矮新星KZ Gem的后续地面观测
Followup ground-based observations of the dwarf nova KZ Gem
摘要：
我们目前的光谱恒星在附近的矮新星（DN）KZ宝石，以确认其身份，这在文献中一直模棱两可。对2014年至2019年的73个径向速度的分析提供了高精度的轨道周期0.2224628（2）\，d（$\sim5.34$ \，hr），并显示KZ\，Gem是双线DN。从2016年到2018年拍摄的时间序列测光显示了可变双峰调制，全振幅为$\sim0.3$ \，mag，以及持续$\sim30$ \，min或更长时间的五个类高斯瞬态事件。利用光变曲线程序XRBinary和非线性拟合程序NMfit，从时间序列测光中得到了矮新星（DN）KZ Gem的优化双星模型，它由一颗质量转移速率为$2.7\,-\,7.9\times10^{-10}\,{\rm M}_{\odot}\,{\rm yr}^{-1}$的充满Roche瓣的K型矮星到一颗围绕着白矮星的大的、冷的、厚的盘组成，其轨道倾角为$51^{\circ}.6(\pm1^{\circ}.4)$ .两个热点上的磁盘被证明是造成所观察到的变化，从第二颗恒星的椭球调制。这个物理模型与KZ，Gem的Gaia距离是相容的。
英文摘要：
We present spectroscopy of stars in the immediate vicinity of the dwarf nova (DN) KZ Gem to confirm its identification, which had been ambiguous in the literature. Analysis of 73 radial velocities spanning from 2014 to 2019 provides a high-precision orbital period of 0.2224628(2)\,d ($\sim5.34$\,hr) and shows KZ\,Gem to be a double-lined DN. Time series photometry taken from 2016 to 2018 shows a variable double-hump modulation with a full amplitude of $\sim0.3$\,mag, along with five Gaussian-like transient events lasting $\sim30$\,min or more. Using the light curve code XRBinary and nonlinear fitting code NMfit, we obtain an optimized binary model of the dwarf nova (DN) KZ Gem, from time series photometry, consisting of a Roche-lobe-filling K type dwarf with a mass transfer rate of $2.7\,-\,7.9\times10^{-10}\,{\rm M}_{\odot}\,{\rm yr}^{-1}$ to a large, cool and thick disk surrounding a white dwarf, in an orbit with an inclination of $51^{\circ}.6(\pm1^{\circ}.4)$. Two hotspots on the disk are demonstrated to cause the observed variations in the ellipsoidal modulations from the secondary star. This physical model is compatible with the Gaia distance of KZ\,Gem.
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