Mode identification in three pulsating hot subdwarfs observed with TESS satellite. Issue 3 (14th May 2020)

• Record Type: Journal Article
• Authors: Sahoo, S K; Baran, A S; Heber, U; Ostrowski, J; Sanjayan, S; Silvotti, R; Irrgang, A; Uzundag, M; Reed, M D; Shoaf, K A; Raddi, R; Vuckovic, M; Ghasemi, H; Zong, W; Bell, K J
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 495:Issue 3(2020)
• Page Start: 2844
• Page End: 2857
• Publication Date: 2020-05-14
• Subjects: asteroseismology -- stars: oscillations (including pulsations) -- subdwarfs; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa1337
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We report on the detection of pulsations of three pulsating subdwarf B stars observed by the Transiting Exoplanet Survey Satellite (TESS ) satellite and our results of mode identification in these stars based on an asymptotic period relation. SB 459 (TIC 067584818), SB 815 (TIC 169285097), and PG 0342 + 026 (TIC 457168745) have been monitored during single sectors resulting in 27 d coverage. These data sets allowed for detecting, in each star, a few tens of frequencies that we interpreted as stellar oscillations. We found no multiplets, though we partially constrained mode geometry by means of period spacing, which recently became a key tool in analyses of pulsating subdwarf B stars. Standard routine that we have used allowed us to select candidates for trapped modes that surely bear signatures of non-uniform chemical profile inside the stars. We have also done statistical analysis using collected spectroscopic and asteroseismic data of previously known subdwarf B stars along with our three stars. Making use of high precision trigonometric parallaxes from the Gaia mission and spectral energy distributions we converted atmospheric parameters to stellar ones. Radii, masses, and luminosities are close to their canonical values for extreme horizontal branch stars. In particular, the stellar masses are close to the canonical one of 0.47 M⊙ for all three stars but uncertainties on the mass are large. The results of the analyses presented here will provide important constrains for asteroseismic modelling.