Near-Infrared Emission Lines of V723 Cassiopeiae (Nova Cassiopeiae 1995)
Near-Infrared Emission Lines of V723 Cassiopeiae (Nova Cassiopeiae 1995)
复制标题
V723 Cassiopeiae 的近红外发射线（Nova Cassiopeiae 1995）
DOI：
10.1086/340943
复制
发表时间：
2002
期刊：
影响因子：
--
通讯作者：
R. Puetter
中科院分区：
文献类型：
--
作者：
R. Rudy;C. Venturini;D. Lynch;S. Mazuk;R. Puetter
本文报道了非常慢的仙后座新星V723仙后座的近红外光谱(0.82.5μm)。其明亮、较窄的发射线(半高宽~500公里S-1)使其成为测定新星星云/日冕阶段的未知发射线波长的理想选择。我们给出了16个以前没有观察到或未识别的特征的波长，并通过寻找与已知原子跃迁的重合来搜索识别。对于候选跃迁，考虑母离子的可能丰度，然后寻找能够激发该特征的碰撞、荧光或复合过程。用这种方式识别了四条谱线，它们都是碰撞激发的、被禁止的跃迁。其中之一，[Tivii]λ22050，是一条新的日冕线，它直接去激发到基态。另外三条谱线与碰撞激发的低能级亚稳态Fe+5跃迁有关。在剩下的未识别特征中，有五条波长分别为8926、11110、11900、15545和20996？的特征在其他新星中被观测到。这些特征与[S VIII]λ9913冕线的时间发展对比表明，它们的母离子的激发态(<；280 eV)都比S+7低。
Near-infrared spectroscopy (0.8-2.5 μm) from two epochs is presented for the very slow nova V723 Cassiopeiae (=Nova Cassiopeiae 1995). Its bright, comparatively narrow emission lines (FWHM ~ 500 km s-1) make it ideal for determining wavelengths of unidentified emission lines that appear in the nebular/coronal stages of novae. We present wavelengths for 16 previously unobserved or unidentified features and search for identifications by looking for coincidences with known atomic transitions. For a candidate transition, the likely abundance of the parent ion is considered and then a collisional, fluorescent, or recombination process capable of exciting the feature is sought. Four of the lines are identified in this manner, all of them collisionally excited, forbidden transitions. One of these, [Ti VII] λ22050, is a new coronal line that de-excites directly to the ground state. Three other lines are associated with transitions from collisionally excited, low-lying, metastable levels of Fe+5. Of the remaining unidentified features, five, with wavelengths of 8926, 11110, 11900, 15545, and 20996 Å, have been observed in other novae. Comparing the time development of these features with the [S VIII] λ9913 coronal line indicates that all have parent ions of lower excitation (<280 eV) than S+7.