Understanding the Characteristics of Active Regions which Produces Super Flares in M Stars

There is a renewed interest in the scientific studies of M stars in the recent times. This is because these low mass stars host many potentially habitable extra solar planets. In this paper we will study the characteristics of active regions which produces super flares in M dwarfs making use of relevant astronomical data. Energy of solar/stellar flares is understood to be related to the size and magnetic flux content of the active regions which produces the same. There is a theoretical upper limit to the magnetic flux content in solar active regions in which for a limiting flux of 7.23 X10²³ Mx the size of the active regions will be comparable to that of the solar radius. We cannot apply this scaling law to infer the size of the active regions in M stars which produces super flares of energy 10³⁴ -10³⁶ ergs because the radii of these stars are relatively small (0.3 to 0.7 solar radii). The magnetic flux associated with M star super flares is inferred to be between 10²⁴ -10²⁵ Mx. Further in contrast with kilo gauss fields found for sunspots we estimate magnetic fields of the order of 100-1000 kG for active regions in M stars. The emergence of exceptionally large magnetic flux in M stars is possibly related to higher poloidal to toroidal magnetic flux amplification factors in these stars compared to our Sun.