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HD 76920 b pinned d...
HD 76920 b pinned down : A detailed analysis of the most eccentric planetary system around an evolved star
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- Bergmann, C. (author)
- German Aerospace Center (DLR),University of New South Wales
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- Jones, M. I. (author)
- Catholic University of the North,European Southern Observatory Santiago
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- Zhao, J. (author)
- University of New South Wales,Pennsylvania State University
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- Mustill, A. J. (author)
- Lund University,Lunds universitet,Astronomi - Genomgår omorganisation,Institutionen för astronomi och teoretisk fysik - Genomgår omorganisation,Naturvetenskapliga fakulteten,Lund Observatory - Undergoing reorganization,Department of Astronomy and Theoretical Physics - Undergoing reorganization,Faculty of Science
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- Brahm, R. (author)
- Millennium Institute for Astrophysics,Adolfo Ibañez University
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- Torres, P. (author)
- Pontifical Catholic University of Chile
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- Wittenmyer, R. A. (author)
- University of Southern Queensland
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- Gunn, F. (author)
- Canterbury University
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- Pollard, K. R. (author)
- Canterbury University
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- Zapata, A. (author)
- Pontifical Catholic University of Chile
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- Vanzi, L. (author)
- Pontifical Catholic University of Chile
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- Wang, Songhu (author)
- Indiana University
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(creator_code:org_t)
- 2021-04-22
- 2021
- English.
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In: Publications of the Astronomical Society of Australia. - : Cambridge University Press (CUP). - 1323-3580 .- 1448-6083. ; 38
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https://arxiv.org/ab... (free)
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http://dx.doi.org/10...
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Abstract
Subject headings
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- We present 63 new multi-site radial velocity (RV) measurements of the K1III giant HD 76920, which was recently reported to host the most eccentric planet known to orbit an evolved star. We focused our observational efforts on the time around the predicted periastron passage and achieved near-continuous phase coverage of the corresponding RV peak. By combining our RV measurements from four different instruments with previously published ones, we confirm the highly eccentric nature of the system and find an even higher eccentricity of , an orbital period of , and a minimum mass of for the planet. The uncertainties in the orbital elements are greatly reduced, especially for the period and eccentricity. We also performed a detailed spectroscopic analysis to derive atmospheric stellar parameters, and thus the fundamental stellar parameters (), taking into account the parallax from Gaia DR2, and independently determined the stellar mass and radius using asteroseismology. Intriguingly, at periastron, the planet comes to within 2.4 stellar radii of its host star's surface. However, we find that the planet is not currently experiencing any significant orbital decay and will not be engulfed by the stellar envelope for at least another 50-80 Myr. Finally, while we calculate a relatively high transit probability of 16%, we did not detect a transit in the TESS photometry.
Subject headings
- NATURVETENSKAP -- Fysik -- Astronomi, astrofysik och kosmologi (hsv//swe)
- NATURAL SCIENCES -- Physical Sciences -- Astronomy, Astrophysics and Cosmology (hsv//eng)
Keyword
- 76920
- Keywords
- planetary systems
- stars: individual: HD
- techniques: radial velocities
Publication and Content Type
- art (subject category)
- ref (subject category)
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Bergmann, C.
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Jones, M. I.
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Zhao, J.
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Mustill, A. J.
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Brahm, R.
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Torres, P.
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Wittenmyer, R. A ...
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Gunn, F.
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Pollard, K. R.
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Zapata, A.
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Vanzi, L.
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Wang, Songhu
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- NATURAL SCIENCES
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NATURAL SCIENCES
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Lund University