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Statistical properties of superflares on solar-type stars based on the Kepler 1-min cadence data

Published online by Cambridge University Press:  09 September 2016

Hiroyuki Maehara ,
Takuya Shibayama ,
Yuta Notsu ,
Shota Notsu ,
Satoshi Honda ,
Daisaku Nogami  and
Kazunari Shibata
Hiroyuki Maehara*
Affiliation:
Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, 3037-5 Honjo, Kamogata, Asakuchi, Okayama, Japan, 719-0232
Takuya Shibayama
Affiliation:
Institute for Space-Earth Environmental Research, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi, Japan, 464-8601
Yuta Notsu
Affiliation:
Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Japan, 606-8502
Shota Notsu
Affiliation:
Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Japan, 606-8502
Satoshi Honda
Affiliation:
Center for Astronomy, University of Hyogo, 407-2, Nishigaichi, Sayo-cho, Sayo, Hyogo, Japan, 679-5313
Daisaku Nogami
Affiliation:
Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Japan, 606-8502
Kazunari Shibata
Affiliation:
Kwasan and Hida Observatories, Kyoto University, Yamashina-ku, Kyoto, Japan, 607-8471
*
*email: h.maehara@oao.nao.ac.jp
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Abstract

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We searched for superflares on solar-type stars using the Kepler short-cadence (1-min sampling) data in order to detect superflares with short duration. We found 187 superflares on 23 solar-type stars whose bolometric energy ranges from the order of 1032 erg to 1036 erg. Using these new data combined with the results from the data with 30-min sampling, we found the occurrence frequency (dN/dE) of superflares as a function of flare energy (E) shows the power-law distribution (dN/dE ∝ E−α) with α=1.5 for 1033 < E < 1036 erg. The upper limit of energy released by superflares is basically comparable to a fraction of the magnetic energy stored near starspots which is estimated from the amplitude of brightness variations. We also found that the duration of superflares (τ) increases with the flare energy (E) as τ ∝ E0.39±0.03. This can be explained if we assume the time-scale of flares is determined by the Alfvén time.

Keywords

stars:activitystars:flarestars:solar-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S320: Solar and Stellar Flares and their Effects on Planets , August 2015 , pp. 144 - 149
Copyright
Copyright © International Astronomical Union 2016 

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