Starspots Modelling and Flare Analysis on Selected MV Stars. (arXiv:2206.11611v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bicz_K/0/1/0/all/0/1">Kamil Bicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falewicz_R/0/1/0/all/0/1">Robert Falewicz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pietras_M/0/1/0/all/0/1">Małgorzata Pietras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siarkowski_M/0/1/0/all/0/1">Marek Siarkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pres_P/0/1/0/all/0/1">Paweł Preś</a>
We studied light curves of GJ 1243, YZ CMi, and V374 Peg, observed by TESS
for the presence of stellar spots and stellar flares. One of the main goals was
to model light curves of spotted stars to estimate the number of spots along
with their parameters using our original BASSMAN software. The modeled light
curves were subtracted from the observations to increase efficiency of flare
detection. Flares were detected automatically with our new dedicated software
WARPFINDER. We estimated the presence of two spots on GJ 1243 with mean
temperature about 2800$,$K and spottedness varying between $3%-4%$ of the
stellar surface and two spots on V374 Peg with a mean temperature of about
3000$,$K and spottedness about 6$%$ of the stellar surface. On YZ CMi we
found two different models for two light curves separated in time by one and a
half year. One of them is three-spot model with mean temperature of about
3000$,$K and spottedness of star about 9$%$ of the stellar surface. The
second is a four-spot model with mean temperature about 2800$,$K and
spottedness about 7$%$ of the stellar surface. We tested whether the flares
are distributed homogeneously in phase and if there is any correlation between
the presence of spots and the distribution of flares. For YZ CMi one spot is in
anticorrelation with the distribution of the flares and for GJ 1243 shows
non-homogeneous distribution of flares.
We studied light curves of GJ 1243, YZ CMi, and V374 Peg, observed by TESS
for the presence of stellar spots and stellar flares. One of the main goals was
to model light curves of spotted stars to estimate the number of spots along
with their parameters using our original BASSMAN software. The modeled light
curves were subtracted from the observations to increase efficiency of flare
detection. Flares were detected automatically with our new dedicated software
WARPFINDER. We estimated the presence of two spots on GJ 1243 with mean
temperature about 2800$,$K and spottedness varying between $3%-4%$ of the
stellar surface and two spots on V374 Peg with a mean temperature of about
3000$,$K and spottedness about 6$%$ of the stellar surface. On YZ CMi we
found two different models for two light curves separated in time by one and a
half year. One of them is three-spot model with mean temperature of about
3000$,$K and spottedness of star about 9$%$ of the stellar surface. The
second is a four-spot model with mean temperature about 2800$,$K and
spottedness about 7$%$ of the stellar surface. We tested whether the flares
are distributed homogeneously in phase and if there is any correlation between
the presence of spots and the distribution of flares. For YZ CMi one spot is in
anticorrelation with the distribution of the flares and for GJ 1243 shows
non-homogeneous distribution of flares.
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