Zhou, George 
ORCID: https://orcid.org/0000-0002-4891-3517 and Rodriguez, Joseph E. and Collins, Karen A. and Beatty, Thomas and Oberst, Thomas and Heintz, Tyler M. and Stassun, Keivan G. and Latham, David W. and Kuhn, Rudolf B. and Bieryla, Allyson and Lund, Michael B. and Labadie-Bartz, Jonathan and Siverd, Robert J. and Stevens, Daniel J. and Gaudi, B. Scott and Pepper, Joshua and Buchhave, Lars A. and Eastman, Jason and Colon, Knicole and Cargile, Phillip and James, David and Gregorio, Joao and Reed, Phillip A. and Jensen, Eric L. N. and Cohen, David H. and McLeod, Kim K. and Tan, T. G. and Zambelli, Roberto and Bayliss, Daniel and Bento, Joao and Esquerdo, Gilbert A. and Berlind, Perry and Calkins, Michael L. and Blancato, Kirsten and Manner, Mark and Samulski, Camile and Stockdale, Christopher and Nelson, Peter and Stephens, Denise and Curtis, Ivan and Kielkopf, John and Fulton, Benjamin J. and DePoy, D. L. and Marshall, Jennifer L. and Pogge, Richard and Gould, Andy and Trueblood, Mark and Trueblood, Pat
(2016)
KELT-17b: A Hot-Jupiter Transiting an A-star in a Misaligned Orbit Detected with Doppler Tomography.
The Astronomical Journal, 152 (5):136.
pp. 1-15.
ISSN 0004-6256
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Text (Accepted Version)
1607.03512.pdf Download (1MB) | Preview |
Abstract
We present the discovery of a hot Jupiter transiting the V = 9.23 mag main-sequence A-star KELT-17 (BD+14 1881). KELT-17b is a , hot-Jupiter in a 3.08-day period orbit misaligned at -115.°9 ± 4.°1 to the rotation axis of the star. The planet is confirmed via both the detection of the radial velocity orbit, and the Doppler tomographic detection of the shadow of the planet during two transits. The nature of the spin-orbit misaligned transit geometry allows us to place a constraint on the level of differential rotation in the host star; we find that KELT-17 is consistent with both rigid-body rotation and solar differential rotation rates (at significance). KELT-17 is only the fourth A-star with a confirmed transiting planet, and with a mass of , an effective temperature of 7454 ± 49 K, and a projected rotational velocity of it is among the most massive, hottest, and most rapidly rotating of known planet hosts.
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| Item Type: | Article (Commonwealth Reporting Category C) |
|---|---|
| Refereed: | Yes |
| Item Status: | Live Archive |
| Faculty/School / Institute/Centre: | No Faculty |
| Faculty/School / Institute/Centre: | No Faculty |
| Date Deposited: | 03 Feb 2022 00:28 |
| Last Modified: | 07 Feb 2022 04:58 |
| Uncontrolled Keywords: | Planets and satellites: individual (KELT-17b); stars: individual (KELT-17, BD+14 1881, TYC 807-903-1); Astrophysics - Earth and Planetary; Astrophysics |
| Fields of Research (2008): | 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems |
| Fields of Research (2020): | 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems |
| Socio-Economic Objectives (2008): | E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences |
| Socio-Economic Objectives (2020): | 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences |
| Identification Number or DOI: | https://doi.org/10.3847/0004-6256/152/5/136 |
| URI: | http://eprints.usq.edu.au/id/eprint/45055 |
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