EPIC 246851721 b: A Tropical Jupiter Transiting a Rapidly Rotating Star in a Well-aligned Orbit
Article
Article Title | EPIC 246851721 b: A Tropical Jupiter Transiting a Rapidly Rotating Star in a Well-aligned Orbit |
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ERA Journal ID | 1048 |
Article Category | Article |
Authors | Yu, Liang (Author), Zhou, George (Author), Rodriguez, Joseph E. (Author), Huang, Chelsea X. (Author), Vanderburg, Andrew (Author), Quinn, Samuel N. (Author), Gaudi, B. Scott (Author), Beichman, Charles A. (Author), Berlind, Perry (Author), Bieryla, Allyson (Author), Calkins, Michael L. (Author), Ciardi, David R. (Author), Crossfield, Ian J. M. (Author), Eastman, Jason D. (Author), Esquerdo, Gilbert A. (Author), Latham, David W. (Author), Stassun, Keivan G. (Author) and Villanueva, Steven, Jr. (Author) |
Journal Title | The Astronomical Journal |
Journal Citation | 156 (6), pp. 1-13 |
Article Number | 250 |
Number of Pages | 13 |
Year | 2018 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-6256 |
1538-3881 | |
Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/aae5d5 |
Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/aae5d5 |
Abstract | We report the discovery of EPIC 246851721 b, a 'tropical' Jupiter in a 6.18-day orbit around the bright (V = 11.439) star EPIC 246851721 (TYC 1283-739-1). We present a detailed analysis of the system using K2 and ground-based photometry, radial velocities, Doppler tomography, and adaptive optics imaging. From our global models, we infer that the host star is a rapidly rotating (nu sin I-* = 74.92 km s(-1)) F dwarf with T-eff = 6202 K, R-* = 1.586 R-circle dot and M-* = 1.317 M-circle dot. EPIC 246851721 b has a radius of 1.051 +/- 0.044 R-J, and a mass of 3.0(-1.2)(+1.1) M-J. Doppler tomography reveals an aligned spin-orbit geometry, with a projected obliquity of -1.degrees 47(-0.86)(+0.87), making EPIC 246851721 the fourth hottest star to host a Jovian planet with P > 5 days and a known obliquity. Using quasi-periodic signatures in its light curve that appear to be spot modulations, we estimate the star's rotation period, and thereby infer the true obliquity of the system to be 3.degrees 7(-1.8)(+3.7). We argue that this near-zero obliquity is likely to be primordial rather than a result of tidal damping. The host star also has a bound stellar companion, a 0.4 M-circle dot M dwarf at a projected separation of 2100 au, but the companion is likely incapable of emplacing EPIC 246851721 b in its current orbit via high-eccentricity Kozai-Lidov migration. |
Keywords | planetary systems; planets and satellites: detection; stars: individual (EPIC 246851721); Astrophysics - Earth and Planetary Astrophysics |
Contains Sensitive Content | Does not contain sensitive content |
ANZSRC Field of Research 2020 | 510109. Stellar astronomy and planetary systems |
Public Notes | File reproduced in accordance with the copyright policy of the publisher/author. |
Institution of Origin | University of Southern Queensland |
Byline Affiliations | Massachusetts Institute of Technology, United States |
Center for Astrophysics Harvard and Smithsonian, United States | |
University of Texas at Austin, United States | |
Ohio State University, United States | |
National Aeronautics and Space Administration (NASA), United States | |
Vanderbilt University, United States |
https://research.usq.edu.au/item/q6x6w/epic-246851721-b-a-tropical-jupiter-transiting-a-rapidly-rotating-star-in-a-well-aligned-orbit
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