The Pre-He White Dwarfs in Eclipsing Binaries. I. WASP 0131+28

TL;DR

This study presents detailed observational analysis of the binary star WASP 0131+28, revealing properties of an extremely low-mass white dwarf and its evolutionary status as an EL CVn system formed via Roche-lobe overflow.

Contribution

First detailed light curves and spectra of WASP 0131+28, providing precise measurements of the white dwarf's properties and confirming its evolutionary stage.

Findings

Secondary's parameters match helium-core white dwarf models

Mass and radius measurements with 1% and 0.6% accuracy

WASP 0131+28 is an EL CVn binary formed from Roche-lobe overflow

Abstract

We report the first $BV$ light curves and high-resolution spectra of the post-mass transfer binary star WASP 0131+28 to study the absolute properties of extremely low-mass white dwarfs. From the observed spectra, the double-lined radial velocities were derived, and the effective temperature and rotational velocity of the brighter, more massive primary were found to be $T_{\rm eff,1} = 10,000 \pm 200$ K and $v_1\sin$$i$ = 55 $\pm$ 10 km s$^{-1}$, respectively. The combined analysis of the {\it TESS} archive data and ours yielded the accurate fundamental parameters of the program target. The masses were derived to about 1.0 \% accuracy and the radii to 0.6 \%, or better. The secondary component's parameters of $M_2 = 0.200 \pm 0.002$ M$_\odot$, $R_2 = 0.528 \pm 0.003$ R$_\odot$, $T_{\rm eff,2}$ = 11,186 $\pm$ 235 K, and $L_2 = 3.9 \pm 0.3$ L$_\odot$ are in excellent agreement with the evolutionary sequence for a helium-core white dwarf of mass 0.203 M$_\odot$, and indicates that this star is halfway through the constant luminosity phase. The results presented in this article demonstrate that WASP 0131+28 is an EL CVn eclipsing binary in a thin disk, which is formed from the stable Roche-lobe overflow channel and composed of a main-sequence dwarf with a spectral type A0 and a pre-He white dwarf.