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TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting an Extremely Eccentric Exoplanet
Journal article   Open access   Peer reviewed

TESS Asteroseismic Analysis of HD 76920: The Giant Star Hosting an Extremely Eccentric Exoplanet

Jiang Chen, Tao Wu, Adina Feinstein, Keivan Stassun, Timothy Bedding, Dimitri Veras, Enrico Corsaro, Derek Buzasi, Dennis Stello, Yaguang Li, …
The Astrophysical journal, Vol.945(1), p.20
03-01-2023

Abstract

Giant stars Light curve Parameters Planet detection Solar oscillations Stellar envelopes Stellar mass Stellar models Stellar oscillations Stellar seismology Transit Extrasolar Planets Mathematical Models Orbits
The Transiting Exoplanet Survey Satellite (TESS) mission searches for new exoplanets. The observing strategy of TESS results in high-precision photometry of millions of stars across the sky, allowing for detailed asteroseismic studies of individual systems. In this work, we present a detailed asteroseismic analysis of the giant star HD 76920 hosting a highly eccentric giant planet (e = 0.878) with an orbital period of 415 days, using five sectors of TESS light curve that cover around 140 days of data. Solar-like oscillations in HD 76920 are detected around 52 μHz by TESS for the first time. By utilizing asteroseismic modeling that takes classical observational parameters and stellar oscillation frequencies as constraints, we determine improved measurements of the stellar mass (1.22 ± 0.11 M⊙), radius (8.68 ± 0.34 R☉), and age (5.2 ± 1.4 Gyr). With the updated parameters of the host star, we update the semimajor axis and mass of the planet as a = 1.165 ± 0.035 au and Mpsini=3.57±0.22MJup. With an orbital pericenter of 0.142 ± 0.005 au, we confirm that the planet is currently far away enough from the star to experience negligible tidal decay until being engulfed in the stellar envelope. We also confirm that this event will occur within about 100 Myr, depending on the stellar model used.
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