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Statistical Study of Solar White-light Flares and Comparison with Superflares on Solar-type Stars

  • Kosuke Namekata (a1), Takahito Sakaue (a1), Kyoko Watanabe (a2), Ayumi Asai (a3) (a4), Hiroyuki Maehara (a1), Yuta Notsu (a1), Shota Notsu (a1), Satoshi Honda (a5), Takako T. Ishii (a3), Kai Ikuta (a1), Daisaku Nogami (a1) and Kazunari Shibata (a3) (a4)...

Abstract

Recently, many superflares on solar-type stars were discovered as white-light flares (WLFs). A correlation between the energies (E) and durations (t) of superflares is derived as tE0.39, and this can be theoretically explained by magnetic reconnection (tE1/3). In this study, we carried out a statistical research on 50 solar WLFs with SDO/HMI to examine the t-E relation. As a result, the t-E relation on solar WLFs (tE0.38) is quite similar stellar superflares, but the durations of stellar superflares are much shorter than those extrapolated from solar WLFs. We present the following two interpretations; (1) in solar flares, the cooling timescale of WL emission may be longer than the reconnection one, and the decay time can be determined by the cooling timescale; (2) the distribution can be understood by applying a scaling law tE1/3B−5/3 derived from the magnetic reconnection theory.

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References

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Statistical Study of Solar White-light Flares and Comparison with Superflares on Solar-type Stars

  • Kosuke Namekata (a1), Takahito Sakaue (a1), Kyoko Watanabe (a2), Ayumi Asai (a3) (a4), Hiroyuki Maehara (a1), Yuta Notsu (a1), Shota Notsu (a1), Satoshi Honda (a5), Takako T. Ishii (a3), Kai Ikuta (a1), Daisaku Nogami (a1) and Kazunari Shibata (a3) (a4)...

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