论文标题
MN112的建模光谱
Modeling spectra of MN112
论文作者
论文摘要
MN112是带有星际星云的银河发光蓝色变量（LBV）。 P Cygni是第一个发现的LBV，是在17世纪重大爆发期间记录的。恒星具有类似的光谱，具有较强的发射氢系，He I，N II，Si II和Fe III系。我们介绍了MN112光谱的光谱分析和建模的结果。我们获得了MN112的主要恒星参数和化学丰度，并将其与P Cygni的化学物质进行了比较。使用非LTE辐射转移代码CMFGEN计算大气模型。我们已经使用了在Apache Point天文台观测值的3.5 m望远镜和3.5 m ARC望远镜的MN112光谱。使用6-M BTA望远镜拍摄P Cygni光谱。我们已经在温度下发现了与模型在温度下观察到的频谱中最合适的频谱m _ {\ odot} \ text {yr}^{ - 1} $，填充因子$ f = 0.1 $，光度$ l = 5.77 \ times 10^5 \，l _ {\ odot} $用于mn112。氦与氢HE/ H的比率为0.37（原子数），氮过多（$ x_ \ text {n}/ x _ {\ odot} = 6.8 $）和碳（$ x_ \ x_ \ text {c}/ x _ _ _ {\ odot} <0.1 $）的比率。
MN112 is the Galactic luminous blue variable (LBV) candidate with circumstellar nebula. P Cygni is the first discovered LBV, which was recorded during major eruptions in the 17th century. The stars have similar spectra with strong emission hydrogen lines, He I, N II, Si II, and Fe III lines. We present results of the spectroscopic analysis and modeling of MN112 spectra. We obtained main stellar parameters and chemical abundances of MN112 and compared them with those of P Cygni. Atmosphere models were calculated using non-LTE radiative transfer code CMFGEN. We have used spectra of MN112 obtained with the 3.5-m telescope at the Observatory of Calar Alto and 3.5-m ARC telescope at the Apache Point Observatory. P Cygni spectra were taken with the 6-m BTA telescope. We have found the best-fit of the observed spectrum with the model at temperature $T_{\text{eff}}= 15\,200$K, clumping-corrected mass-loss rate $\dot{M}f^{-0.5}=5.74 \times 10^{-5}\, M_{\odot}\text{yr}^{-1}$, filling-factor $f=0.1$, luminosity $L=5.77 \times 10^5\, L_{\odot}$ for MN112. The ratio of helium to hydrogen He/H is 0.37 (by the number of atoms) with nitrogen overabundance ($X_\text{N}/ X_{\odot} = 6.8$) and the underabundance of carbon ($X_\text{C}/ X_{\odot} < 0.1$).
