B3V恒星中弱金属发射线的光谱研究
A Spectroscopic Study of Weak Metallic Emission Lines in a B3V Star iota Her
摘要：
本文给出了一个在锐线B3 V星ι Her（HD 160762）中用高分辨率（R = 65000）和高SN（~1300）光谱数据观测到的弱发射线（WELs）列表。该列表涵盖了4900 A和10000 A之间的光谱区域。我们在这颗恒星中记录了207条WELS，并确定了190条谱线，包括10种离子（9种元素）。首次在正常B型星中发现了C II、N I、Cr II、Mn II和Ni II的发射线。17条发射谱线仍未确认。我们将我们的列表与已公布的3 Cen A的WEL列表（Wahlgren and Hubrig 2004）进行比较，发现检测到的发射线数量反映了这两颗恒星之间丰度的差异。我们在iota Her中检测到13条C I发射线（C正常），而在3 Cen A中仅发现一条C I发射线（C缺乏）。在3Cen A中检测到许多P II和Cu II的发射线（P和Cu都过量），而在iHer中没有发现这些离子的发射线。在iHer中，在6000 A的较短波长侧可以看到许多Fe II的发射线，而这些发射线在3Cen A中缺失。仔细检查3 Cen A的光谱数据显示，显然缺失的Fe II线出现在这颗恒星的吸收线。由于这两颗恒星有几乎相同的大气参数（Teff和log g），需要一个独立于这两个参数的物理解释来解释这一观测结果。
英文摘要：
We present a list of weak emission lines (WELs) observed in a sharp-lined B3 V star ι Her (HD 160762) using high resolution (R = 65000) and high SN (~1300) spectral data. The list covers a spectral region between 4900A and 10000A. We register 207 WELs in this star and identified 190 lines including ten ions (nine elements). Emission lines of C II, N I, Cr II, Mn II, and Ni II have been identified among normal B-type stars for the first time. 17 emission lines remain unidentified. We compare our list with the published list of WELs for 3 Cen A (Wahlgren and Hubrig 2004) and found that numbers of detected emission lines reflect differences in abundance between these two stars. We detect 13 C I emission lines in iota Her (normal in C), while only one C I emission line is found in 3 Cen A (deficient in C). Many emission lines of P II and Cu II have been detected in 3 Cen A (overabundant in both P and Cu), while no emission line of these ions has been found in ι Her. Many emission lines of Fe II are visible in the shorter wavelength side of 6000 A in iota Her, while these emission lines are missing in 3 Cen A. Close inspections of spectral data of 3 Cen A reveal that apparently missing Fe II lines appear as absorption lines in this star. Because these two stars have nearly the same atmospheric parameters (Teff and log g), a physical interpretation which is independent on these two parameters is needed to account for this observation.
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