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The Flaring Activity of M Dwarfs in the Kepler Field
Yang, Huiqin1,2; Liu, Jifeng1,2; Gao, Qing1; Fang, Xuan3,4; Guo, Jincheng5; Zhang, Yong6; Hou, Yonghui6; Wang, Yuefei6; Cao, Zihuang1
2017-11-01
Source PublicationASTROPHYSICAL JOURNAL
Volume849Issue:1
AbstractFlare events are mainly due to magnetic reconnection and thus are indicative of stellar activity. The Kepler Space Observatory records numerous stellar activities with unprecedented high photometric precision in flux measurements. It is perfectly suitable for carrying out a statistical study of flares. Here we present 540 M dwarfs with flare events discovered using Kepler long-cadence data. The normalized flare energy, as defined by the ratio to bolometric stellar luminosity, L-flare/L-bol, is used to indicate the flare activity. We find that, similar to the X-ray luminosity relation, the L-flare/L-bol versus P-rot relation can also be described with three phases, supersaturation, saturation, and exponential decay, corresponding to an ultra-short period, a short period, and a long period. The flare activity and the number fraction of flaring stars in M dwarfs rise steeply near M4, which is consistent with the prediction of a turbulent dynamo. The size of starspots are positively correlated with flare activity. The L-flare/L-bol ratio has a power-law dependence on L-H alpha/L-bol, a parameter indicative of stellar chromosphere activity. According to this relation, a small enhancement in chromosphere activity may cause a huge rise in flare energy, which suggests that superflares or hyperflares may not need an extra excitation mechanism. Through a comparison study, we suggest that flare activity is a more suitable indicator for stellar activity, especially in the boundary region. However, contrary to what is expected, some M dwarfs with strong flares do not show any light variation caused by starspots. Follow-up observations are needed to investigate this problem.
SubtypeArticle
KeywordStars: Activity Stars: Flare Stars: Late-type Stars: Statistics Starspots
WOS HeadingsScience & Technology ; Physical Sciences
Funding OrganizationChinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; 973 Program(2014CB845705) ; 973 Program(2014CB845705) ; National Science Foundation of China(NSFC-11333004/11425313) ; National Science Foundation of China(NSFC-11333004/11425313) ; NASA Science Mission Directorate ; NASA Science Mission Directorate ; NASA(NAS5-26555) ; NASA(NAS5-26555) ; NASA Office of Space Science(NNX09AF08G) ; NASA Office of Space Science(NNX09AF08G) ; National Development and Reform Commission ; National Development and Reform Commission ; Chinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; 973 Program(2014CB845705) ; 973 Program(2014CB845705) ; National Science Foundation of China(NSFC-11333004/11425313) ; National Science Foundation of China(NSFC-11333004/11425313) ; NASA Science Mission Directorate ; NASA Science Mission Directorate ; NASA(NAS5-26555) ; NASA(NAS5-26555) ; NASA Office of Space Science(NNX09AF08G) ; NASA Office of Space Science(NNX09AF08G) ; National Development and Reform Commission ; National Development and Reform Commission
DOI10.3847/1538-4357/aa8ea2
WOS KeywordSPECTROSCOPIC TELESCOPE LAMOST ; SCALE MAGNETIC TOPOLOGIES ; MAIN-SEQUENCE STARS ; X-RAY-EMISSION ; OPEN CLUSTER ; COOL STARS ; SKY SURVEY ; SUPERSATURATION ; ROTATION ; SUPERFLARES
Indexed BySCI
Language英语
Funding OrganizationChinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; 973 Program(2014CB845705) ; 973 Program(2014CB845705) ; National Science Foundation of China(NSFC-11333004/11425313) ; National Science Foundation of China(NSFC-11333004/11425313) ; NASA Science Mission Directorate ; NASA Science Mission Directorate ; NASA(NAS5-26555) ; NASA(NAS5-26555) ; NASA Office of Space Science(NNX09AF08G) ; NASA Office of Space Science(NNX09AF08G) ; National Development and Reform Commission ; National Development and Reform Commission ; Chinese Academy of Sciences(XDB09000000) ; Chinese Academy of Sciences(XDB09000000) ; 973 Program(2014CB845705) ; 973 Program(2014CB845705) ; National Science Foundation of China(NSFC-11333004/11425313) ; National Science Foundation of China(NSFC-11333004/11425313) ; NASA Science Mission Directorate ; NASA Science Mission Directorate ; NASA(NAS5-26555) ; NASA(NAS5-26555) ; NASA Office of Space Science(NNX09AF08G) ; NASA Office of Space Science(NNX09AF08G) ; National Development and Reform Commission ; National Development and Reform Commission
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000413865300007
Citation statistics
Cited Times:16[WOS]   [WOS Record]     [Related Records in WOS]
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/20188
Collection光学天文研究部
Affiliation1.Chinese Acad Sci, Key Lab Opt Astron, Natl Astron Observ, Beijing 100012, Peoples R China
2.Univ Chinese Acad Sci, Beijing 100049, Peoples R China
3.Univ Hong Kong, Lab Space Res, Pokfulam, Hong Kong, Peoples R China
4.Univ Hong Kong, Dept Earth Sci, Pokfulam, Hong Kong, Peoples R China
5.Peking Univ, Dept Astron, Beijing 100871, Peoples R China
6.Chinese Acad Sci, Natl Astron Observ, Nanjing Inst Astron Opt & Technol, Nanjing 210042, Jiangsu, Peoples R China
Recommended Citation
GB/T 7714
Yang, Huiqin,Liu, Jifeng,Gao, Qing,et al. The Flaring Activity of M Dwarfs in the Kepler Field[J]. ASTROPHYSICAL JOURNAL,2017,849(1).
APA Yang, Huiqin.,Liu, Jifeng.,Gao, Qing.,Fang, Xuan.,Guo, Jincheng.,...&Cao, Zihuang.(2017).The Flaring Activity of M Dwarfs in the Kepler Field.ASTROPHYSICAL JOURNAL,849(1).
MLA Yang, Huiqin,et al."The Flaring Activity of M Dwarfs in the Kepler Field".ASTROPHYSICAL JOURNAL 849.1(2017).
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