https://doi.org/10.1051/epjconf/201510102007
3D spin-orbit angle of Kepler-25 and HAT-P-7
1 Department of Astronomy, The University of Tokyo, School of Science, Tokyo 113-0033
2 Department of Physics, The University of Tokyo, School of Science, Tokyo 113-0033
3 Research Center for the Early Universe, School of Science, The University of Tokyo, Tokyo 1130033
a e-mail: othman.benomar@astron.s.u-tokyo.ac.jp
Published online: 23 September 2015
The number of discovered exoplanets now exceeds 1500, mostly due to the Kepler space instrument observations. Many of these planet orbit in less than a week around their host stars. This implies that the inward migration of those planets is a basic ingredient of successful theories of planet formation and evolution. Several mechanisms have been proposed to explain the observed periods, which lead to different orbit eccentricity and obliquity distributions. Here we summarise and discuss the results of obliquities for two Kepler stars: HAT-P-7 and Kepler-25. These are interesting stellar systems as we could carry out a joint analysis using asteroseismology, transit lightcurve and the Rossiter-McLaughlin effect in order to measure the three dimensional obliquity.
© Owned by the authors, published by EDP Sciences, 2015
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
