论文标题
Novae＆Symbiotic Star的静脉相光谱的光离子化建模
Photoionization modelling of quiescence phase spectra of novae & symbiotic star
论文作者
论文摘要
我们在光学区域中使用观察到的光谱和发表光谱的结果呈现了研究结果，在其静止阶段和共生星（BX MON）中，很少有Novae（T Crb，Gk Per，RS OPH，V3890 SGR和V745 SCO）。使用2M喜马拉雅望远镜（HCT）可用的设施进行观察。通常，由于凉爽的二级成分，光谱显示出明显的低电离发射特征以及由于凉爽的二级成分而引起的TIO吸收特征。 T CRB和GK每张显示较高的电离线。我们使用光电代码云量来对这些光谱进行建模。从最佳拟合模型中，我们估计了物理参数，例如温度，光度和氢密度；与系统相关的估计元素丰度和其他参数。通过将各种巨头的光谱与吸收特征相匹配，并且从最佳拟合中匹配，我们确定了次生的类型及其对光谱的贡献。
We present results of study, using observed and published spectra in optical region, of few novae (T CrB, GK Per, RS Oph, V3890 Sgr and V745 Sco) in their quiescence phase and a symbiotic star (BX Mon). Observations were made using the facilities available at 2m Himalayan Chandra Telescope (HCT). Generally, the spectra show prominent low ionization emission features of hydrogen, helium, iron and oxygen and TiO absorption features due to the cool secondary component; T CrB and GK Per show higher ionization lines. We used photoionization code CLOUDY to model these spectra. From the best-fit models, we have estimated the physical parameters, e.g., temperature, luminosity & hydrogen density; estimated elemental abundances and other parameters related to the system. By matching the spectra of various giants with the absorption features and from the best-fit, we determined the type of secondaries and also their contribution to the spectra.
