The Asteroseismology Analysis of 14 Solar-like Stars Based on TESS and LAMOST Observations

• Published in: The Astrophysical journal Vol. 934; no. 2; pp. 128 - 141
• Main Authors: Gai, Ning, Tang, Yanke, Li, Zhikai, Huang, Yang, Dong, Wenhui, Zhou, Xiaoshuang
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.08.2022; IOP Publishing
• Subjects: Asteroseismology; Astrophysics; Constraint modelling; Extrasolar planets; Grid method; Light curve; Maximum power; Parameters; Planet detection; Rapid stellar oscillations; Red giant stars; Satellite observation; Scaling; Sky surveys (astronomy); Solar oscillations; Stars; Stellar age; Stellar oscillations; Stellar properties; Stellar pulsations; Stellar seismology; Stellar structures; Transit
• DOI: 10.3847/1538-4357/ac7b7d
• ISSN: 0004-637X

The Transiting Exoplanet Survey Satellite (TESS) is performing a near all-sky survey for planets that transit bright stars. It provides excellent photometric data for asteroseismology of solar-like stars that exhibit oscillation by a convection-driven mechanism. In this paper, we analyze the light curves of 14 stars that are observed by TESS. These stars mainly focus on Sector 21 and the other Sectors intersecting with Sector 21. Through crossmatching with the LAMOST surveys, 14 stars with signals of solar-like oscillations are selected, and asteroseismic analysis is present. The frequency of maximum power ν max and the large frequency separation Δ ν are extracted from its frequency power spectrum using the pySYD pipeline. Scaling relations are an attractive method that can easily and immediately be applied to observations to derive the stellar properties. To validate the different calibrated scaling relations for 14 TESS stars, the fundamental stellar properties are estimated by the relations and compared with grid-based modeling results, which use the constraints of global asteroseismic parameters and nonasteroseismic parameters. The new red-giant branch (RGB) scaling relations are found to overestimate the radius and mass when compared to the grid results, while the f Δ ν scaling relations lead to overall lower radius and mass estimates. The average uncertainties of these stars from grid modeling are within 2% in the radius and 3% in the mass. Regardless of the method, we can get almost equally good results of log g for all the stars. Besides the grid method, the new RGB scaling relations for ages provide a simple and accurate method to determine the stellar ages.