5618 lines
223 KiB
Plaintext
5618 lines
223 KiB
Plaintext
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\field{eid}{123}
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\field{journaltitle}{aj}
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\field{month}{9}
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\field{title}{{The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package}}
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\field{year}{2018}
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\verb{doi}
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\endentry
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giveni={A\bibinitperiod}}}%
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{{hash=6c3ef3d33781b8c11cb52f03adbc8a6e}{%
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family={{James}},
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familyi={J\bibinitperiod},
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given={D.},
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giveni={D\bibinitperiod}}}%
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{{hash=5b9f6028716a1613c79e1cee1687fbf7}{%
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family={{Ansdell}},
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given={M.},
|
|
giveni={M\bibinitperiod}}}%
|
|
{{hash=7216932ad414c8617e720861de1c35e6}{%
|
|
family={{Petrucci}},
|
|
familyi={P\bibinitperiod},
|
|
given={R.},
|
|
giveni={R\bibinitperiod}}}%
|
|
{{hash=938047aac5a02d1b5af56da6a7680974}{%
|
|
family={{Mauas}},
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familyi={M\bibinitperiod},
|
|
given={P.},
|
|
giveni={P\bibinitperiod}}}%
|
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{{hash=590d04db277a18b196ab1e9ffefb1f59}{%
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family={{Hilton}},
|
|
familyi={H\bibinitperiod},
|
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given={E.\bibnamedelimi J.},
|
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giveni={E\bibinitperiod\bibinitdelim J\bibinitperiod}}}%
|
|
}
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\strng{namehash}{8ab930e5f59213cf37af8d0a3a14a6f2}
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|
\strng{fullhash}{89f031a09a73e9e61cf5a3db7e595f5c}
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|
\strng{fullhashraw}{89f031a09a73e9e61cf5a3db7e595f5c}
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\strng{bibnamehash}{0aebaf0a651d69d9efe0cda1141ada99}
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\strng{authorbibnamehash}{0aebaf0a651d69d9efe0cda1141ada99}
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\strng{authornamehash}{8ab930e5f59213cf37af8d0a3a14a6f2}
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\strng{authorfullhash}{89f031a09a73e9e61cf5a3db7e595f5c}
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\strng{authorfullhashraw}{89f031a09a73e9e61cf5a3db7e595f5c}
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\field{sortinit}{G}
|
|
\field{sortinithash}{32d67eca0634bf53703493fb1090a2e8}
|
|
\field{extradatescope}{labelyear}
|
|
\field{labeldatesource}{}
|
|
\field{labelnamesource}{author}
|
|
\field{labeltitlesource}{title}
|
|
\field{eprintclass}{astro-ph.SR}
|
|
\field{eprinttype}{arXiv}
|
|
\field{journaltitle}{\mnras}
|
|
\field{month}{9}
|
|
\field{number}{3}
|
|
\field{title}{{Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life}}
|
|
\field{volume}{443}
|
|
\field{year}{2014}
|
|
\field{pages}{2561\bibrangedash 2578}
|
|
\range{pages}{18}
|
|
\verb{doi}
|
|
\verb 10.1093/mnras/stu1313
|
|
\endverb
|
|
\verb{eprint}
|
|
\verb 1406.7353
|
|
\endverb
|
|
\keyw{astrobiology,techniques: spectroscopic,planets and satellites: detection,stars: fundamental parameters,stars: late-type,stars: low-mass,Astrophysics - Solar and Stellar Astrophysics}
|
|
\endentry
|
|
\entry{kepler_mission_stellar_and_instrument_noise}{article}{}{}
|
|
\name{author}{17}{}{%
|
|
{{hash=6bd6b75ba5e030b70eeae1169a494183}{%
|
|
family={Gilliland},
|
|
familyi={G\bibinitperiod},
|
|
given={Ronald\bibnamedelima L.},
|
|
giveni={R\bibinitperiod\bibinitdelim L\bibinitperiod}}}%
|
|
{{hash=32ad9690d3379d7726f93a560eed416f}{%
|
|
family={Chaplin},
|
|
familyi={C\bibinitperiod},
|
|
given={William\bibnamedelima J.},
|
|
giveni={W\bibinitperiod\bibinitdelim J\bibinitperiod}}}%
|
|
{{hash=1374862852dc88e3610cc1e0fececb20}{%
|
|
family={Dunham},
|
|
familyi={D\bibinitperiod},
|
|
given={Edward\bibnamedelima W.},
|
|
giveni={E\bibinitperiod\bibinitdelim W\bibinitperiod}}}%
|
|
{{hash=795adf4207f188b75272a1e58e1bbd83}{%
|
|
family={Argabright},
|
|
familyi={A\bibinitperiod},
|
|
given={Vic\bibnamedelima S.},
|
|
giveni={V\bibinitperiod\bibinitdelim S\bibinitperiod}}}%
|
|
{{hash=8c0eff532b591fcda33946ba1b6c4984}{%
|
|
family={Borucki},
|
|
familyi={B\bibinitperiod},
|
|
given={William\bibnamedelima J.},
|
|
giveni={W\bibinitperiod\bibinitdelim J\bibinitperiod}}}%
|
|
{{hash=9f2ac918346114450f1833a0e16da45c}{%
|
|
family={Basri},
|
|
familyi={B\bibinitperiod},
|
|
given={Gibor},
|
|
giveni={G\bibinitperiod}}}%
|
|
{{hash=4ed01ec6cd7e83b9eea5be248558a6ab}{%
|
|
family={Bryson},
|
|
familyi={B\bibinitperiod},
|
|
given={Stephen\bibnamedelima T.},
|
|
giveni={S\bibinitperiod\bibinitdelim T\bibinitperiod}}}%
|
|
{{hash=2ec97bc65453e6791e5d485c91e0d649}{%
|
|
family={Buzasi},
|
|
familyi={B\bibinitperiod},
|
|
given={Derek\bibnamedelima L.},
|
|
giveni={D\bibinitperiod\bibinitdelim L\bibinitperiod}}}%
|
|
{{hash=141303e7aef9a18504e1db58c89643e4}{%
|
|
family={Caldwell},
|
|
familyi={C\bibinitperiod},
|
|
given={Douglas\bibnamedelima A.},
|
|
giveni={D\bibinitperiod\bibinitdelim A\bibinitperiod}}}%
|
|
{{hash=fac7dc989574725686436c9ba14ab120}{%
|
|
family={Elsworth},
|
|
familyi={E\bibinitperiod},
|
|
given={Yvonne\bibnamedelima P.},
|
|
giveni={Y\bibinitperiod\bibinitdelim P\bibinitperiod}}}%
|
|
{{hash=6ec5ab96601498ff4ac4d2404d1bf0c3}{%
|
|
family={Jenkins},
|
|
familyi={J\bibinitperiod},
|
|
given={Jon\bibnamedelima M.},
|
|
giveni={J\bibinitperiod\bibinitdelim M\bibinitperiod}}}%
|
|
{{hash=c2c0f8688cd9e92d125b3366d194a5a0}{%
|
|
family={Koch},
|
|
familyi={K\bibinitperiod},
|
|
given={David\bibnamedelima G.},
|
|
giveni={D\bibinitperiod\bibinitdelim G\bibinitperiod}}}%
|
|
{{hash=1817db02e4f1e8bf21d78c34861251cd}{%
|
|
family={Kolodziejczak},
|
|
familyi={K\bibinitperiod},
|
|
given={Jeffrey},
|
|
giveni={J\bibinitperiod}}}%
|
|
{{hash=35b151fb026f71c99d0c267814a8dbb5}{%
|
|
family={Miglio},
|
|
familyi={M\bibinitperiod},
|
|
given={Andrea},
|
|
giveni={A\bibinitperiod}}}%
|
|
{{hash=b3f9de358f894c608081e78cc05c8d73}{%
|
|
family={Cleve},
|
|
familyi={C\bibinitperiod},
|
|
given={Jeffrey},
|
|
giveni={J\bibinitperiod},
|
|
prefix={van},
|
|
prefixi={v\bibinitperiod}}}%
|
|
{{hash=da82af9f91a0f156725a8953a1d8394b}{%
|
|
family={Walkowicz},
|
|
familyi={W\bibinitperiod},
|
|
given={Lucianne\bibnamedelima M.},
|
|
giveni={L\bibinitperiod\bibinitdelim M\bibinitperiod}}}%
|
|
{{hash=51d8a4c8c7e9560952a32628ff733f10}{%
|
|
family={Welsh},
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|
familyi={W\bibinitperiod},
|
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given={William\bibnamedelima F.},
|
|
giveni={W\bibinitperiod\bibinitdelim F\bibinitperiod}}}%
|
|
}
|
|
\list{publisher}{1}{%
|
|
{The American Astronomical Society}%
|
|
}
|
|
\strng{namehash}{e1efa8486b8f5d4b350e64896cdf23c7}
|
|
\strng{fullhash}{f310a431c344c1ccec1388870a3a5dbb}
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\strng{bibnamehash}{4f74c384571193e171a6c83a6218d821}
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\strng{authorbibnamehash}{4f74c384571193e171a6c83a6218d821}
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\field{labeldatesource}{}
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\field{labelnamesource}{author}
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\field{labeltitlesource}{title}
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|
\field{abstract}{Kepler mission results are rapidly contributing to fundamentally new discoveries in both the exoplanet and asteroseismology fields. The data returned from Kepler are unique in terms of the number of stars observed, precision of photometry for time series observations, and the temporal extent of high duty cycle observations. As the first mission to provide extensive time series measurements on thousands of stars over months to years at a level hitherto possible only for the Sun, the results from Kepler will vastly increase our knowledge of stellar variability for quiet solar-type stars. Here, we report on the stellar noise inferred on the timescale of a few hours of most interest for detection of exoplanets via transits. By design the data from moderately bright Kepler stars are expected to have roughly comparable levels of noise intrinsic to the stars and arising from a combination of fundamental limitations such as Poisson statistics and any instrument noise. The noise levels attained by Kepler on-orbit exceed by some 50% the target levels for solar-type, quiet stars. We provide a decomposition of observed noise for an ensemble of 12th magnitude stars arising from fundamental terms (Poisson and readout noise), added noise due to the instrument and that intrinsic to the stars. The largest factor in the modestly higher than anticipated noise follows from intrinsic stellar noise. We show that using stellar parameters from galactic stellar synthesis models, and projections to stellar rotation, activity, and hence noise levels reproduce the primary intrinsic stellar noise features.}
|
|
\field{journaltitle}{The Astrophysical Journal Supplement Series}
|
|
\field{month}{10}
|
|
\field{number}{1}
|
|
\field{title}{KEPLER MISSION STELLAR AND INSTRUMENT NOISE PROPERTIES}
|
|
\field{volume}{197}
|
|
\field{year}{2011}
|
|
\field{pages}{6}
|
|
\range{pages}{1}
|
|
\verb{doi}
|
|
\verb 10.1088/0067-0049/197/1/6
|
|
\endverb
|
|
\verb{urlraw}
|
|
\verb https://dx.doi.org/10.1088/0067-0049/197/1/6
|
|
\endverb
|
|
\verb{url}
|
|
\verb https://dx.doi.org/10.1088/0067-0049/197/1/6
|
|
\endverb
|
|
\endentry
|
|
\entry{astroquery}{article}{}{}
|
|
\name{author}{25}{}{%
|
|
{{hash=9f597dfaaa61fb28e8dbda878a4dab55}{%
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family={{Ginsburg}},
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familyi={G\bibinitperiod},
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given={A.},
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giveni={A\bibinitperiod}}}%
|
|
{{hash=ca0f675b9a1f55f16252de00b9185e8e}{%
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family={{Sipőcz}},
|
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familyi={S\bibinitperiod},
|
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given={B.\bibnamedelimi M.},
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giveni={B\bibinitperiod\bibinitdelim M\bibinitperiod}}}%
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{{hash=4fa63d2b7281b54f9120f17767541f17}{%
|
|
family={{Brasseur}},
|
|
familyi={B\bibinitperiod},
|
|
given={C.\bibnamedelimi E.},
|
|
giveni={C\bibinitperiod\bibinitdelim E\bibinitperiod}}}%
|
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{{hash=31c31d2c69fdcdbbf70408123a1fd103}{%
|
|
family={{Cowperthwaite}},
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|
familyi={C\bibinitperiod},
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|
given={P.\bibnamedelimi S.},
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|
giveni={P\bibinitperiod\bibinitdelim S\bibinitperiod}}}%
|
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{{hash=fdeb6068961e12b16d29f3a3c36a62d8}{%
|
|
family={{Craig}},
|
|
familyi={C\bibinitperiod},
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given={M.\bibnamedelimi W.},
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|
giveni={M\bibinitperiod\bibinitdelim W\bibinitperiod}}}%
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{{hash=6e98c577c89bbf4fddef54b8e0447a4c}{%
|
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family={{Deil}},
|
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familyi={D\bibinitperiod},
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given={C.},
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giveni={C\bibinitperiod}}}%
|
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{{hash=877c1d27cd5dc63c353a7781624e7839}{%
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family={{Guillochon}},
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familyi={G\bibinitperiod},
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given={J.},
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giveni={J\bibinitperiod}}}%
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{{hash=0b73f631683d8637045b48a6f6585eb7}{%
|
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family={{Guzman}},
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familyi={G\bibinitperiod},
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given={G.},
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giveni={G\bibinitperiod}}}%
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{{hash=500244b20089ceb8dd2fe134027a3903}{%
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family={{Liedtke}},
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familyi={L\bibinitperiod},
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given={S.},
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giveni={S\bibinitperiod}}}%
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{{hash=6fde5ebc532efb4d328799efd9947432}{%
|
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family={{Lian Lim}},
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familyi={L\bibinitperiod},
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given={P.},
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giveni={P\bibinitperiod}}}%
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{{hash=261f109a80f8249bc3952d41598a6fde}{%
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family={{Lockhart}},
|
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familyi={L\bibinitperiod},
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given={K.\bibnamedelimi E.},
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giveni={K\bibinitperiod\bibinitdelim E\bibinitperiod}}}%
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{{hash=657d151b840c8989c5a03336fcdd6813}{%
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family={{Mommert}},
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familyi={M\bibinitperiod},
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given={M.},
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giveni={M\bibinitperiod}}}%
|
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{{hash=fa5b30cc88d5249b2d652ff5d9539151}{%
|
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family={{Morris}},
|
|
familyi={M\bibinitperiod},
|
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given={B.\bibnamedelimi M.},
|
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giveni={B\bibinitperiod\bibinitdelim M\bibinitperiod}}}%
|
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{{hash=3f12b01d5318704fe168261edba8f0d2}{%
|
|
family={{Norman}},
|
|
familyi={N\bibinitperiod},
|
|
given={H.},
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giveni={H\bibinitperiod}}}%
|
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{{hash=6b5657cfda5e034b453f3ac5daba3f5e}{%
|
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family={{Parikh}},
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familyi={P\bibinitperiod},
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given={M.},
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giveni={M\bibinitperiod}}}%
|
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{{hash=6377431fd466702aea8af7ac6a67a5ed}{%
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family={{Persson}},
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familyi={P\bibinitperiod},
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given={M.\bibnamedelimi V.},
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giveni={M\bibinitperiod\bibinitdelim V\bibinitperiod}}}%
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{{hash=8a68ee797f520823fce706841ca26433}{%
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family={{Robitaille}},
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{{hash=1b357470d35a2cc4fe0c135799fb9021}{%
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family={{Segovia}},
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given={J.-C.},
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{{hash=b4f0e450949796df0c4dbb8140ce1307}{%
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family={{Singer}},
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familyi={S\bibinitperiod},
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given={L.\bibnamedelimi P.},
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giveni={L\bibinitperiod\bibinitdelim P\bibinitperiod}}}%
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{{hash=83542361e3db5d6dcef0a9ef99bbce2d}{%
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family={{Tollerud}},
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familyi={T\bibinitperiod},
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given={E.\bibnamedelimi J.},
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giveni={E\bibinitperiod\bibinitdelim J\bibinitperiod}}}%
|
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{{hash=db0fe38377cdfb1ef0af4ea1e48c4852}{%
|
|
family={{de Val-Borro}},
|
|
familyi={d\bibinitperiod},
|
|
given={M.},
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giveni={M\bibinitperiod}}}%
|
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{{hash=1c3d80a15c45a817c786d8e1d02956e2}{%
|
|
family={{Valtchanov}},
|
|
familyi={V\bibinitperiod},
|
|
given={I.},
|
|
giveni={I\bibinitperiod}}}%
|
|
{{hash=aecc545cdf9649d19b302fc37de841f8}{%
|
|
family={{Woillez}},
|
|
familyi={W\bibinitperiod},
|
|
given={J.},
|
|
giveni={J\bibinitperiod}}}%
|
|
{{hash=46214351dfbc66888988cb9a89050ab6}{%
|
|
family={{The Astroquery collaboration}},
|
|
familyi={T\bibinitperiod}}}%
|
|
{{hash=fea4603787c4816a0374294c96e61d98}{%
|
|
family={{a subset of the astropy collaboration}},
|
|
familyi={a\bibinitperiod}}}%
|
|
}
|
|
\strng{namehash}{0a0fd0d0b2ce36063362f5b8ea02cd1c}
|
|
\strng{fullhash}{a2a9b203bba9023dabe6286e96d9a827}
|
|
\strng{fullhashraw}{a2a9b203bba9023dabe6286e96d9a827}
|
|
\strng{bibnamehash}{37fdf9f73e3c6e6c28748a6601898c9e}
|
|
\strng{authorbibnamehash}{37fdf9f73e3c6e6c28748a6601898c9e}
|
|
\strng{authornamehash}{0a0fd0d0b2ce36063362f5b8ea02cd1c}
|
|
\strng{authorfullhash}{a2a9b203bba9023dabe6286e96d9a827}
|
|
\strng{authorfullhashraw}{a2a9b203bba9023dabe6286e96d9a827}
|
|
\field{sortinit}{G}
|
|
\field{sortinithash}{32d67eca0634bf53703493fb1090a2e8}
|
|
\field{extradatescope}{labelyear}
|
|
\field{labeldatesource}{}
|
|
\field{labelnamesource}{author}
|
|
\field{labeltitlesource}{title}
|
|
\field{eid}{98}
|
|
\field{eprintclass}{astro-ph.IM}
|
|
\field{eprinttype}{arXiv}
|
|
\field{journaltitle}{\aj}
|
|
\field{month}{3}
|
|
\field{title}{{astroquery: An Astronomical Web-querying Package in Python}}
|
|
\field{volume}{157}
|
|
\field{year}{2019}
|
|
\field{pages}{98}
|
|
\range{pages}{1}
|
|
\verb{doi}
|
|
\verb 10.3847/1538-3881/aafc33
|
|
\endverb
|
|
\verb{eprint}
|
|
\verb 1901.04520
|
|
\endverb
|
|
\keyw{astronomical databases: miscellaneous,virtual observatory tools}
|
|
\endentry
|
|
\entry{solar_flare_mag_field}{article}{}{}
|
|
\name{author}{12}{}{%
|
|
{{hash=08cb4195c9863b085814cf7b058020de}{%
|
|
family={{Gopika}},
|
|
familyi={G\bibinitperiod},
|
|
given={V.\bibnamedelimi S.},
|
|
giveni={V\bibinitperiod\bibinitdelim S\bibinitperiod}}}%
|
|
{{hash=e393bf2c2404a188fbc373f984a1afc6}{%
|
|
family={{Blessy}},
|
|
familyi={B\bibinitperiod},
|
|
given={V.},
|
|
giveni={V\bibinitperiod}}}%
|
|
{{hash=c34aa69e3e9c428c5e284ebe577e5e8b}{%
|
|
family={{Asha}},
|
|
familyi={A\bibinitperiod},
|
|
given={V.\bibnamedelimi A.},
|
|
giveni={V\bibinitperiod\bibinitdelim A\bibinitperiod}}}%
|
|
{{hash=bcf488d66405b0acc2a93f319dfa2dc1}{%
|
|
family={{Ankitha}},
|
|
familyi={A\bibinitperiod},
|
|
given={N.},
|
|
giveni={N\bibinitperiod}}}%
|
|
{{hash=bae8b34ad7c7127a3035d261326e7714}{%
|
|
family={{Syamily}},
|
|
familyi={S\bibinitperiod},
|
|
given={P.},
|
|
giveni={P\bibinitperiod}}}%
|
|
{{hash=343bed6472341403206c41a9cdd3a6ce}{%
|
|
family={{Amrutha}},
|
|
familyi={A\bibinitperiod},
|
|
given={S.},
|
|
giveni={S\bibinitperiod}}}%
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{{hash=d4dafd15fd2507f9fb17d552ec5ac715}{%
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{{hash=a11a3260045b38f7bb40637951d52fe0}{%
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family={{Law}},
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\field{journaltitle}{\apj}
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\field{month}{10}
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\field{number}{1}
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|
\field{title}{{EvryFlare. IV. Detection of Periodicity in Flare Occurrence from Cool Stars with TESS}}
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\field{volume}{920}
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\field{year}{2021}
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\verb 2107.06293
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\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}
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\field{title}{{Searching for flaring star-planet interactions in AU Mic TESS observations}}
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\field{volume}{513}
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\field{year}{2022}
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\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}
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\endentry
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\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.}
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\field{title}{{A confined dynamo: Magnetic activity of the K-dwarf component in the pre-cataclysmic binary system V471 Tauri}}
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\keyw{stars: activity,binaries: eclipsing,starspots,stars: flare,stars: late-type,stars: individual: V471 Tau,Astrophysics - Solar and Stellar Astrophysics}
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\field{title}{A THIRD FLARE OF L 726-8B}
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|
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\endverb
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\verb{urlraw}
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\verb https://dx.doi.org/10.1086/126169
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\verb https://dx.doi.org/10.1086/126169
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\field{booktitle}{Living Around Active Stars}
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\field{month}{10}
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|
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{{hash=20abe3812625b1f32105a33f66474a37}{%
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|
|
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{{hash=68e70c86c91dec9289cd263d8f1087a8}{%
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{{hash=e21242c02073dce96845c446abd3ec2b}{%
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{{hash=ce5c945a58e32e3fe998c8dd0774a246}{%
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{{hash=4774e2f7f9f58fdbb25f8619f89af9d9}{%
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family={{Honda}},
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{{hash=20abe3812625b1f32105a33f66474a37}{%
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{{hash=f1b717a188c0398fdf0b2eb36a34f93b}{%
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|
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|
|
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|
|
\field{year}{2012}
|
|
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\verb{doi}
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|
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|
\endverb
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|
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|
\entry{flare_study_1}{article}{}{}
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|
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{{hash=5d1d3d270a3612684876f6dbf5344ae7}{%
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family={{Maehara}},
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familyi={M\bibinitperiod},
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given={Hiroyuki},
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giveni={H\bibinitperiod}}}%
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{{hash=03d4831cc720f5ed189bdfebe9f78a99}{%
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family={{Shibayama}},
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familyi={S\bibinitperiod},
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{{hash=e21242c02073dce96845c446abd3ec2b}{%
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{{hash=68e70c86c91dec9289cd263d8f1087a8}{%
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family={{Notsu}},
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{{hash=4774e2f7f9f58fdbb25f8619f89af9d9}{%
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{{hash=20abe3812625b1f32105a33f66474a37}{%
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family={{Nogami}},
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giveni={D\bibinitperiod}}}%
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{{hash=f1b717a188c0398fdf0b2eb36a34f93b}{%
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family={{Shibata}},
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familyi={S\bibinitperiod},
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given={Kazunari},
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\field{labelnamesource}{author}
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|
\field{labeltitlesource}{title}
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\field{eid}{59}
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|
\field{eprintclass}{astro-ph.SR}
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|
\field{eprinttype}{arXiv}
|
|
\field{journaltitle}{Earth, Planets and Space}
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|
\field{month}{12}
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|
\field{title}{{Statistical properties of superflares on solar-type stars based on 1-min cadence data}}
|
|
\field{volume}{67}
|
|
\field{year}{2015}
|
|
\field{pages}{59}
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|
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\verb{eprint}
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\verb 1504.00074
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|
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{{hash=761c92228af626556dc841a203fcd005}{%
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{{hash=eca9aeefdc8563b0e153fbedf08bc1a1}{%
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\field{title}{{Characterizing the Cool KOIs. V. KOI-256: A Mutually Eclipsing Post-common Envelope Binary}}
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|
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\keyw{binaries: eclipsing,binaries: spectroscopic,stars: abundances,stars: activity,stars: fundamental parameters,stars: individual: KOI-256,stars: late-type,stars: low-mass,stars: rotation,Astrophysics - Solar and Stellar Astrophysics}
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family={{NASA Exoplanet Archive}},
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{NExScI-Caltech/IPAC}%
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\keyw{stars: activity,stars: flare,stars: variables: general,starspots,Astrophysics - Solar and Stellar Astrophysics}
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