiod}}}% + {{hash=dec47574ede3e08e3a8b77dd93a3dc9c}{% + family={{Pascual}}, + familyi={P\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=a4013b53be8edee428d3a5f0eeeb0556}{% + family={{Patil}}, + familyi={P\bibinitperiod}, + given={R.}, + giveni={R\bibinitperiod}}}% + {{hash=5a7cd2f1e64317cbd5132d41c0fc77ae}{% + family={{Patil}}, + familyi={P\bibinitperiod}, + given={A.\bibnamedelimi A.}, + giveni={A\bibinitperiod\bibinitdelim A\bibinitperiod}}}% + {{hash=b86d8c56664f16d39ef774bbd15739bd}{% + family={{Plunkett}}, + familyi={P\bibinitperiod}, + given={A.\bibnamedelimi L.}, + giveni={A\bibinitperiod\bibinitdelim L\bibinitperiod}}}% + {{hash=ad9eeaa2a4f039078eaf29f3802b92c8}{% + family={{Prochaska}}, + familyi={P\bibinitperiod}, + given={J.\bibnamedelimi X.}, + giveni={J\bibinitperiod\bibinitdelim X\bibinitperiod}}}% + {{hash=95d22dea0c4cd001547a22c61ae790f5}{% + family={{Rastogi}}, + familyi={R\bibinitperiod}, + given={T.}, + giveni={T\bibinitperiod}}}% + {{hash=c15747278783dd0280c5ebd0126932a5}{% + family={{Reddy Janga}}, + familyi={R\bibinitperiod}, + given={V.}, + giveni={V\bibinitperiod}}}% + {{hash=2c22d98e1a1f7e77fd61af59a93bf6ae}{% + family={{Sabater}}, + familyi={S\bibinitperiod}, + given={J.}, + giveni={J\bibinitperiod}}}% + {{hash=d6e4a4871b227ff4e6779103cf0a148f}{% + family={{Sakurikar}}, + familyi={S\bibinitperiod}, + given={P.}, + giveni={P\bibinitperiod}}}% + {{hash=6d3a6bbb661afd5100ac430696d5f14a}{% + family={{Seifert}}, + familyi={S\bibinitperiod}, + given={M.}, + giveni={M\bibinitperiod}}}% + {{hash=a2962bc8e1c2e465932ce4b6f23f230f}{% + family={{Sherbert}}, + familyi={S\bibinitperiod}, + given={L.\bibnamedelimi E.}, + giveni={L\bibinitperiod\bibinitdelim E\bibinitperiod}}}% + {{hash=39dc6cd11d70b4582ac7772e2c284ee8}{% + family={{Sherwood-Taylor}}, + familyi={S\bibinitperiod}, + given={H.}, + giveni={H\bibinitperiod}}}% + {{hash=9524ea939a58d06bdd77bca4af8605c8}{% + family={{Shih}}, + familyi={S\bibinitperiod}, + given={A.\bibnamedelimi Y.}, + giveni={A\bibinitperiod\bibinitdelim Y\bibinitperiod}}}% + {{hash=daaea0989734a3e391fc9946eebcbce9}{% + family={{Sick}}, + familyi={S\bibinitperiod}, + given={J.}, + giveni={J\bibinitperiod}}}% + {{hash=0c6bd49afa1df9cafa7c1ec4e334f4b8}{% + family={{Silbiger}}, + familyi={S\bibinitperiod}, + given={M.\bibnamedelimi T.}, + giveni={M\bibinitperiod\bibinitdelim T\bibinitperiod}}}% + {{hash=254cbaaf7da9424f3026b557efc27bca}{% + family={{Singanamalla}}, + familyi={S\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=b4f0e450949796df0c4dbb8140ce1307}{% + family={{Singer}}, + familyi={S\bibinitperiod}, + given={L.\bibnamedelimi P.}, + giveni={L\bibinitperiod\bibinitdelim P\bibinitperiod}}}% + {{hash=83d3d275432ac0d69c0f8208ca8c350e}{% + family={{Sladen}}, + familyi={S\bibinitperiod}, + given={P.\bibnamedelimi H.}, + giveni={P\bibinitperiod\bibinitdelim H\bibinitperiod}}}% + {{hash=6a42c2b0a8a32abfdff1de3b1deeb217}{% + family={{Sooley}}, + familyi={S\bibinitperiod}, + given={K.\bibnamedelimi A.}, + giveni={K\bibinitperiod\bibinitdelim A\bibinitperiod}}}% + {{hash=a3abc2aaec7e28a2640042fbfb1e60a7}{% + family={{Sornarajah}}, + familyi={S\bibinitperiod}, + given={S.}, + giveni={S\bibinitperiod}}}% + {{hash=0f9ce97ad68b621da6042ba9748fd496}{% + family={{Streicher}}, + familyi={S\bibinitperiod}, + given={O.}, + 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Detection of Periodicity in Flare Occurrence from Cool Stars with TESS}} + \field{volume}{920} + \field{year}{2021} + \field{pages}{42} + \range{pages}{1} + \verb{doi} + \verb 10.3847/1538-4357/ac142a + \endverb + \verb{eprint} + \verb 2107.06293 + \endverb + \keyw{Stellar rotation,Stellar flares,Stellar magnetic fields,Star-planet interactions,Starspots,Wide-field telescopes,1629,1603,1610,2177,1572,1800,Astrophysics - Solar and Stellar Astrophysics,Astrophysics - Earth and Planetary Astrophysics} + \endentry + \entry{4160265}{article}{}{} + \name{author}{1}{}{% + {{hash=a27d092a3c70c59360ac990a48514314}{% + family={{Hunter}}, + familyi={H\bibinitperiod}, + given={J.\bibnamedelimi D.}, + giveni={J\bibinitperiod\bibinitdelim D\bibinitperiod}}}% + } + \strng{namehash}{a27d092a3c70c59360ac990a48514314} + \strng{fullhash}{a27d092a3c70c59360ac990a48514314} + \strng{fullhashraw}{a27d092a3c70c59360ac990a48514314} + \strng{bibnamehash}{a27d092a3c70c59360ac990a48514314} + \strng{authorbibnamehash}{a27d092a3c70c59360ac990a48514314} + \strng{authornamehash}{a27d092a3c70c59360ac990a48514314} + \strng{authorfullhash}{a27d092a3c70c59360ac990a48514314} + \strng{authorfullhashraw}{a27d092a3c70c59360ac990a48514314} + \field{sortinit}{H} + \field{sortinithash}{23a3aa7c24e56cfa16945d55545109b5} + \field{extradatescope}{labelyear} + \field{labeldatesource}{} + \field{labelnamesource}{author} + \field{labeltitlesource}{title} + \field{journaltitle}{Computing in Science Engineering} + \field{number}{3} + \field{title}{Matplotlib: A 2D Graphics Environment} + \field{volume}{9} + \field{year}{2007} + \field{pages}{90\bibrangedash 95} + \range{pages}{6} + \endentry + \entry{au_mic_flaring_spi}{article}{}{} + \name{author}{2}{}{% + {{hash=0124d1a542f76e7c67abe0c22e0910e9}{% + family={{Ilin}}, + familyi={I\bibinitperiod}, + given={E.}, + giveni={E\bibinitperiod}}}% + {{hash=d55d1b16ab0f3c69890193f90c554a54}{% + family={{Poppenhaeger}}, + familyi={P\bibinitperiod}, + given={K.}, + giveni={K\bibinitperiod}}}% + } + \strng{namehash}{9b569f5cd77cffc82349e3407a4135a7} + \strng{fullhash}{9b569f5cd77cffc82349e3407a4135a7} + \strng{fullhashraw}{9b569f5cd77cffc82349e3407a4135a7} + \strng{bibnamehash}{9b569f5cd77cffc82349e3407a4135a7} + \strng{authorbibnamehash}{9b569f5cd77cffc82349e3407a4135a7} + \strng{authornamehash}{9b569f5cd77cffc82349e3407a4135a7} + \strng{authorfullhash}{9b569f5cd77cffc82349e3407a4135a7} + \strng{authorfullhashraw}{9b569f5cd77cffc82349e3407a4135a7} + \field{sortinit}{I} + \field{sortinithash}{8d291c51ee89b6cd86bf5379f0b151d8} + \field{extradatescope}{labelyear} + \field{labeldatesource}{} + \field{labelnamesource}{author} + \field{labeltitlesource}{title} + \field{eprintclass}{astro-ph.SR} + \field{eprinttype}{arXiv} + \field{journaltitle}{\mnras} + \field{month}{7} + \field{number}{3} + \field{title}{{Searching for flaring star-planet interactions in AU Mic TESS observations}} + \field{volume}{513} + \field{year}{2022} + \field{pages}{4579\bibrangedash 4586} + \range{pages}{8} + \verb{doi} + \verb 10.1093/mnras/stac1232 + \endverb + \verb{eprint} + \verb 2204.14090 + \endverb + \keyw{planets and satellites: individual: AU Mic b,planet-star interactions,stars: flare,stars: individual: AU Mic,Astrophysics - Solar and Stellar Astrophysics,Astrophysics - Earth and Planetary Astrophysics} + \endentry + \entry{SPI_2}{article}{}{} + \name{author}{3}{}{% + {{hash=f46c193e40e05ed94434d3aee6becbf9}{% + family={Ip}, + familyi={I\bibinitperiod}, + given={Wing-Huen}, + giveni={W\bibinithyphendelim H\bibinitperiod}}}% + {{hash=64013eba27823b7d3ee88e063dd07d84}{% + family={Kopp}, + familyi={K\bibinitperiod}, + given={Andreas}, + giveni={A\bibinitperiod}}}% + {{hash=3f26ae6096d507059e170539fc36cea1}{% + family={Hu}, + familyi={H\bibinitperiod}, + given={Juei-Hwa}, + giveni={J\bibinithyphendelim H\bibinitperiod}}}% + } + \strng{namehash}{84a7d1e421a642b3f2dedcb84722bbf1} + \strng{fullhash}{7785ee3f0a0d35ca9d8f0f2350b0b179} + \strng{fullhashraw}{7785ee3f0a0d35ca9d8f0f2350b0b179} + \strng{bibnamehash}{7785ee3f0a0d35ca9d8f0f2350b0b179} + \strng{authorbibnamehash}{7785ee3f0a0d35ca9d8f0f2350b0b179} + \strng{authornamehash}{84a7d1e421a642b3f2dedcb84722bbf1} + \strng{authorfullhash}{7785ee3f0a0d35ca9d8f0f2350b0b179} + \strng{authorfullhashraw}{7785ee3f0a0d35ca9d8f0f2350b0b179} + \field{sortinit}{I} + \field{sortinithash}{8d291c51ee89b6cd86bf5379f0b151d8} + \field{extradatescope}{labelyear} + \field{labeldatesource}{} + \field{labelnamesource}{author} + \field{labeltitlesource}{title} + \field{abstract}{Numerical simulations using a resistive MHD code are performed in order to investigate the interaction of the magnetospheres of hot Jupiters (or close-in extrasolar giant planets) with the central host stars. Because of the sub-Alfvénic nature of the stellar wind outflow at the orbital positions of these close-in exoplanets, no bow shock would form. When the orientation of the stellar coronal magnetic field is favorable to strong coupling with magnetic reconnection, the power (~1027 ergs s-1) generated could reach the level of a typical solar flare. As a particular type of star-planet atmospheric interaction, as investigated by Cuntz, Saar, & Musielak, magnetospheric interaction as studied in this Letter could lead to extensive energy injection into the auroral zones of the exoplanets, producing massive atmospheric escape process as recently detected.} + \field{journaltitle}{The Astrophysical Journal} + \field{month}{2} + \field{number}{1} + \field{title}{On the Star-Magnetosphere Interaction of Close-in Exoplanets} + \field{volume}{602} + \field{year}{2004} + \field{pages}{L53} + \range{pages}{1} + \verb{doi} + \verb 10.1086/382274 + \endverb + \verb{urlraw} + \verb https://dx.doi.org/10.1086/382274 + \endverb + \verb{url} + \verb https://dx.doi.org/10.1086/382274 + \endverb + \endentry + \entry{early_stellar_flares1}{article}{}{} + \name{author}{2}{}{% + {{hash=eda5250dda87777dbd41a87a66bed2e2}{% + family={{Joy}}, + familyi={J\bibinitperiod}, + given={A.\bibnamedelimi H.}, + giveni={A\bibinitperiod\bibinitdelim 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29} + \range{pages}{8} + \verb{doi} + \verb 10.1017/S1743921317003945 + \endverb + \keyw{stars:activity,stars:flare,stars:solar-type} + \endentry + \entry{flare_study_2}{inproceedings}{}{} + \name{author}{8}{}{% + {{hash=5d1d3d270a3612684876f6dbf5344ae7}{% + family={{Maehara}}, + familyi={M\bibinitperiod}, + given={Hiroyuki}, + giveni={H\bibinitperiod}}}% + {{hash=e21242c02073dce96845c446abd3ec2b}{% + family={{Notsu}}, + familyi={N\bibinitperiod}, + given={Yuta}, + giveni={Y\bibinitperiod}}}% + {{hash=68e70c86c91dec9289cd263d8f1087a8}{% + family={{Notsu}}, + familyi={N\bibinitperiod}, + given={Shota}, + giveni={S\bibinitperiod}}}% + {{hash=e3eac47de9f2494bb379cabbc171d5d1}{% + family={{Namekata}}, + familyi={N\bibinitperiod}, + given={Kousuke}, + giveni={K\bibinitperiod}}}% + {{hash=b78a0840cfab966ca3ea144ab8e5c1a2}{% + family={{Ikuta}}, + familyi={I\bibinitperiod}, + given={Kai}, + giveni={K\bibinitperiod}}}% + {{hash=4774e2f7f9f58fdbb25f8619f89af9d9}{% + family={{Honda}}, + 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