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Title:
Radius Determination of Solar-type Stars Using Asteroseismology: What to Expect from the Kepler Mission
Authors:
Stello, Dennis; Chaplin, William J.; Bruntt, Hans; Creevey, Orlagh L.; García-Hernández, Antonio; Monteiro, Mario J. P. F. G.; Moya, Andrés; Quirion, Pierre-Olivier; Sousa, Sergio G.; Suárez, Juan-Carlos; Appourchaux, Thierry; Arentoft, Torben; Ballot, Jerome; Bedding, Timothy R.; Christensen-Dalsgaard, Jørgen; Elsworth, Yvonne; Fletcher, Stephen T.; García, Rafael A.; Houdek, Günter; Jiménez-Reyes, Sebastian J.; Kjeldsen, Hans; New, Roger; Régulo, Clara; Salabert, David; Toutain, Thierry
Affiliation:
AA(Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia ; Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark ; ), AB(School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK ), AC(Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia ), AD(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ), AE(Instituto de Astrofísica de Andalucía, CSIC, CP3004 Granada, Spain ), AF(Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal ; Departamento de Matemática Aplicada, Faculdade de Ciências da Universidade do Porto, Porto, Portugal ), AG(Instituto de Astrofísica de Andalucía, CSIC, CP3004 Granada, Spain ), AH(Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark ), AI(Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal ; Departamento de Matemática Aplicada, Faculdade de Ciências da Universidade do Porto, Porto, Portugal ), AJ(Instituto de Astrofísica de Andalucía, CSIC, CP3004 Granada, Spain ), AK(Institut d' Astrophysique Spatiale (IAS), UMR8617, Batiment 121, F-91405 Orsay Cedex, France ), AL(Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark ), AM(Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, Postfach 1317, 85741 Garching, Germany ; Laboratoire d RAstrophysique de Toulouse-Tarbes, Universit de Toulouse, CNRS, 14 avenue Edouard Belin, F-31400 Toulouse, France ), AN(Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, Sydney, NSW 2006, Australia ), AO(Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark ), AP(School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK ), AQ(Faculty of Arts, Computing, Engineering and Sciences, Sheffield Hallam University, Sheffield S1 1WB, UK ), AR(Laboratoire AIM, CEA/DSM-CNRS-Université Paris Diderot, CEA, IRFU, SAp, centre de Saclay, F-91191 Gif-sur-Yvette, France ), AS(Institute of Astronomy, University of Vienna, A-1180 Vienna, Austria ; Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK ), AT(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ), AU(Danish AsteroSeismology Centre (DASC), Department of Physics and Astronomy, Aarhus University, 8000 Aarhus C, Denmark ), AV(Laboratoire d RAstrophysique de Toulouse-Tarbes, Universit de Toulouse, CNRS, 14 avenue Edouard Belin, F-31400 Toulouse, France ), AW(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; Departamento de Astrofísica, Universidad de La Laguna, La Laguna 38206, Tenerife, Spain ), AX(Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain ; National Solar Observatory, 950 North Cherry Avenue, Tucson, AZ 85719, USA), AY(School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK )
Publication:
The Astrophysical Journal, Volume 700, Issue 2, pp. 1589-1602 (2009). (ApJ Homepage)
Publication Date:
08/2009
Origin:
IOP
ApJ Keywords:
stars: fundamental parameters, stars: interiors, stars: oscillations
DOI:
10.1088/0004-637X/700/2/1589
Bibliographic Code:
2009ApJ...700.1589S

Abstract

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. We investigated stars in the range 9 < V < 15, both with and without parallaxes. We further test different uncertainties in T eff, and compare results with and without using asteroseismic constraints. Based on the asteroseismic large frequency spacing, obtained from simulations of 4 yr 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. Given the uncertainties used for this exercise we find that the input log g and parallax do not help to constrain the radius, and that T eff and metallicity are the only parameters we need in addition to the large frequency spacing. It is the uncertainty in the metallicity that dominates the uncertainty in the radius.
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