论文标题
Hubble太空望远镜STIS光谱1891年
Hubble Space Telescope STIS Spectroscopy of Nova T Aurigae 1891
论文作者
论文摘要
T aurigae是一个黯然失色的旧新星，在1891年爆炸。在Gaia Edr3距离为815-871 PC的距离时，它是一个相对附近的旧Nova。通过紫外光谱建模并使用新的精确的Gaia距离，我们发现t aurigae的HST/stis光谱与带有质量转移率$ \ dot $ \ dot {m} $ $ 10^{ - 8} m _ 8} m _ {\ odot} $/yr的增值{m} $一致。 0.7 \ pm 0.2 m _ {\ odot} $，$ i \ sim 60^{\ circ} $的倾斜度，GAIA的距离为$ 840 _ { - 25}^{+31} $ 〜p。金属的急剧吸收线不能在磁盘中形成，并且很可能在磁盘上方的材料（例如，圆盘溢出），圆形材料和/或与1891年Nova爆炸中弹出的壳相关的材料中形成。饱和的氢$α$吸收特征归因于$ 10^{21} $ cm $^{ - 2} $的大型星际中氢柱密度，归因于t aur，并证实了其红色$ e（b-v）= 0.42 \ pm pm 0.08 $。
T Aurigae is an eclipsing old nova which exploded in 1891. At a Gaia EDR3 distance of 815-871 pc, it is a relatively nearby old nova. Through ultraviolet spectral modeling and using the new precise Gaia distance, we find that the HST/STIS spectrum of T Aurigae is consistent with an accretion disk with a mass transfer rate $\dot{M}$ of the order of $10^{-8}M_{\odot}$/yr, for a white dwarf mass of $M_{\rm wd} \approx 0.7 \pm 0.2 M_{\odot}$, an inclination of $i \sim 60^{\circ}$, and a Gaia distance of of $840_{-25}^{+31}$~pc. The sharp absorption lines of metals cannot form in the disk and are likely forming in material above the disk (e.g. due stream disk overflow), in circumbinary material, and/or in material associated with the ejected shell from the 1891 nova explosion. The saturated hydrogen Ly$α$ absorption feature is attributed to a large interstellar medium hydrogen column density of the order of $10^{21}$cm$^{-2}$ towards T Aur, as corroborated by the value of its reddening $E(B-V)=0.42 \pm 0.08$.
