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Properties of Kepler Stars with the Most Powerful Flaresстатья
Информация о цитировании статьи получена из
Web of Science,
Scopus
Дата последнего поиска статьи во внешних источниках: 22 февраля 2019 г.
- Авторы: Katsova M.M., Nizamov B.A.
- Сборник: ArXiv Solar and Stellar Astrophysics
- Серия: 1812.09580
- Том: 12
- Год издания: 2018
- Место издания: Cornell University Library Ithaca, New York astro-ph.SR
- Первая страница: 1
- Последняя страница: 7
- DOI: 10.1134/S0016793218070095
- Аннотация: We analyze physical characteristics of late-type stars wherein the Kepler mission registered superflares. We use the revised stellar fundamental parameters, i.e. effective temperatures T_eff and surface gravitational accelerations log g, from the Kepler archive published in 2017, as compared to previous studies by Balona (2015) based on the release of 2011. 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 cannot 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.
- Добавил в систему: Кацова Мария Михайловна