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Magnetic Activity Discrepancies of Solar-Type Stars Revealed by Kepler Light Curves

Published online by Cambridge University Press:  24 July 2018

Han He Open the ORCID record for Han He [Opens in a new window] ,
Huaning Wang ,
Yan Yan  and
Duo Yun
Han He*
Affiliation:
CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
Huaning Wang
Affiliation:
CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
Yan Yan
Affiliation:
CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
Duo Yun
Affiliation:
CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
*
* *email: hehan@nao.cas.cn
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Abstract

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Magnetic activity information is concealed in the shape of stellar light curves owing to the process of rotational modulation. We developed approaches to extract magnetic activity characteristics from stellar light curves, and applied the method to a solar-type star observed with Kepler space telescope and also to the Sun for comparison. The result reveals distinct magnetic activity discrepancies between the solar-type star and the Sun. (1) The light-curve periodicity of the solar-type star is generally stronger than that of the Sun. (2) For the solar-type star, when the range of light-curve fluctuation is larger, the periodicity is also higher; while for the Sun, only during the solar minima with minimal range of fluctuation, the light curves show some periodicity. We propose that on the solar-type star, it is the large-scale magnetic field that leads to the light curves with both high periodicity and large range of fluctuation.

Keywords

stars: activitystars: magnetic fieldstars: rotationstars: solar-typeSun: activity
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S335: Space Weather of the Heliosphere: Processes and Forecasts , July 2017 , pp. 7 - 10
Copyright
Copyright © International Astronomical Union 2018 

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