The peculiar infrared temporal development of Nova Vulpeculae 1987 (QV Vulpeculae)
The peculiar infrared temporal development of Nova Vulpeculae 1987 (QV Vulpeculae)
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DOI：
10.1086/172029
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发表时间：
1992-12
期刊：
影响因子：
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通讯作者：
R. Gehrz;T. Jones;C. Woodward;M. Greenhouse;R. Wagner;T. Harrison;T. Hayward;J. Benson
中科院分区：
文献类型：
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作者：
R. Gehrz;T. Jones;C. Woodward;M. Greenhouse;R. Wagner;T. Harrison;T. Hayward;J. Benson
该论文报告了 Nova QV Vul（1987）从 1987 年 11 月到 1989 年 9 月的 1.25-19.5 微米红外光度测量和光学/红外光谱。测量结果表明，在爆发后 83 天内形成了光学厚的碳尘埃壳，并且在爆发后的 2 年时间内，四种类型的天体物理颗粒的光谱特征出现在不同的时间。首先形成碳、SiC和碳氢化合物；随后形成富氧硅酸盐。这表明碳尘成分在快速移动的极地水槽中形成，而硅酸盐在缓慢移动的赤道环中形成。红外光度测定和光谱学的质量估计证实，QV Vul 的慢速和快速喷射物中的颗粒凝结与之前对其他尘埃新星的观测所建立的约束一致。结论是这些颗粒中的可凝结元素的丰度大约是太阳的丰度。
The paper reports 1.25-19.5-micron IR photometry and optical/IR spectroscopy of Nova QV Vul (1987) from November 1987 through September 1989. The measurements show that an optically thick carbon dust shell formed within 83 d of the outburst, and that the spectral signatures of four types of astrophysical grains appeared at various times during a 2-yr period following the eruption. Carbon, SiC, and hydrocarbons formed first; oxygen-rich silicates formed later. It is suggested that the carbon dust components formed in fast-moving polar flumes, and that the silicates formed in a slow-moving equatorial ring. Mass estimates from the IR photometry and optical spectroscopy confirm that grain condensation in both the slow and fast ejecta of QV Vul is consistent with constraints established by previous observations of other dusty novae. It is concluded that the condensible elements in these grains were present in approximately solar abundance.