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Using planetary transits to estimate magnetic cycles lengths in Kepler stars

Published online by Cambridge University Press:  12 September 2017

Raissa Estrela  and
Adriana Valio
Raissa Estrela
Affiliation:
Center for Radio Astronomy and Astrophysics (CRAAM), Mackenzie Presbyterian University, Sao Paulo, Brazil email: rlf.estrela@gmail.com Rua da Consolacao01301-000, 896, Sao Paulo, Brazil email: avalio@craam.mackenzie.br
Adriana Valio
Affiliation:
Center for Radio Astronomy and Astrophysics (CRAAM), Mackenzie Presbyterian University, Sao Paulo, Brazil email: rlf.estrela@gmail.com Rua da Consolacao01301-000, 896, Sao Paulo, Brazil email: avalio@craam.mackenzie.br
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Abstract

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Observations of various solar-type stars along decades showed that they could have magnetic cycles, just like our Sun. These observations yield a relation between the rotation period Prot and the cycle length Pcycle of these stars. Two distinct branches for the cycling stars were identified: active and inactive, classified according to stellar activity level and rotation rate. In this work, we determined the magnetic activity cycle for 6 active stars observed by the Kepler telescope. The method adopted here estimates the activity from the excess in the residuals of the transit light curves. This excess is obtained by subtracting a spotless model transit from the light curve, and then integrating over all the residuals during the transit. The presence of long term periodicity is estimated from the analysis of a Lomb-Scargle periodogram of the complete time series. Finally, we investigate the rotation-cycle period relation for the stars analysed here.

Keywords

magneticactivityrotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 152 - 158
Copyright
Copyright © International Astronomical Union 2017 

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