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

被引：1
|
作者：
Maehara, Hiroyuki [1 ]
Shibayama, Takuya [2 ]
Notsu, Yuta [3 ]
Notsu, Shota [3 ]
Honda, Satoshi [4 ]
Nogami, Daisaku [3 ]
Shibata, Kazunari [5 ]
机构：
[1] Natl Astron Observ Japan, Okayama Astrophys Observ, 3037-5 Honjo, Asakuchi, Okayama 7190232, Japan
[2] Nagoya Univ, Inst Space Earth Environm Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan
[3] Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan
[4] Univ Hyogo, Ctr Astron, 407-2 Nishigaichi,Sayo Cho, Sayo, Hyogo 6795313, Japan
[5] Kyoto Univ, Kwasan & Hida Observ, Yamashina Ku, Kyoto 6078471, Japan
来源：
SOLAR AND STELLAR FLARES AND THEIR EFFECTS ON PLANETS | 2016年 / 11卷 / S320期
关键词：
stars:activity; stars:flare; stars:solar-type; ENERGETICS;
D O I：
10.1017/S1743921316000065
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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 10(32) erg to 10(36) 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 proportional to E-alpha) with alpha = 1.5 for 10(33) < E < 10(36) 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 (tau) increases with the flare energy (E) as tau proportional to E-0.39 +/- 0.03. This can be explained if we assume the time-scale of flares is determined by the Alfven time.
引用
收藏
页码：144 / 149
页数：6
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