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Phase difference between long-term magnetic feature activity and flare activity of solar-type stars

Published online by Cambridge University Press:  27 November 2018

Han He Open the ORCID record for Han He [Opens in a new window] ,
Huaning Wang ,
Mei Zhang ,
Ahmad Mehrabi ,
Yan Yan  and
Duo Yun
Han He*
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China CAS Key Laboratory of Solar Activity, Chinese Academy of Sciences, Beijing, China School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China
Huaning Wang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China CAS Key Laboratory of Solar Activity, Chinese Academy of Sciences, Beijing, China School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China
Mei Zhang
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China CAS Key Laboratory of Solar Activity, Chinese Academy of Sciences, Beijing, China School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China
Ahmad Mehrabi
Affiliation:
Department of Physics, Bu Ali Sina University, Hamedan, Iran School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, Iran
Yan Yan
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China CAS Key Laboratory of Solar Activity, Chinese Academy of Sciences, Beijing, China
Duo Yun
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China CAS Key Laboratory of Solar Activity, Chinese Academy of Sciences, Beijing, China School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China
*
*email: hehan@nao.cas.cn
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Abstract

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In the light curves of some solar-type stars, both rotational modulation (caused by corotating bright or dark magnetic features) and flare phenomena can be seen simultaneously. Based on these light curve observations, the relation between stellar magnetic feature activity (reflected by the rotational modulation component of the light curves) and flare activity can be investigated. Here, we analyze the light curve data of a flare-abundant solar-type star, KIC 6034120, observed with Kepler space telescope, and describe magnetic feature activity property by fluctuation range of light curves and flare activity property by time occupation ratio of flares. Distinct phase difference between long-term magnetic feature activity and flare activity is found for this star, which indicates that the source regions of stellar flares (e.g., starspots) on this star do not dominate the rotational modulation of light curves, yet they might be related to a same stellar dynamo process.

Keywords

stars: activitystars: flarestars: magnetic fieldstars: solar-typestars: spots
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S340: Long-term Datasets for the Understanding of Solar and Stellar Magnetic Cycles , February 2018 , pp. 217 - 220
Copyright
Copyright © International Astronomical Union 2018 

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