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some more refinements

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SGCMarkus
2025-06-01 18:20:02 +02:00
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Physics_Thesis_Template/content/appendixB.tex
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\chapter{Additional folded lightcurves \label{chap:apB}}
\section{KOI-256 \label{apB:KOI-256}}
\FloatBarrier
\section{TYC 4595-107-1 \label{apB:TYC_4595-107-1}}
\begin{figure}[pt!]
\begin{figure}[H]
\centering
\begin{subfigure}[b]{.49\textwidth}
\centering
@@ -47,6 +45,12 @@
\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}
\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-47-foldedLC-marked_fit_flares.png}
@@ -57,11 +61,6 @@
\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}
@@ -109,7 +108,7 @@
\FloatBarrier
\section{V471 Tau \label{apB:V471_tau}}
\begin{figure}[pt!]
\begin{figure}[H]
\centering
\begin{subfigure}[b]{.49\textwidth}
\centering
@@ -129,14 +128,14 @@
\caption{TESS Sector 44}
\label{apB:fig:V471Tau-TESS44}
\end{subfigure}
\caption{Folded lightcurves for V* V471 Tau.}
\caption{Folded lightcurves for V* V471 Tau by rotational period.}
\label{apB:fig:V471Tau-TESS_foldedLC}
\end{figure}
\FloatBarrier
\section{KOI-256 \label{apB:koi-256}}
\begin{figure}[pt!]
\begin{figure}[H]
\centering
\begin{subfigure}[b]{.49\textwidth}
\centering
Physics_Thesis_Template/content/appendixC.tex
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@@ -3,32 +3,38 @@
Appendix for miscellaneous lightcurves that can not be attributed to any of the topics, but are still noteworthy.
\begin{figure}[pt!]
\FloatBarrier
\section{2MASS J19033576+3941263 \label{apB:KOI-6423}}
2MASS J19033576+3941263 also known as KOI-6423.
\begin{figure}[H]
\centering
\begin{subfigure}[b]{.98\textwidth}
\begin{subfigure}[b]{.90\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}
\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]{.90\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}
\begin{subfigure}[b]{.90\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}
\begin{subfigure}[b]{.90\textwidth}
\centering
\includegraphics[width=\linewidth]{plots/KOI-6423/2MASS J19033576+3941263_TESS-54-lc.png}
\caption{TESS Sector 54}
@@ -38,20 +44,23 @@ Appendix for miscellaneous lightcurves that can not be attributed to any of the
\label{apC:fig:KOI-6423-TESS_lightcurves2}
\end{figure}
\begin{figure}[pt!]
\FloatBarrier
\section{V* V452 Lyr \label{apB:V452Lyr}}
\begin{figure}[H]
\centering
\begin{subfigure}[b]{.98\textwidth}
\begin{subfigure}[b]{.90\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}
\begin{subfigure}[b]{.90\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.}
\caption{Lightcurves for V* V452 Lyr.}
\label{apC:fig:V452Lyr-Kepler_lightcurves}
\end{figure}
Physics_Thesis_Template/content/chapter-conclusion.tex
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@@ -1,3 +1,7 @@
\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
In conclusion the only cumulative results which shows a significant spot dependence are those for the G type stars. It shows a significant increase in flares during the phase minimum over the overall flare distribution. The distribution has a similar form to a bell curve. The same goes for the two selected G type stars BD-08 995 and TYC 4595-107-1 which were presented and discussed. The histograms for K dwarfs on the other hand do not have the form of a bell curve. There appears a singular peak in the histogram with 10 bins at the phase minimum, with a few additional narrower peaks in the histogram with 30 bins. This could indicate a dependence of some sort, but a more detailed view at the individual stars is needed. As this category includes V* V471 Tau (close binary system with a white dwarf), similar interactions could happen on other stars. While there is no significant result for a spot dependence of the detected flares on M dwarfs, some individual stars show behaviour which would indicate this. HK Aqr and KOI-256 as examples, but 2MASS J19230963+3739397 also shows an interesting behaviour and should be studied in more detail as it shows most flares at the lightcurve maxima.\\
Overall improvements to the folding algorithms are required to handle edge cases better (e.g. KOI-256) , while not breaking for others. This could either be done automatically, or by setting special parameters for individual stars. Even though the latter would require manual user interaction and checking the edge cases manually. Additionally a common folding epoch for multiple fits files of the same star could be implemented. A good example would be V471 Tau, which showed a consistent spot modulation in some of its TESS lightcurves which differed from its rotational period. Implementing something like this could guarantee that the (in this case) transit of the white dwarf would always be at the same position in the phase, and not "jump" between the center and the edges. Furthermore the energy for the flares could be calculated. For this an improvments for the flare duration algorithm is required though, as it currently is just an estimation and does not account for the longest flare durations. It neither makes a distinction between TESS lightcurves with a 2 minute cadence and the Kepler/K2 short cadence data which has a cadence of 1 minute.\\
Furthermore more stars could be taken into consideration. While the Kepler/K2 missions are complete, the TESS mission is being extended and still observing as of writing. One could also take into account Kepler long cadence data (30 minute cadence), which would not be able to detect shorter duration flares, but is available for a larger amount of stars.
Physics_Thesis_Template/content/chapter-discussion.tex
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@@ -16,7 +16,7 @@ Limiting the flare by maximum flare peak height indicates a dependency of flares
%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.\\
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. With the exception of the bin (bins for the histogram with 30 bins) around the phase minimum. This bin shows a significantly increased flare count. One of the, but not the sole cause 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.
@@ -36,7 +36,7 @@ Out of a total of \textasciitilde13 F dwarfs in the list of stars to be analyzed
% 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.
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 results will be published on github. The program will be available at \href{URL}{text} while the data will be available at \href{URL}{text}.
% All data combined, peak at phase minimum dominated by G/K dwarfs, dip in transition maxima -> minima dominated by dip from M dwarf results.
Physics_Thesis_Template/content/chapter-results.tex
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@@ -116,7 +116,7 @@ The difference becomes less obvious when increasing the bin size 30 (figure \ref
\section{K dwarfs \label{sec:results:k_dwarfs}}
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}.\\
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. One of the major contributions is 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.
\begin{figure}[pt!]
@@ -498,7 +498,7 @@ Increasing the bins to 30 (figure \ref{fig:V471Tau-Flarecount-30_Bins}) does not
\label{fig:V471Tau-Flarecount}
\end{figure}
Looking at the folded lightcurves for this star (see figures \ref{fig:V471Tau-TESS42_foldedLC}, \ref{fig:V471Tau-TESS43_foldedLC} and \ref{fig:V471Tau-TESS44_foldedLC}), the transit of the white dwarf (sudden dip in the folded lightcurve) is clearly visible, and always happens around phase 0.
Looking at the folded lightcurves for this star (see figures \ref{fig:V471Tau-TESS42_foldedLC}, \ref{fig:V471Tau-TESS43_foldedLC} and \ref{fig:V471Tau-TESS44_foldedLC}), the transit of the white dwarf (sudden dip in the folded lightcurve) is clearly visible, and always happens around phase 0. Additional folded lightcurves can be seen in appendix \ref{apB:V471_tau}, figure \ref{apB:fig:V471Tau-TESS_foldedLC} like the ones which were folded by the rotational period for when a spot modulation was detected.
\begin{figure}[pt!]
\centering