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Fundamental Properties of Kepler Planet-Candidate Host Stars using Asteroseismology

Huber, Daniel and Howard, Andrew W. (2013) Fundamental Properties of Kepler Planet-Candidate Host Stars using Asteroseismology. Astrophysical Journal, 767 (2). Art. No. 127. ISSN 0004-637X. doi:10.1088/0004-637X/767/2/127.

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We have used asteroseismology to determine fundamental properties for 66 Kepler planet-candidate host stars, with typical uncertainties of 3% and 7% in radius and mass, respectively. The results include new asteroseismic solutions for four host stars with confirmed planets (Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total number of Kepler host stars with asteroseismic solutions to 77. A comparison with stellar properties in the planet-candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow-up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement. We furthermore apply asteroseismology to confirm that a large majority of cool main-sequence hosts are indeed dwarfs and not misclassified giants. Using the revised stellar properties, we recalculate the radii for 107 planet candidates in our sample, and comment on candidates for which the radii change from a previously giant-planet/brown-dwarf/stellar regime to a sub-Jupiter size or vice versa. A comparison of stellar densities from asteroseismology with densities derived from transit models in Batalha et al. assuming circular orbits shows significant disagreement for more than half of the sample due to systematics in the modeled impact parameters or due to planet candidates that may be in eccentric orbits. Finally, we investigate tentative correlations between host-star masses and planet-candidate radii, orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases.

Item Type:Article
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URLURL TypeDescription Paper
Huber, Daniel0000-0001-8832-4488
Howard, Andrew W.0000-0001-8638-0320
Additional Information:© 2013 The American Astronomical Society. Received 2012 December 20; accepted 2013 February 8; published 2013 April 4. We thank Willie Torres, Josh Winn, and our anonymous referee for helpful comments and discussions. We furthermore gratefully acknowledge the entire Kepler team and everyone involved in the Kepler mission for making this paper possible. Funding for the Kepler mission is provided by NASA's Science Mission Directorate. D.H. is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. S.B. acknowledges NSF grant AST-1105930. S.H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). T.S.M. acknowledges NASA grant NNX13AE91G. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (Grant agreement No.: 267864).
Funding AgencyGrant Number
NASA Postdoctoral ProgramUNSPECIFIED
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)UNSPECIFIED
Danish National Research FoundationDNRF106
European Research Council (ERC)267864 ASTERISK
Subject Keywords:planetary systems – stars: late-type – stars: oscillations – techniques: photometric – techniques: spectroscopic
Issue or Number:2
Record Number:CaltechAUTHORS:20170621-143657842
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Official Citation:Daniel Huber et al 2013 ApJ 767 127
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78428
Deposited By: Tony Diaz
Deposited On:21 Jun 2017 21:50
Last Modified:15 Nov 2021 17:39

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