Asteroseismology study of a new faint ZZ Ceti J053009.62+594557.0 discovered in WFST

TL;DR

This paper presents the first detailed asteroseismological analysis of a newly discovered faint white dwarf, using high-precision photometry and spectroscopy to determine its internal structure and confirm its properties.

Contribution

The study provides the first asteroseismological modeling of WFST J053009.62+594557.0, combining photometry, spectroscopy, and evolutionary models to accurately determine its physical parameters.

Findings

Identified three significant pulsation frequencies.

Derived stellar parameters consistent with Gaia data.

Confirmed the white dwarf's internal structure through modeling.

Abstract

In this work, we present a detailed asteroseismological analysis of WFST J053009.62+594557.0, a newly discovered faint pulsating white dwarf by the Wide Field Survey Telescope (WFST) with a Gaia G magnitude of 19.13. Analysis of two nights of high-precision WFST g band photometry reveals three significant pulsation frequencies with high signal-to-noise ratios. Follow-up P200/DBSP spectroscopy classifies the object as a DA white dwarf with Teff=11,609 $\pm$ 605 K and M = 0.63$\pm$ 0.22 $M_{\odot}$. To probe its internal structure, we construct asteroseismological models with the White Dwarf Evolution Code (WDEC). After exploring sufficient matching models, best-fitting solutions yield Teff=11,850$\pm$ 10 K and M = 0.600 $\pm$ 0.005 $M_{\odot}$, consistent with independent constraints from Gaia color-magnitude diagram, Gaia XP spectrum, P200 spectral fitting, SED fitting, and Gaia parallax. It has shown that the asteroseismological distance agrees with the Gaia parallax to 1.45\%.