HATS-70b: A 13 MJ Brown Dwarf Transiting an A Star
Article
Article Title | HATS-70b: A 13 MJ Brown Dwarf Transiting an A Star |
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ERA Journal ID | 1048 |
Article Category | Article |
Authors | Zhou, G. (Author), Bakos, G. A. (Author), Bayliss, D. (Author), Bento, J. (Author), Bhatti, W. (Author), Brahm, R. (Author), Csubry, Z. (Author), Espinoza, N. (Author), Hartman, J. D. (Author), Henning, T. (Author), Jordan, A. (Author), Mancini, L. (Author), Penev, K. (Author), Rabus, M. (Author), Sarkis, P. (Author), Suc, V. (Author), de Val-Borro, M. (Author), Rodriguez, J. E. (Author), Osip, D. (Author), Kedziora-Chudczer, L. (Author), Bailey, J. (Author), Tinney, C. G. (Author), Durkan, S. (Author), Lazar, J. (Author), Papp, I. (Author) and Sari, P. (Author) |
Journal Title | The Astronomical Journal |
Journal Citation | 157 (1), pp. 1-14 |
Article Number | 31 |
Number of Pages | 14 |
Year | 2019 |
Publisher | IOP Publishing |
Place of Publication | United States |
ISSN | 0004-6256 |
1538-3881 | |
Digital Object Identifier (DOI) | https://doi.org/10.3847/1538-3881/aaf1bb |
Web Address (URL) | https://iopscience.iop.org/article/10.3847/1538-3881/aaf1bb |
Abstract | We report the discovery of HATS-70b, a transiting brown dwarf at the deuterium burning limit. HATS-70b has a mass of Mp = 12.9+1.8-1.6 MJup and a radius of Rp 1.384+ 0.074 0.079 MJup, residing in a close-in orbit with a period of 1.89 days. The host star is a M∗= M 1.78 0.12 M A star rotating at = v sin I 40.61+ km s- 0.35 0.32 1, enabling us to characterize the spectroscopic transit of the brown dwarf via Doppler tomography. We find that HATS-70b, like other massive planets and brown dwarfs previously sampled, orbits in a low projected-obliquity orbit with l = 8.9+4.5 5.6. The low obliquities of these systems is surprising given all brown dwarf and massive planets with obliquities measured orbit stars hotter than the Kraft break. This trend is tentatively inconsistent with dynamically chaotic migration for systems with massive companions, though the stronger tidal influence of these companions makes it difficult to draw conclusions on the primordial obliquity distribution of this population. We also introduce a modeling scheme for planets around rapidly rotating stars, accounting for the influence of gravity darkening on the derived stellar and planetary parameters. |
Keywords | stars: individual (HATS-70); techniques: spectroscopic; techniques: photometric; 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 | Center for Astrophysics Harvard and Smithsonian, United States |
Princeton University, United States | |
University of Warwick, United Kingdom | |
Australian National University | |
Millennium Institute of Astrophysics, Chile | |
Max Planck Society, Germany | |
Pontifical Catholic University of Chile, Chile | |
University of Texas at Dallas, United States | |
NASA Goddard Space Flight Center, United States | |
Carnegie Institution of Washington, United States | |
University of New South Wales | |
Queen's University Belfast, United Kingdom | |
Hungarian Astronomical Association, Hungary |
https://research.usq.edu.au/item/q6x6z/hats-70b-a-13-mj-brown-dwarf-transiting-an-a-star
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