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Spin-orbit alignment of exoplanet systems: how can Asteroseismology help us?

Published online by Cambridge University Press:  27 October 2016

Tiago L. Campante
Tiago L. Campante*
Affiliation:
School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK email: campante@bison.ph.bham.ac.uk Stellar Astrophysics Centre (SAC), Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
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Abstract

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Measuring the obliquities of exoplanet-host stars provides invaluable diagnostic information for theories of planetary formation and migration. Most of these results have so far been obtained by measuring the Rossiter--McLaughlin effect, clearly favoring systems that harbor hot Jupiters. While it would be extremely helpful to extend these measurements to long-period and multiple-planet systems, it is also true that the latter systems tend to involve smaller planets, making it ever so difficult to apply such techniques. Asteroseismology provides a powerful method of determining the inclination of the stellar spin axis from an analysis of the rotationally-induced splittings of the oscillation modes. This provides an estimate of the obliquity independently of other methods. The applicability of the asteroseismic method is determined by the stellar properties and not by the signal-to-noise ratio of the transit data. Here we present a recap of the spin-orbit geometry, explain how the asteroseismic method works, and review previous applications of the method to exoplanet-host stars.

Keywords

asteroseismologymethods: statisticalplanetary systemsplanets and satellites: generalstars: solar-typetechniques: photometric
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29A: Astronomy in Focus , August 2015 , pp. 71 - 76
Copyright
Copyright © International Astronomical Union 2016 

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