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
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 curren...
| Main Authors: | , , , , , , , , , , , , , , |
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| Format: | Article |
| Language: | en_US |
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Institute of Physics/American Astronomical Society
2015
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| Online Access: | http://hdl.handle.net/1721.1/93250 |
| _version_ | 1811071250695454720 |
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| author | 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. Tingley, B. Christensen-Dalsgaard, J. Aerts, C. Campante, T. L. Bryson, Stephen T. |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics 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. Tingley, B. Christensen-Dalsgaard, J. Aerts, C. Campante, T. L. Bryson, Stephen T. |
| author_sort | Van Eylen, V. |
| collection | MIT |
| description | 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. |
| first_indexed | 2024-09-23T08:48:16Z |
| format | Article |
| id | mit-1721.1/93250 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T08:48:16Z |
| publishDate | 2015 |
| publisher | Institute of Physics/American Astronomical Society |
| record_format | dspace |
| spelling | mit-1721.1/932502022-09-30T11:22:29Z 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, 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. Tingley, B. Christensen-Dalsgaard, J. Aerts, C. Campante, T. L. Bryson, Stephen T. Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research Albrecht, Simon H. 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. Science and Technology Facilities Council (Great Britain) Danish Natural Science Research Council (grant agreement No. DNRF106) European Research Council (grant agreement No. 267864) United States. National Aeronautics and Space Administration (NASA Science Mission Directorate) 2015-01-30T20:46:39Z 2015-01-30T20:46:39Z 2014-02 2013-11 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/93250 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. en_US http://dx.doi.org/10.1088/0004-637X/782/1/14 Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf Institute of Physics/American Astronomical Society American Astronomical Society |
| spellingShingle | 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. Tingley, B. Christensen-Dalsgaard, J. Aerts, C. Campante, T. 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 |
| 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 |
| title_full | 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 |
| title_fullStr | 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 |
| title_full_unstemmed | 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 |
| title_short | 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 |
| title_sort | 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 |
| url | http://hdl.handle.net/1721.1/93250 |
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