http://arxiv.org/abs/2212.10224
We wrote and used an automated flare detection Python script to search for super-flares on main-sequence stars of types A, F, G, K, and M in the entire Kepler’s long-cadence data from Q0 to Q17 following Shibayama et al. 2013 method. Hence, we extended previous studies by Shibayama et al. 2013, who considered a smaller number of quarters, Q0-Q6, and on G-type dwarfs only. Using these new data, we studied the statistical properties of the occurrence rate of super-flares using three different data-sets, namely, Q0-Q6, Q7-Q17 and Q0-Q17 and provide their inter-comparison. For Q0-Q17 data-set we estimated that a super-flare on G-type dwarfs of energy of $10^{35}$ erg occurs on a star once every 4360 years. We found 4637 super-flares on 1896 G-type dwarfs. Moreover, we found 321, 1125, 4538 and 5445 super-flares on 136, 522, 770 and 312 dwarfs of types A, F, K and M respectively. We found that the occurrence rate ($dN/dE$) of super-flares versus flare energy, $E$, shows a power-law distribution with $dN/dE \propto E^{-\alpha}$, where $\alpha \simeq$ 2.0 to 2.1 for all different spectral types from F-type to M-type stars. The similarity of the power-law index values implies that the flares are generated by similar conditions in the underlying physical mechanism, which is believed to be magnetic reconnection. In contrast, the obtained $\alpha \simeq$ 1.3 for A-type stars suggests that the flare conditions are different from the rest spectral type stars. We note a general increase in flare incidence rate 4.79 \% – 14.04 \% in F-type to M-type stars and a slight decrease in flare incidence rate 5.13 \% – 4.79 \% in A-type to F-type stars. These results are similar to other results, who studied stars with any size, not necessarily the main-sequence, considered here.
A. Althukair and D. Tsiklauri
Wed, 21 Dec 22
75/81
Comments: Submitted for publication in MNRAS
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