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Mikkel Nørup Lund

What asteroseismology can do for exoplanets: Kepler-410A b is a Small Neptune around a bright star, in an eccentric orbit consistent with low obliquity

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What asteroseismology can do for exoplanets: Kepler-410A b is a Small Neptune around a bright star, in an eccentric orbit consistent with low obliquity. / Van Eylen, Vincent; Lund, Mikkel N.; Silva Aguirre, Victor; Arentoft, Torben; Kjeldsen, Hans; Albrecht, Simon; Chaplin, William J.; Isaacson, Howard; Pedersen, May G.; Jessen-Hansen, Jens; Tingley, Brandon W.; Christensen-Dalsgaard, Joergen; Aerts, Conny; Campante, Tiago L.; Bryson, Stephen T.

I: Astrophysical Journal, Bind 782, Nr. 1, 21.01.2014.

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avisTidsskriftartikelForskningpeer review

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Van Eylen, Vincent ; Lund, Mikkel N. ; Silva Aguirre, Victor ; Arentoft, Torben ; Kjeldsen, Hans ; Albrecht, Simon ; Chaplin, William J. ; Isaacson, Howard ; Pedersen, May G. ; Jessen-Hansen, Jens ; Tingley, Brandon W. ; Christensen-Dalsgaard, Joergen ; Aerts, Conny ; Campante, Tiago L. ; Bryson, Stephen T. / What asteroseismology can do for exoplanets: Kepler-410A b is a Small Neptune around a bright star, in an eccentric orbit consistent with low obliquity. I: Astrophysical Journal. 2014 ; Bind 782, Nr. 1.

Bibtex

@article{4b6e3aece40a4194a0609c21604eb639,
title = "What asteroseismology can do for exoplanets: Kepler-410A b is a Small Neptune around a bright star, in an eccentric orbit consistent with low obliquity",
abstract = "We confirm the Kepler planet candidate Kepler-410b (KOI-42b) as a Neptune sized exoplanet on a 17.8 day, eccentric orbit around the bright (Kp = 9.4) star Kepler-410A. This is the third brightest confirmed planet host star in the Kepler field and one of the brightest hosts of all currently known transiting exoplanets. Kepler-410 consists of a blend between the fast rotating planet host star (Kepler-410A) and a fainter star (Kepler-410B), which has complicated the confirmation of the planetary candidate. Employing asteroseismology, using constraints from the transit light curve, adaptive optics and speckle images, and Spitzer transit observations, we demonstrate that the candidate can only be an exoplanet orbiting Kepler-410A. Via asteroseismology we determine the following stellar and planetary parameters with high precision; M$_\star = 1.214 \pm 0.033$ M$_\odot$, R$_\star = 1.352 \pm 0.010$ R$_\odot$, Age = $2.76 \pm 0.54$ Gyr, planetary radius ($2.838 \pm 0.054$ R$_\oplus$), and orbital eccentricity ($0.17^{+0.07}_{-0.06}$). In addition, rotational splitting of the pulsation modes allows for a measurement of Kepler-410A's inclination and rotation rate. Our measurement of an inclination of $82.5^{+7.5}_{-2.5}$ [$^\circ$] indicates a low obliquity in this system. Transit timing variations indicate the presence of at least one additional (non-transiting) planet in the system.",
keywords = "Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics",
author = "{Van Eylen}, Vincent and Lund, {Mikkel N.} and {Silva Aguirre}, Victor and Torben Arentoft and Hans Kjeldsen and Simon Albrecht and Chaplin, {William J.} and Howard Isaacson and Pedersen, {May G.} and Jens Jessen-Hansen and Tingley, {Brandon W.} and Joergen Christensen-Dalsgaard and Conny Aerts and Campante, {Tiago L.} and Bryson, {Stephen T.}",
year = "2014",
month = jan,
day = "21",
doi = "10.1088/0004-637X/782/1/14",
language = "English",
volume = "782",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing, Inc",
number = "1",

}

RIS

TY - JOUR

T1 - What asteroseismology can do for exoplanets: Kepler-410A b is a Small Neptune around a bright star, in an eccentric orbit consistent with low obliquity

AU - Van Eylen, Vincent

AU - Lund, Mikkel N.

AU - Silva Aguirre, Victor

AU - Arentoft, Torben

AU - Kjeldsen, Hans

AU - Albrecht, Simon

AU - Chaplin, William J.

AU - Isaacson, Howard

AU - Pedersen, May G.

AU - Jessen-Hansen, Jens

AU - Tingley, Brandon W.

AU - Christensen-Dalsgaard, Joergen

AU - Aerts, Conny

AU - Campante, Tiago L.

AU - Bryson, Stephen T.

PY - 2014/1/21

Y1 - 2014/1/21

N2 - We confirm the Kepler planet candidate Kepler-410b (KOI-42b) as a Neptune sized exoplanet on a 17.8 day, eccentric orbit around the bright (Kp = 9.4) star Kepler-410A. This is the third brightest confirmed planet host star in the Kepler field and one of the brightest hosts of all currently known transiting exoplanets. Kepler-410 consists of a blend between the fast rotating planet host star (Kepler-410A) and a fainter star (Kepler-410B), which has complicated the confirmation of the planetary candidate. Employing asteroseismology, using constraints from the transit light curve, adaptive optics and speckle images, and Spitzer transit observations, we demonstrate that the candidate can only be an exoplanet orbiting Kepler-410A. Via asteroseismology we determine the following stellar and planetary parameters with high precision; M$_\star = 1.214 \pm 0.033$ M$_\odot$, R$_\star = 1.352 \pm 0.010$ R$_\odot$, Age = $2.76 \pm 0.54$ Gyr, planetary radius ($2.838 \pm 0.054$ R$_\oplus$), and orbital eccentricity ($0.17^{+0.07}_{-0.06}$). In addition, rotational splitting of the pulsation modes allows for a measurement of Kepler-410A's inclination and rotation rate. Our measurement of an inclination of $82.5^{+7.5}_{-2.5}$ [$^\circ$] indicates a low obliquity in this system. Transit timing variations indicate the presence of at least one additional (non-transiting) planet in the system.

AB - We confirm the Kepler planet candidate Kepler-410b (KOI-42b) as a Neptune sized exoplanet on a 17.8 day, eccentric orbit around the bright (Kp = 9.4) star Kepler-410A. This is the third brightest confirmed planet host star in the Kepler field and one of the brightest hosts of all currently known transiting exoplanets. Kepler-410 consists of a blend between the fast rotating planet host star (Kepler-410A) and a fainter star (Kepler-410B), which has complicated the confirmation of the planetary candidate. Employing asteroseismology, using constraints from the transit light curve, adaptive optics and speckle images, and Spitzer transit observations, we demonstrate that the candidate can only be an exoplanet orbiting Kepler-410A. Via asteroseismology we determine the following stellar and planetary parameters with high precision; M$_\star = 1.214 \pm 0.033$ M$_\odot$, R$_\star = 1.352 \pm 0.010$ R$_\odot$, Age = $2.76 \pm 0.54$ Gyr, planetary radius ($2.838 \pm 0.054$ R$_\oplus$), and orbital eccentricity ($0.17^{+0.07}_{-0.06}$). In addition, rotational splitting of the pulsation modes allows for a measurement of Kepler-410A's inclination and rotation rate. Our measurement of an inclination of $82.5^{+7.5}_{-2.5}$ [$^\circ$] indicates a low obliquity in this system. Transit timing variations indicate the presence of at least one additional (non-transiting) planet in the system.

KW - Astrophysics - Earth and Planetary Astrophysics

KW - Astrophysics - Solar and Stellar Astrophysics

U2 - 10.1088/0004-637X/782/1/14

DO - 10.1088/0004-637X/782/1/14

M3 - Journal article

VL - 782

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -