Detalles de publicación
PP 09034
Radius determination of solar-type stars using asteroseismology: What to expect from the Kepler mission
1 Sydney Institute for Astronomy (SIfA), School of
Physics, University of Sydney, NSW 2006, Australia;
stello@physics.usyd.edu.au.
2 Danish AsteroSeismology Centre (DASC), Department of
Physics and Astronomy, Aarhus University, 8000 Aarhus C,
Denmark
3 School of Physics and Astronomy, University of Birmingham,
Edgbaston, Birmingham, B15 2TT, UK
4 Instituto de Astrof ́ ısica de Canarias, E-38200, La Laguna,
Tenerife, Spain
5 Instituto de Astrof ́ ısica de Andaluc ́ ıa, CSIC, CP3004,
Granada, Spain
6 Centro de Astrof ́ ısica da Universidade do Porto, Rua das
Estrelas, 4150-762 Porto, Portugal
7 Departamento de Matem ́tica Aplicada, Faculdade de Ciˆncias
a e
da Universidade do Porto, Portugal
8 Institut d’ Astrophysique Spatiale (IAS), UMR8617, Batiment
121, F-91405, Orsay Cedex, France
9 Max-Planck-Institut f ̈ r Astrophysik, Karl-Schwarzschild-Str.
u
1, Postfach 1317, 85741, Garching, Germany
10 Laboratoire d RAstrophysique de Toulouse-Tarbes, Universit
de Toulouse, CNRS, 14 avenue Edouard Belin, F-31400 Toulouse,
France
11 Faculty of Arts, Computing, Engineering and Sciences,
Sheffield Hallam University, Sheffield S1 1WB, UK
12 Laboratoire AIM, CEA/DSM-CNRS-Universit ́ Paris e
Diderot; CEA, IRFU, SAp, centre de Saclay, F-91191, Gif-sur-
Yvette, France
13 Institute of Astronomy, University of Vienna, A-1180 Vienna,
Austria
14 Institute of Astronomy, University of Cambridge, Cambridge
CB3 0HA, UK
15 Departamento de Astrof ́ ısica, Universidad de La Laguna, La
Laguna, 38206, Tenerife, Spain
16 National Solar Observatory, 950 North Cherry Avenue,
Tucson, AZ 85719, USA
For distant stars, as observed by the NASA Kepler satellite, parallax information is currently of fairly low quality and is not complete. This limits the precision with which the absolute sizes of the stars and their potential transiting planets can be determined by traditional methods. Asteroseismology will be used to aid the radius determination of stars observed during NASA's Kepler mission. We report on the recent asteroFLAG hare-and-hounds Exercise#2, where a group of `hares' simulated data of F-K main-sequence stars that a group of `hounds' sought to analyze, aimed at determining the stellar radii. Based on the asteroseismic large frequency spacing, obtained from simulations of 4-year time series data from the Kepler mission, we demonstrate that the stellar radii can be correctly and precisely determined, when combined with traditional stellar parameters from the Kepler Input Catalogue. The radii found by the various methods used by each independent hound generally agree with the true values of the artificial stars to within 3%, when the large frequency spacing is used. This is 5--10 times better than the results where seismology is not applied. These results give strong confidence that radius estimation can be performed to better than 3% for solar-like stars using automatic pipeline reduction. Even when the stellar distance and luminosity are unknown we can obtain the same level of agreement.