https://doi.org/10.1051/epjconf/201510102005
What asteroseismology can do for exoplanets
1 Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark
2 Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200 B, B-3001 Heverlee, Belgium
3 Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA
4 Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, NSW 2006, Australia
5 School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham, B15 2TT, UK
6 Department of Astronomy, University of California, Berkeley, CA 94820, USA
7 NASA Ames Research Center, Moffett Field, CA 94035, USA
a e-mail: vincent@phys.au.dk
Published online: 23 September 2015
We describe three useful applications of asteroseismology in the context of exoplanet science: (1) the detailed characterisation of exoplanet host stars; (2) the measurement of stellar inclinations; and (3) the determination of orbital eccentricity from transit duration making use of asteroseismic stellar densities. We do so using the example system Kepler-410 [1]. This is one of the brightest (V = 9.4) Kepler exoplanet host stars, containing a small (2.8 R⊕) transiting planet in a long orbit (17.8 days), and one or more additional non-transiting planets as indicated by transit timing variations. The validation of Kepler-410 (KOI-42) was complicated due to the presence of a companion star, and the planetary nature of the system was confirmed after analyzing a Spitzer transit observation as well as ground-based follow-up observations.
© 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.
