Properties of Kepler Stars with the Most Powerful Flaresстатья
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Дата последнего поиска статьи во внешних источниках: 22 февраля 2019 г.
Аннотация:We analyze physical characteristics of late-type stars wherein the Kepler mission registered superflares. We use the revised fundamental parameters, i.e. effective temperatures Teff and surface gravity accelerations log g, as compared to previous studies. Among superflare stars there are both single object and members of eclipsing binaries. We select the late-type stars (with T_eff < 6500 K) wherein occured the most powerful flares with the total flare energy >10^35 erg and consider their locations in the T_eff — log g diagram. Both components of binaries and single stars appear to reside mostly in between the main sequence and the subgiant branches and therefore have larger radii compared to that of the Sun. Besides, as a rule these single stars are fast rotators and can be considered as young objects that it is difficult to attribute to “solar-type stars”. Extremely high flare energy of these stars requires quite strong magnetic fields that can not to be generated even due to scaling of the solar dynamo. Apparently, for explanation of the strongest non-stationary phenomena on stars considered, it would be worthwhile to attract another regime of the dynamo mechanism that can be realized in these objects.