Interstellar absorption lines toward gamma Arae
Interstellar absorption lines toward gamma Arae
复制标题
朝向伽马Arae的星际吸收线
DOI：
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发表时间：
1975
期刊：
影响因子：
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通讯作者：
E. Hu
中科院分区：
文献类型：
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作者：
D. Morton;E. Hu
本文分析了γ Ara（E/sub B//sub -//sub V/=0.08）星际吸收谱线的地面观测数据和哥白尼望远镜观测数据，给出了H、C、N、O、Na、Mg、Si、P、S、Ar、Ca、Mn和Fe各离子级的柱密度。相对于H核在H i区域的元素丰度是类似的zeta OPH值，与相对于太阳的损耗往往会随着冷凝温度的增加而增加。例如，对于$gamma$ Ara，Fe的消耗系数为50; Mg、Si和Mn的消耗系数约为10;而S、P和N的消耗系数很小或没有。星际Si iv和可能的S iv看起来比大多数其他恒星更强，但它们与Si iii和S iii的比率仍然很低，这表明软X射线和低能宇宙射线不是电离的重要来源。Ovi线的宽度和Nv的缺失被解释为一个温度在3 ~ 7 × 10$sup 5$ K之间的碰撞电离区的证据，该区域包含至少4 × 10$sup-4 $的总星际柱密度。（AIP）
The available data on interstellar absorption lines in the spectrum of $gamma$ Ara (E/subB//sub -//subV/=0.08) observed from the ground and with the Copernicus telescope have been analyzed to give column densities of various ion stages of H, C, N, O, Na, Mg, Si, P, S, Ar, Ca, Mn, and Fe. The element abundances with respect to H nuclei in H i regions are similar to the values for zeta Oph, with depletions relative to the Sun tending to increase with increasing condensation temperature. For example, toward $gamma$ Ara Fe is depleted by a factor of 50; Mg, Si, and Mn by about 10; and S, P, and N little or none. Interstellar Si iv and probably S iv appear stronger than in most other stars, but still their low ratios to Si iii and S iii suggest that soft X-rays and low- energy cosmic rays are not important sources of ionization. The width of the O vi lines and the absence of N v have been interpreted as evidence for a collisionally ionized region with a temperature between 3 and 7x10$sup 5$ K containing at least 4x10$sup -4$ of the total interstellar column density. (AIP)