标题： V583 天琴座的光度学和光谱分析：一颗具有 g 模振荡初级和吸积盘的天鹰座β型变星 显示英文标题

标题： Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk

摘要： V583 天琴座是一颗轨道周期为 11.2580 天的极低质量比大陵型食双星。我们从新观测的光谱中确定了有效温度 T_{eff1} = 9000 \pm 350 K，由于质量转移可能被低估。基于次级星充满洛希瓣且同步旋转的假设，得到质量比 q = 0.1 \pm 0.004 和轨道倾角 i = 85.5{\deg }。 径向速度曲线由时间序列光谱获得，这使得能够更精确地估算恒星质量和半径：M1 = 3.56 \pm 0.5 Msun，R1 = 2.4 \pm 0.2 Rsun；以及 M2 = 0.36 \pm 0.02 Msun，R2= 6.9 \pm 0.4 Rsun。 双峰H_{\alpha }发射的变化表明质量转移期间形成了一个稳定的盘。 根据使用O-C周期分析估计的质量转移，V583 Lyr似乎是一个后质量反转系统。 它的轨道周期正在缓慢增加，由此估算出主星的质量吸积率为 dM1/dt = 3.384 \times 10^{-8} Msun/yr。 脉动分析是在光曲线的残差上进行的。 主星被发现是一颗g模脉动星，在低于9 d^{-1}的频率中共提取出26个频率。 详细研究了g模的频率分组和旋转分裂特性。 本研究为围绕g模脉动主星的吸积盘提供了有力的证据。 显示英文摘要

摘要： V583 Lyr is an extremely low mass ratio Algol-type binary with an orbital period of 11.2580 days. We determined an effective temperature of T_{eff1} = 9000 \pm 350 K from newly observed spectra, which might be an underestimate due to binary mass transfer. The binary mass ratio q = 0.1 \pm 0.004 and the orbital inclination i = 85.5{\deg} are determined based on the assumption that the secondary fills its Roche lobe and rotates synchronously. The radial velocity curve is obtained from time series spectra, allowing for improved estimation of stellar masses and radii: M1 = 3.56 \pm 0.5 Msun, R1 = 2.4 \pm 0.2 Rsun; and M2 = 0.36 \pm 0.02 Msun, R2= 6.9 \pm 0.4 Rsun. The variations in the double-peaked H_{\alpha} emission indicate the formation of a stable disk during mass transfer. V583 Lyr appears to be a post-mass-reversal system, according to the estimated mass transfer using O-C period analysis. Its orbital period is slowly increasing, from which the rate of mass accretion by the primary star is estimated to be dM1/dt = 3.384 \times10^{-8} Msun/yr. The pulsation analysis was conducted on the residuals of the light curve. The primary component was found to be a g-mode pulsating star with 26 frequencies extracted lower than 9 d^{-1}. The frequency groups and rotational splitting properties of the g-mode were studied in detail. This study provides compelling evidence for an accretion disk surrounding the g-mode pulsating primary.