论文标题
RS OPH的2021年爆发：光谱进化的图画图集。 ii。从第19天到102（太阳能连接）
The 2021 outburst of RS Oph: a pictorial atlas of the spectroscopic evolution. II. From day 19 to 102 (solar conjunction)
论文作者
论文摘要
我们介绍了2021年Nova爆发期间RS OPH光谱演变的高分辨率梯队的第二部分（第19至102天）。可以得出的一些快速结论是：（1）光谱演化已经顺利进行，这表明弹射器通过预先存在的RG风的扩展以及中心源的光电发量都没有遇到突然的不连续性，然后再关闭核燃烧。 （2）2021光谱演化与2006年喷发相似，带有三峰线曲线的镜面表现（2006年的蓝色峰值比红色明亮，在2021年相反）； （3）三峰轮廓的演变通过不同的激发和电离度相似，这表明嵌套到赤道的双极流出中的起源； （4）冠状发射线的时间行为看起来都很平滑，无论是在辐射通量和三峰轮廓的演变方面，其高原的最大持续时间可持续到大约87天； (5) there seems to exist within RS Oph two distinct types of ejecta: one fast moving and producing Gaussian-like line profiles (primarely [NII] and [OIII]), that keep expanding at FWHM=1000 km/s with no sign of ongoing deceleration during the two months leading up to Solar conjunction, and slower moving ejecta giving rise to the triple-peaked line profiles (HeI, HeII,冠状线，以及后来的Balmer线），在太阳连接时，蓝色和红色峰的速度分离仍在缩小，当时平均达到330 km/s时； （6）由于中性氢的拉曼散射OVI 1032，在6825 ANG处的“共生带”与冠状线同时出现：它的存在表明，在冠状线发育过程中，red巨人风中很大的一部分仍然保持中立。
We present the second part (days 19 to 102) of our high-resolution Echelle atlas of the spectral evolution of RS Oph during the 2021 nova outburst. Some quick conclusions that can be drawn are: (1) the spectra evolution has progressed smoothly, suggesting that both the expansion of the ejecta through the pre-existing RG wind and the photo-ionization from the central source did not encountered sudden discontinuities prior to switch-off of the nuclear burning; (2) the 2021 spectral evolution is similar to that of the 2006 eruption, with a mirror-appearance of the triple-peaked line profiles (blue peak brighter than red in 2006, the opposite in 2021); (3) the evolution of the triple-peaked profiles progressed similarly through different excitation and ionization degrees, suggesting an origin in a bipolar outflow nested to an equatorial torus; (4) the time-behavior of coronal emission lines appears quite smooth, both in terms of radiated flux as well as evolution of the triple-peaked profiles, with a plateau at maximum lasting up to about day 87; (5) there seems to exist within RS Oph two distinct types of ejecta: one fast moving and producing Gaussian-like line profiles (primarely [NII] and [OIII]), that keep expanding at FWHM=1000 km/s with no sign of ongoing deceleration during the two months leading up to Solar conjunction, and slower moving ejecta giving rise to the triple-peaked line profiles (HeI, HeII, coronal lines, and also Balmer lines at later times), for which the separation in velocity of blue and red peaks is still shrinking at the time of Solar conjunction when it reaches an average of 330 km/s; (6) the "symbiotic band" at 6825 Ang, due to Raman scattering of OVI 1032 by neutral hydrogen, appears simultaneously with the coronal lines: its very presence indicates that a sizeable part of the wind of the red giant has remained neutral during the development of coronal lines.
