Investigating photometric variability in M-dwarfs
Stellar Variability, Stellar Flares, M-dwarfs.
M-dwarf stars are the most common stars in our galaxy, comprising approximately 75% of the Milky Way's stellar population.
They are expected to host a significant number of Earth-mass planets in the habitable zone. This study will analyze both low-
and high-cadence light curves of M-dwarf stars observed by the Kepler and Transiting Exoplanet Survey Satellite (TESS)
missions. To identify various forms of stellar variability, including those related to rotation, potential pulsations (oscillations),
binarity, and flares, specific analytical methods will be employed. The Fast Fourier Transform (FFT), Lomb-Scargle
periodogram, and the wavelet map will be used to determine the periodicities of these variations. Stellar flares will be detected
and characterized using the AltaiPony algorithm, with energy estimates calculated based on the properties identified in each
event. The results of this study will provide a significant contribution to the understanding of the variability of these stars,
deepening the knowledge of their intrinsic behaviors and characteristics.