Estimating the Energy of Solar and Stellar Superflares
Abstract
We discuss the current observations of the most powerful non-steady phenomena on solar-like stars. While remaining within even the most extreme solar ideas, it is very problematic to get the flare energy more than (3-5) × 1034 erg, which is apparently an absolute upper limit for solar-type flares. For explanation of the higher flare energy, about of 1036 erg, one need to adopt that spots with the magnetic field strength of a few kG should cover more than 30% of a hemisphere. This estimate leads to a mean magnetic field around 1 kG. New observational evidences for a presence of the strong magnetic fields on solar-like stars appeared recently. We discuss to what extent it is necessary to change the mechanisms of convection and dynamo with a corresponding change in the models of the atmosphere. We consider possible ways of solving the problem of the energy of superflares.
- Publication:
-
Geomagnetism and Aeronomy
- Pub Date:
- December 2021
- DOI:
- 10.1134/S0016793221070094
- Bibcode:
- 2021Ge&Ae..61.1063K