Fundamental properties of Kepler planet-candidate host stars using asteroseismology

Daniel Huber; William J. Chaplin; Jørgen Christensen-Dalsgaard; Ronald L. Gilliland; Hans Kjeldsen; Lars A. Buchhave; Debra A. Fischer; Jacj J. Lissauer; Jason F. Rowe; Roberto Sanchis-Ojeda; Sarbani Basu; Rasmus Handberg; Saskia Hekker; Andrew W. Howard; Howard Isaacson; Christoffer Karoff; David W. Latham; Mikkel N. Lund; Mia Lundkvist; Geoffrey W. Marcy; Andrea Miglio; Victor Silva Aguirre; Dennis Stello; Torben Arentoft; Thomas Barclay; Timothy R. Bedding; Christopher J. Burke; Jessie L. Christiansen; Yvonne P. Elsworth; Michael R. Haas; Steven D. Kawaler; Travis S. Metcalfe; Fergal Mullally; Susan E. Thompson

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

Fundamental properties of Kepler planet-candidate host stars using asteroseismology

Daniel Huber, William J. Chaplin, Jørgen Christensen-Dalsgaard, Ronald L. Gilliland, Hans Kjeldsen, Lars A. Buchhave, Debra A. Fischer, Jacj J. Lissauer, Jason F. Rowe, Roberto Sanchis-Ojeda, Sarbani Basu, Rasmus Handberg, Saskia Hekker, Andrew W. Howard, Howard Isaacson, Christoffer Karoff, David W. Latham, Mikkel N. Lund, Mia Lundkvist, Geoffrey W. MarcyAndrea Miglio, Victor Silva Aguirre, Dennis Stello, Torben Arentoft, Thomas Barclay, Timothy R. Bedding, Christopher J. Burke, Jessie L. Christiansen, Yvonne P. Elsworth, Michael R. Haas, Steven D. Kawaler, Travis S. Metcalfe, Fergal Mullally, Susan E. Thompson

Astrofysik og Planetforskning

192 Citationer (Scopus)

Abstract

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.

Originalsprog	Engelsk
Artikelnummer	127
Tidsskrift	The Astrophysical Journal
Vol/bind	767
Udgave nummer	2
Antal sider	17
ISSN	0004-637X
DOI	https://doi.org/10.1088/0004-637X/767/2/127
Status	Udgivet - 20 apr. 2013

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

Citationsformater

Huber, D., Chaplin, W. J., Christensen-Dalsgaard, J., Gilliland, R. L., Kjeldsen, H., Buchhave, L. A., Fischer, D. A., Lissauer, J. J., Rowe, J. F., Sanchis-Ojeda, R., Basu, S., Handberg, R., Hekker, S., Howard, A. W., Isaacson, H., Karoff, C., Latham, D. W., Lund, M. N., Lundkvist, M., ... Thompson, S. E. (2013). Fundamental properties of Kepler planet-candidate host stars using asteroseismology. The Astrophysical Journal, 767(2), [127]. https://doi.org/10.1088/0004-637X/767/2/127

Huber, D, Chaplin, WJ, Christensen-Dalsgaard, J, Gilliland, RL, Kjeldsen, H, Buchhave, LA, Fischer, DA, Lissauer, JJ, Rowe, JF, Sanchis-Ojeda, R, Basu, S, Handberg, R, Hekker, S, Howard, AW, Isaacson, H, Karoff, C, Latham, DW, Lund, MN, Lundkvist, M, Marcy, GW, Miglio, A, Aguirre, VS, Stello, D, Arentoft, T, Barclay, T, Bedding, TR, Burke, CJ, Christiansen, JL, Elsworth, YP, Haas, MR, Kawaler, SD, Metcalfe, TS, Mullally, F & Thompson, SE 2013, 'Fundamental properties of Kepler planet-candidate host stars using asteroseismology', The Astrophysical Journal, bind 767, nr. 2, 127. https://doi.org/10.1088/0004-637X/767/2/127

@article{6058e811d002487fa3220df0508dfc77,

title = "Fundamental properties of Kepler planet-candidate host stars using asteroseismology",

abstract = "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.",

author = "Daniel Huber and Chaplin, {William J.} and J{\o}rgen Christensen-Dalsgaard and Gilliland, {Ronald L.} and Hans Kjeldsen and Buchhave, {Lars A.} and Fischer, {Debra A.} and Lissauer, {Jacj J.} and Rowe, {Jason F.} and Roberto Sanchis-Ojeda and Sarbani Basu and Rasmus Handberg and Saskia Hekker and Howard, {Andrew W.} and Howard Isaacson and Christoffer Karoff and Latham, {David W.} and Lund, {Mikkel N.} and Mia Lundkvist and Marcy, {Geoffrey W.} and Andrea Miglio and Aguirre, {Victor Silva} and Dennis Stello and Torben Arentoft and Thomas Barclay and Bedding, {Timothy R.} and Burke, {Christopher J.} and Christiansen, {Jessie L.} and Elsworth, {Yvonne P.} and Haas, {Michael R.} and Kawaler, {Steven D.} and Metcalfe, {Travis S.} and Fergal Mullally and Thompson, {Susan E.}",

year = "2013",

month = apr,

day = "20",

doi = "10.1088/0004-637X/767/2/127",

language = "English",

volume = "767",

journal = "Astrophysical Journal",

issn = "0004-637X",

publisher = "Institute of Physics Publishing, Inc",

number = "2",

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TY - JOUR

T1 - Fundamental properties of Kepler planet-candidate host stars using asteroseismology

AU - Huber, Daniel

AU - Chaplin, William J.

AU - Christensen-Dalsgaard, Jørgen

AU - Gilliland, Ronald L.

AU - Kjeldsen, Hans

AU - Buchhave, Lars A.

AU - Fischer, Debra A.

AU - Lissauer, Jacj J.

AU - Rowe, Jason F.

AU - Sanchis-Ojeda, Roberto

AU - Basu, Sarbani

AU - Handberg, Rasmus

AU - Hekker, Saskia

AU - Howard, Andrew W.

AU - Isaacson, Howard

AU - Karoff, Christoffer

AU - Latham, David W.

AU - Lund, Mikkel N.

AU - Lundkvist, Mia

AU - Marcy, Geoffrey W.

AU - Miglio, Andrea

AU - Aguirre, Victor Silva

AU - Stello, Dennis

AU - Arentoft, Torben

AU - Barclay, Thomas

AU - Bedding, Timothy R.

AU - Burke, Christopher J.

AU - Christiansen, Jessie L.

AU - Elsworth, Yvonne P.

AU - Haas, Michael R.

AU - Kawaler, Steven D.

AU - Metcalfe, Travis S.

AU - Mullally, Fergal

AU - Thompson, Susan E.

PY - 2013/4/20

Y1 - 2013/4/20

N2 - 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.

AB - 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.

U2 - 10.1088/0004-637X/767/2/127

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

M3 - Journal article

SN - 0004-637X

VL - 767

JO - Astrophysical Journal

JF - Astrophysical Journal

IS - 2

M1 - 127

ER -

Fundamental properties of Kepler planet-candidate host stars using asteroseismology

Abstract

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