论文标题
他的白色矮人在黯然失色的二进制文件中。 iv。 WASP 1814+48具有多重脉动
The Pre-He White Dwarfs in Eclipsing Binaries. IV. WASP 1814+48 with Multiperiodic Pulsations
论文作者
论文摘要
对于El CVN候选人1SWASPJ181417.43+481117.0（WASP 1814+48），我们在2015年4月至3月之间获得了第一个光谱观察结果。使用棘轮光谱，用$ t _ {\ rm eff，1} = 7770 \ pm130 $ k和$ v_1 $ k和$ v_1 $$ \ sin $ sin $ i = 47 \ pm6 $ km s $ s $ s $ s $ s $ km^{ - 1} $测量了主要恒星的径向速度（RV）。我们同时安装了单线RV和Tess Light曲线。从二进制建模中，我们确定了每个组件的以下基本参数：$ m_1 = 1.659 \ pm0.048 $ $ $ $ $ $ m_ \ odot $，$ r_1 = 1.945 \ pm0.027 $ $ $ $ $ $ $ r_ \ odot $，以及$ l_1 = 12.35 \ pm0.35 \ pm0.90 $ $ l_ \ odoot+48 $ m_2 = 0.172 \ pm0.005 $ $ $ $ $ m_ \ odot $，$ r_2 = 0.194 \ pm0.005 $ $ $ $ $ r_ \ odot $，$ l_2 = 0.69 \ pm0.07 $ $ $ $ $ $ $ $ $ $ l_ \ odot $ for Wasp 1814+48+48 B. $ m_2 $和$ r_2 $与直接从可观察量直接计算的5.097 $ \ pm $ 0.025并发。 WASP 1814+48 b与0.176 m $ _ \ odot $ white dwarf（WD）进化模型相匹配，$ z = 0.01 $。金属性和我们的银河运动学表明该程序目标是薄盘恒星。分析了去除二元趋势后的整个光残差，并以52个频率振荡。其中，大多数低于24天以下的低频$^{ - 1} $是别名和轨道谐波。 32至36天$^{ - 1} $之间的五个重要频率是WASP 1814+48 a的脉动模式，位于ZAMS上的$δ$ SCT域，而高频为128 $ -288 DAY $^{ - 1} $的高频来自Pre-Pre-he wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd wd。我们的结果表明，WASP 1814+48是由$δ$ sct型初级和eLMV组成的第五颗EL CVN恒星（极低的质量pre-he wd变量）。
For the EL CVn candidate 1SWASPJ181417.43+481117.0 (WASP 1814+48), we secured the first spectroscopic observations between 2015 April and 2021 March. Using the echelle spectra, the radial velocities (RVs) of the primary star were measured with its atmospheric parameters of $T_{\rm eff,1}=7770\pm130$ K and $v_1$$\sin$$i=47\pm6$ km s$^{-1}$. We fitted our single-lined RVs and the TESS light curve simultaneously. From the binary modeling, we determined the following fundamental parameters for each component: $M_1=1.659\pm0.048$ $M_\odot$, $R_1=1.945\pm0.027$ $R_\odot$, and $L_1=12.35\pm0.90$ $L_\odot$ for WASP 1814+48 A, and $M_2=0.172\pm0.005$ $M_\odot$, $R_2=0.194\pm0.005$ $R_\odot$, and $L_2=0.69\pm0.07$ $L_\odot$ for WASP 1814+48 B. The surface gravity of $\log g_2=5.098\pm0.026$ obtained from $M_2$ and $R_2$ is concurrent with 5.097$\pm$0.025 computed directly from the observable quantities. WASP 1814+48 B is well-matched with the 0.176 M$_\odot$ white dwarf (WD) evolutionary model for $Z=0.01$. The metallicity and our Galactic kinematics indicate that the program target is a thin-disk star. The whole light residuals after removal of the binary trend were analyzed and found to oscillate at a total of 52 frequencies. Among these, most of the low frequencies below 24 day$^{-1}$ are aliases and orbital harmonics. The five significant frequencies between 32 and 36 day$^{-1}$ are the pulsation modes of WASP 1814+48 A located in the $δ$ Sct domain on ZAMS, and the high frequencies of 128$-$288 day$^{-1}$ arise from WASP 1814+48 B in the pre-He WD instability strip. Our results reveal that WASP 1814+48 is the fifth EL CVn star that is composed of a $δ$ Sct-type primary and a pre-ELMV (extremely low-mass pre-He WD variable).
