论文标题
$β$ ly的光学薄室内媒介系统
Optically thin circumstellar medium in $β$ Lyr A system
论文作者
论文摘要
Beta Lyl A是一个复杂的二进制系统，具有广泛的观测数据集：光曲线（从FUV到FIR），干涉平方可见性，闭合相，三乘积测量值，光谱 - 能源分布（SED），高分辨率光谱谱图，差异可见性幅度幅度差异以及相差相。特别是，我们使用从2013年至2015年的Ondrejov 2M望远镜的光谱来衡量HALPHA，HEI，SIII，NEI或CII线的发射以及Chara/Vega在2013年与Chara/Vega的差异干扰测量，从2013年活动中，我们不仅可以衡量ACCREGTION的范围，不仅可以衡量ACCREGTION的尺寸。磁盘），但还具有光学薄的物体（磁盘气氛，喷气机，外壳）。我们扩展了建模工具PyshellSpec（基于ShellSpec； 1D LTE辐射传输代码），包括所有新的可观察物，以计算差异性可见性/相位，以执行多普勒断层扫描，并确定关节CHI^2公制。在优化了38个自由参数之后，我们得出了beta lyra系统的强大模型。根据该模型，发射是在磁盘的扩展大气中形成的，两个垂直喷气机在〜700 km s^-1处膨胀，而半径〜70 r_s的对称壳。光谱法表明碳的丰度低，即太阳值的10^-2。我们还量化了数据集之间的系统差异，并讨论具有更高分辨率，其他不对称或富裕度的替代模型。
beta Lyr A is a complex binary system with an extensive observational dataset: light curves (from FUV to FIR), interferometric squared visibility, closure phase, triple product measurements, spectral-energy distribution (SED), high-resolution spectroscopy, differential visibility amplitude, and also differential phase. In particular, we use spectra from Ondrejov 2m telescope from 2013 to 2015, to measure the emission in Halpha, HeI, SiII, NeI, or CII lines, and differential interferometry by CHARA/VEGA from the 2013 campaign to measure wavelength-dependent sizes across Halpha and HeI 6678. This allows us to constrain not only optically thick objects (primary, secondary, accretion disk), but also optically thin objects (disk atmosphere, jets, shell). We extended our modelling tool Pyshellspec (based on Shellspec; a 1D LTE radiative transfer code) to include all new observables, to compute differential visibilities/phases, to perform a Doppler tomography, and to determine a joint chi^2 metric. After an optimisation of 38 free parameters, we derive a robust model of the beta Lyr A system. According to the model, the emission is formed in an extended atmosphere of the disk, two perpendicular jets expanding at ~700 km s^-1, and a symmetric shell with the radius ~70 R_S. The spectroscopy indicates a low abundance of carbon, 10^-2 of the solar value. We also quantify systematic differences between datasets and discuss alternative models, with higher resolution, additional asymmetries, or He-rich abundance.
