TESS Asteroseismic Analysis of the Known Exoplanet Host Star HD 222076

• Type: Article in International Scientific Journal
• Date: 2020

Authors

Jiang, C (Author) Other; Bedding, TR (Author) Other; Stassun, KG (Author) Other; Veras, D (Author) Other; Corsaro, E (Author) Other; Buzasi, DL (Author) Other; Mikolajczyk, P (Author) Other; Zhang, QS (Author) Other; Ou, JW (Author) Other; Campante, TL (Author) Other; Rodrigues, TS (Author) Other; Nsamba, B (Author) Other; Bossini, D (Author) Other; Kane, SR (Author) Other; Ong, JMJ (Author) Other; Yildiz, M (Author) Other; Orhan, ZC (Author) Other; Ortel, S (Author) Other; Wu, T (Author) Other; Zhang, XY (Author) Other; Li, TD (Author) Other; Basu, S (Author) Other; Cunha, MS (Author) FCUP; Christensen Dalsgaard, J (Author) Other; Chaplin, WJ (Author) Other

Journal

Title: Astrophysical Journal

Vol. 896

Final page: 65

ISSN: 0004-637X

Publisher: American Astronomical Society

Indexing

ISI Web of Knowledge - 3 Citations

Scopus - 4 Citations

Other information

Authenticus ID: P-00S-EH7

DOI: 10.3847/1538-4357/ab8f29

Abstract (EN): The Transiting Exoplanet Survey Satellite (TESS) is an all-sky survey mission aiming to search for exoplanets that transit bright stars. The high-quality photometric data of TESS are excellent for the asteroseismic study of solar-like stars. In this work, we present an asteroseismic analysis of the red-giant star HD 222076 hosting a long-period (2.4 yr) giant planet discovered through radial velocities. Solar-like oscillations of HD 222076 are detected around 203 mu Hz by TESS for the first time. Asteroseismic modeling, using global asteroseismic parameters as inputs, yields a determination of the stellar mass (M-* = 1.12 +/- 0.12 M-circle dot), radius (R-* = 4.34 +/- 0.21 R-circle dot), and age (7.4 +/- 2.7 Gyr), with precisions greatly improved from previous studies. The period spacing of the dipolar mixed modes extracted from the observed power spectrum reveals that the star is on the red-giant branch burning hydrogen in a shell surrounding the core. We find that the planet will not escape the tidal pull of the star and will be engulfed into it within about 800 Myr, before the tip of the red-giant branch is reached.

Language: English

Type (Professor's evaluation): Scientific

No. of pages: 10