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HD 76920 b pinned down: A detailed analysis of the most eccentric planetary system around an evolved star

Published online by Cambridge University Press:  22 April 2021

C. Bergmann
Affiliation:
Exoplanetary Science at UNSW, School of Physics, UNSW Sydney, NSW 2052, Australia Deutsches Zentrum für Luft- und Raumfahrt, Münchener Str. 20, 82234 Weßling, Germany
M. I. Jones
Affiliation:
European Southern Observatory, Alonso de Córdova 3107, Casilla, Santiago 19001, Chile Instituto de Astronomía, Universidad Católica del Norte, Angamos 0610, Antofagasta 1270709, Chile
J. Zhao
Affiliation:
Exoplanetary Science at UNSW, School of Physics, UNSW Sydney, NSW 2052, Australia Penn State University, Department of Astronomy and Astrophysics, University Park, PA 16802, USA
A. J. Mustill
Affiliation:
Lund Observatory, Department of Astronomy & Theoretical Physics, Lund University, Box 43, Lund 221 00, Sweden
R. Brahm
Affiliation:
Millennium Institute for Astrophysics, Santiago, Chile Facultad de Ingeniería y Ciencias, Universidad Adolfo Ibáñez, Av. Diagonal las Torres 2640, Peñalolén, Santiago, Chile
P. Torres
Affiliation:
Department of Electrical Engineering and Center of Astro Engineering, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Santiago, Chile
R. A. Wittenmyer
Affiliation:
University of Southern Queensland, Centre for Astrophysics, Toowoomba, QLD 4350, Australia
F. Gunn
Affiliation:
School of Physical and Chemical Sciences, Te Kura Matū, University of Canterbury, Christchurch 8020, New Zealand
K. R. Pollard
Affiliation:
School of Physical and Chemical Sciences, Te Kura Matū, University of Canterbury, Christchurch 8020, New Zealand
A. Zapata
Affiliation:
Department of Electrical Engineering and Center of Astro Engineering, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Santiago, Chile
L. Vanzi
Affiliation:
Department of Electrical Engineering and Center of Astro Engineering, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Santiago, Chile
Songhu Wang
Affiliation:
Department of Astronomy, Indiana University, Bloomington, IN 47405, USA
Corresponding
E-mail address:

Abstract

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 $e=0.8782 \pm 0.0025$ , an orbital period of $415.891^{+0.043}_{-0.039}\,\textrm{d}$ , and a minimum mass of $3.13^{+0.41}_{-0.43}\,\textrm{M}_{\textrm{J}}$ 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 ( $M_*, R_*, L_*$ ), 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.

Type
Research Article
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of the Astronomical Society of Australia

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Footnotes

*

Visiting Astronomer, University of Canterbury Mt John Observatory.

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HD 76920 b pinned down: A detailed analysis of the most eccentric planetary system around an evolved star
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