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Rotation Profile of Kepler-63 from Planetary Transits

Published online by Cambridge University Press:  27 January 2016

Yuri Netto  and
Adriana Valio
Yuri Netto
Affiliation:
Centro de Rádio Astronomia e Astrofísica Mackenzie (CRAAM), São Paulo, Brasil email: [email protected]
Adriana Valio
Affiliation:
Centro de Rádio Astronomia e Astrofísica Mackenzie (CRAAM), São Paulo, Brasil email: [email protected]
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Abstract

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Currently it is possible to estimate the rotation profile of a star that harbours a planet in an orbit such that it eclipses the star periodically. During one of these transits, the planet may occult a spot on the photosphere of the star, causing small variations in its light curve. By detecting the same spot in a later transit, it is possible to estimate the stellar rotation period. Here we present the results of this model for the case of the star Kepler-63, which has a planet in an orbit with high obliquity. This means that the planetary eclipse occults many latitude bands of the star, from near the equator to the poles. The results show that Kepler-63 has differential rotation of 0.133 rd/d and a relative differential rotation of 11.4%.

Keywords

stars: rotation - starspots - planetary system - star: individual: Kepler-63
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S314: Young Stars & Planets Near the Sun , November 2015 , pp. 259 - 261
Copyright
Copyright © International Astronomical Union 2016 

References

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