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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Eylen-2014-What asteroseismolog.pdf
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Author(s)
Van Eylen, V.
Lund, Mikkel N.
Aguirre, V. Silva
Arentoft, T.
Kjeldsen, H.
Albrecht, Simon H.
Chaplin, William J.
Isaacson, Howard
Pedersen, M. G.
Jessen-Hansen, J.
Date Issued
February 2014
Journal
Astrophysical Journal
Publisher
Institute of Physics/American Astronomical Society
Citation
Van Eylen, V., M. N. Lund, V. Silva Aguirre, T. Arentoft, H. Kjeldsen, S. Albrecht, W. J. Chaplin, et al. “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.” The Astrophysical Journal 782, no. 1 (January 21, 2014): 14. © 2014 American Astronomical Society.
Version
Final published version
Abstract
We confirm the Kepler planet candidate Kepler-410A b (KOI-42b) as a Neptune-sized exoplanet on a 17.8 day, eccentric orbit around the bright (K p = 9.4) star Kepler-410A (KOI-42A). 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. We determine via asteroseismology the following stellar and planetary parameters with high precision; M [subscript *] = 1.214 ± 0.033 M ☉, R [subscript *] = 1.352 ± 0.010 R ☉, age =2.76 ± 0.54 Gyr, planetary radius (2.838 ± 0.054 R ⊕), and orbital eccentricity (0.17[+0.07 over -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 over -2.5] [°] indicates a low obliquity in this system. Transit timing variations indicate the presence of at least one additional (non-transiting) planet (Kepler-410A c) in the system.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637X/782/1/14
