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arXiv 2005.10394astro-ph.SR
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双星系统中的前氦白矮星。I. WASP 0131+28

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

Jae Woo Lee, Jae-Rim Koo, Kyeongsoo Hong, Jang-Ho Park

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22 pages, including 7 figures and 6 tables
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摘要：

我们首次报道了质量转移后双星WASP 0131+28的$BV$光变曲线和高分辨率光谱，以研究极低质量白矮星的绝对性质。从观测到的光谱中，导出了双线径向速度，发现较亮、质量较大的主星的有效温度和自转速度分别为$T_{\rm eff,1} = 10,000 \pm 200$ K和$v_1\sin$ $i$ = 55 $\pm$ 10 km s $^{-1}$.结合{ \it TESS}存档数据和我们的分析，得出了计划目标的准确基本参数。质量的精确度约为1.0%，半径的精确度为0.6%或更好。次级成分的参数为$M_2 = 0.200 \pm 0.002$ M $_\odot$、$R_2 = 0.528 \pm 0.003$ R $_\odot$、$T_{\rm eff,2}$ = 11，186 $\pm$ 235 K、$L_2 = 3.9 \pm 0.3$ L $_\odot$，与质量为0.203 M $_\odot$的氦核白矮星的演化序列非常吻合，表明这颗恒星正处于恒光阶段的一半。结果表明，WASP 0131+28是一颗薄盘中的EL CVn食双星，它是由一颗光谱型为A0的主序星矮星和一颗前He白矮星组成，形成于稳定的Roche瓣溢出通道中。

英文摘要：

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.

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