Asteroseismology of the ZZ Ceti star WD 1310+583 using the Transiting Exoplanet Survey Satellite

¹ Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences, MTA Centre of Excellence H-1121 Budapest Konkoly Thege Miklós út 15-17, Hungary
² Institute of Astronomy, KU Leuven Celestijnenlaan 200D B-3001 Leuven, Belgium
³ Instituto de Astrofísica de La Plata, IALP (CCT La Plata), CONICET-UNLP La Plata, Argentina
⁴ Grupo de Evolución Estelar y Pulsaciones. Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata Paseo del Bosque s/n (1900) La Plata, Argentina
⁵ Department of Physics, Gibbet Hill Road University of Warwick Coventry CV4 7AL, United Kingdom
⁶ Department of Astronomy, University of Texas at Austin Austin TX-78712, USA
⁷ McDonald Observatory Fort Davis TX-79734, USA

^★ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.

Received: 11 August 2025
Accepted: 12 January 2026

Abstract

Aims. By analysing the light curves of the ZZ Ceti star WD 1310+583, we aim to determine its pulsational frequencies and to give constraints on the main stellar parameters using asteroseismology.

Methods. We performed the Fourier analysis of the TESS light curves of WD 1310+583 and selected the possible pulsational modes. We also used spectroscopic data collected with the Cosmic Origins Spectrograph of the Hubble Space Telescope to give constraints for the asteroseismic analysis. We perform the latter with period-to-period fits using fully evolutionary white dwarf models.

Results. The star presented in this paper shows a particularly high number (41) of pulsational frequencies, which provides a potential opportunity for detailed asteroseismic investigations. We found a mean period spacing of ∼40.5 seconds, which allows us to state that the stellar mass of WD 1310+583 is larger than ∼0.57 M_⊙. We also attempted an asteroseismological analysis by performing period-to-period fits, but we were unable to find a single statistically significant asteroseismological solution. We adopted a tentative solution consisting of a white dwarf model with M_* = 0.632 M_⊙, T_eff = 11 702 K, and an asteroseismic distance d = 27.75_−0.15^+0.17 pc, which is significantly smaller than the one predicted by Gaia (d = 30.79 ± 0.2 pc). We also determined that the rotational period of our target is 1.18 d.