极地V348 Pav的光学观测和独眼巨人激波后区域模拟
Optical observations and cyclops post-shock region modelling of the polar V348 Pav
摘要：
极区激变变星的激波后区域（PSR）产生了它们的大部分光度，并产生了光学波长的高圆偏振和白矮星旋转周期的强烈变化，这是这些系统的显着特征。为了研究极候选者V348 Pav，我们获得了一个全面的观测数据集，包括光度，偏振和光谱数据，用于约束系统的冲击后性质。该物体呈现出高圆偏振（$\sim30$ %）和高He II 4686 A与H $~β$线比，证实它是一个极性。从径向速度和光变曲线，我们确定的轨道周期为79.98~min，接近CV的轨道周期最小值。H $~β$径向速度曲线的半振幅为$141.4\pm1.5$ km s $^{-1}$。多普勒层析成像表明，该系统的谱线发射的大部分起源于该地区的伴星面临的WD，可能是由有关的PSR辐射。我们使用Cyclops代码对PSR进行建模。PSR的密度和温度分布，通过适当的解决方案的水热动力学方程，得到的，被用于三维辐射传输的解决方案，考虑到系统的几何形状。我们可以用一个WD磁场为$\sim28$ MG、WD质量为$\sim0.85$ ~M $_{\odot}$和低轨道倾角（$\sim25^{\circ}$）的模型重现V348 Pav \textit{B, V, R}和\textit{I}的光度和偏振数据。WD质量和轨道倾角的这些值与测量的径向速度一致。
英文摘要：
Post-shock regions (PSR) of polar cataclysmic variables produce most of their luminosity and give rise to high circular polarization in optical wavelengths and strong variability on the white dwarf rotation period, which are distinctive features of these systems. To investigate the polar candidate V348 Pav, we obtained a comprehensive observational set including photometric, polarimetric, and spectroscopic data, which was used to constrain the post-shock properties of the system. The object presents high circular polarization ($\sim30$ per cent) and high He II 4686A to H$~β$ line ratio, confirming it is a polar. From both radial velocities and light curves, we determined an orbital period of 79.98~min, close to the orbital period minimum of CVs. The H$~β$ radial velocity curve has a semi-amplitude of $141.4\pm1.5$ km s$^{-1}$. Doppler tomography showed that most of the spectral line emission in this system is originated in the region of the companion star facing the WD, possibly irradiated by the emission related to the PSR. We modelled the PSR using the Cyclops code. The PSR density and temperature profiles, obtained by a proper solution of the hydro-thermodynamic equations, were used in a 3D radiative transfer solution that takes into account the system geometry. We could reproduce the V348 Pav \textit{B, V, R}, and \textit{I} photometric and polarimetric data using a model with a WD magnetic field of $\sim28$ MG, a WD mass of $\sim0.85$~M$_{\odot}$ and a low ($\sim25^{\circ}$) orbital inclination. These values for the WD mass and orbital inclination are consistent with the measured radial velocities.
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