FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY

被引：229

作者：

Huber, Daniel ^{[1
]}

Chaplin, William J. ^{[2
,3
]}

Christensen-Dalsgaard, Jorgen ^{[3
]}

Gilliland, Ronald L. ^{[4
]}

Kjeldsen, Hans ^{[3
]}

Buchhave, Lars A. ^{[5
,6
]}

Fischer, Debra A. ^{[7
]}

Lissauer, Jack J. ^{[1
]}

Rowe, Jason F. ^{[1
]}

Sanchis-Ojeda, Roberto ^{[8
]}

Basu, Sarbani ^{[7
]}

Handberg, Rasmus ^{[3
]}

Hekker, Saskia ^{[9
]}

Howard, Andrew W. ^{[10
]}

Isaacson, Howard ^{[11
]}

Karoff, Christoffer ^{[3
]}

Latham, David W. ^{[12
]}

Lund, Mikkel N. ^{[3
]}

Lundkvist, Mia ^{[3
]}

Marcy, Geoffrey W. ^{[11
]}

Miglio, Andrea ^{[2
]}

Aguirre, Victor Silva ^{[3
]}

Stello, Dennis ^{[3
,13
]}

Arentoft, Torben ^{[3
]}

Barclay, Thomas ^{[1
]}

Bedding, Timothy R. ^{[3
,13
]}

Burke, Christopher J. ^{[1
]}

Christiansen, Jessie L. ^{[1
]}

Elsworth, Yvonne P. ^{[2
]}

Haas, Michael R. ^{[1
]}

Kawaler, Steven D. ^{[14
]}

Metcalfe, Travis S. ^{[15
]}

Mullally, Fergal ^{[1
]}

Thompson, Susan E. ^{[1
]}

机构：

[1] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[2] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[3] Aarhus Univ, Dept Phys & Astron, Stellar Astrophys Ctr, DK-8000 Aarhus C, Denmark

[4] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA

[5] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark

[6] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark

[7] Yale Univ, Dept Astron, New Haven, CT 06511 USA

[8] MIT, Dept Phys, Cambridge, MA 02139 USA

[9] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands

[10] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[11] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[12] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[13] Univ Sydney, Sch Phys, Sydney Inst Astron SIfA, Sydney, NSW 2006, Australia

[14] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA

[15] Space Sci Inst, Boulder, CO 80301 USA

来源：

ASTROPHYSICAL JOURNAL | 2013年 / 767卷 / 02期

基金：

美国国家科学基金会; 欧洲研究理事会; 新加坡国家研究基金会;

关键词：

planetary systems; stars: late-type; stars: oscillations; techniques: photometric; techniques: spectroscopic; SOLAR-LIKE OSCILLATIONS; TRANSIT TIMING OBSERVATIONS; 1ST; 4; MONTHS; RED GIANTS; MAIN-SEQUENCE; EXTRASOLAR PLANETS; OPEN CLUSTERS; NGC; 6791; ECCENTRICITY DISTRIBUTION; INITIAL CHARACTERISTICS;

D O I：

10.1088/0004-637X/767/2/127

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：17