arXiv 1007.09322010-07-06astro-ph.SR

老新星HR Del的长期分光光度研究

A long term spectroscopic and photometric study of the old nova HR Del

M. Friedjung, M. Dennefeld, I. Voloshina

备注：: 12 pages, 15 figures, accepted for publication in Astronomy & Astrophysics
DOI：: 10.1051/0004-6361/200913936

摘要：

1967年发现的Nova HR Del在IUE卫星的整个寿命期间（1996年结束）在光学和紫外线方面都非常明亮，今天似乎仍然非常明亮。这种持续活动的原因尚不清楚;可能涉及持续的弱热核燃烧。因此，在几年内，在H $α$光谱区域的宽带光度法和光谱法中监测HR Del。H $α$线的轮廓显示了两个组成部分：一个狭窄的中央部分和较宽的翅膀。前者最容易理解为是由于一个吸积盘，其几何形状可能导致它部分地遮蔽自己。该分量显示出类似于具有轨道相位依赖性的S波，这表明它可能是由于H $α$中的亮点。宽的成分一定来自另一个区域，其中可能有1967年爆发期间喷出的物质的不可忽视的贡献。H $α$等效宽度的非轨道变化被发现在长和短的时间尺度。在光度学中也发现了类似的变化，显示出一个组分与轨道相位有明显的依赖性，但与H $α$变化没有明显的关系。光度变化的轨道部分可以用伴星的辐射来解释，而H $α$的性质可以用吸积盘和H $α$中的亮点来解释。

英文摘要：

The Nova HR Del, discovered in 1967, was found to be exceptionally bright in the optical and UV during the whole lifetime of the IUE satellite (ending in 1996) and appears to be still extremely luminous today. The reason for this continuing activity is not clear; continuing weak thermonuclear burning might be involved. HR Del was thus monitored over several years, both in broad band photometry and spectroscopically in the H$α$ spectral region. The profile of the H$α$ line shows two components: a narrow, central component; and broader wings. The former is most easily understood as being due to an accretion disk, whose geometry might lead to it partly occulting itself. That component shows something like an S wave with an orbital phase dependance, suggesting that it could be due to a spot bright in H$α$. The wide component must come from another region, with a probably non-negligible contribution from the material ejected during the 1967 outburst. Non-orbital variations of the H$α$ equivalent width were found both on long and short time scales. Similar variations were found in the photometry, showing a component with a clear dependence on the orbital phase, but no obvious relation with the H$α$ variations. The orbital part of the photometric variations can be explained by irradiation of the companion, while the properties of H$α$ are explicable by the presence of an accretion disk and a spot bright in H$α$.

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