Stellar Rotation Period Versus Energy Variation of Flares in TESS Stars of Spectral Types K and M
Keywords: Flares, Spectral types K and M Stars, Rotation Period, TESS
Under the development of new technologies, the Aerospace Engineering is increasingly
improving its equipments in order to assist exploration that goes beyond our Heliopause.
As an example of this we can cite the launch of the space artfact Transiting Exoplanet Survey Satellite
(TESS) that has been contributing photometric data to Space Sciences, like Astrophysics,
with the aim of study various physical phenomena. As an exemple, the magnetic activity
of stars can be fundamental in forming the atmosphere of exoplanets and impact your
habitability as well as, it can trigger life in the orbit of type K and M stars, which are
considered to be cold and they are the most numerous in the main sequence phase in
the Hertzsprung-Russell diagram. Based on these investigations and through statistical
analysis of the behavior of stellar flares in relation to their classi cations, rotational periods
and spectral subtype, this dissertation presents a study on the variation of energie
of stellar flares as a function of their rotational period in a sample of 679 TESS stars of
spectral type K and M. None of the stars in this sample showed a correlation between the
energy of their surface stellar eruptions as a function of their rotational period. Finally
we present four scenarios involving the stars and their stellar eruptions and theirs that
can explain our results.