红色矩形的形成机制及其紫外光子源
The Red Rectangle: Its Shaping Mechanism and its Source of Ultraviolet Photons
摘要：
原行星状红色矩形星云由HD 44179提供动力，HD 44179是一个光谱双星（P = 318 d），其中一个明亮的后AGB成分是光度和当前质量损失的主要来源。在这里，我们提出了一个为期七年，八轨道的光谱监测计划的HD 44179，旨在揭示新的信息的莱曼/远紫外连续光谱系统的源，以及驱动机制的双极外流产生当前的星云。我们对上合轨道相位周围的H-α线轮廓的观测揭示了第二分量是快速（最大）的起源。v~560 $ km s$ ^{-1} $) bipolar outflow in the Red Rectangle. The variation of total H-alpha flux from the central H II region with orbital phase also identifies the secondary or its surroundings as the source of the far-ultraviolet ionizing radiation in the system. The estimated mass of the secondary (~0.94 M$ \sun $) and the speed of the outflow suggest that this component is a main sequence star and not a white dwarf, as previously suggested. We identify the source of the Lyman/far-ultraviolet continuum in the system as the hot, inner region (T$ _{max} \ge 17，000 $ K) of an accretion disk surrounding the secondary, fed by Roche lobe overflow from the post-AGB primary at a rate of about $ 2 - 5 \times 10^{-5} $ M$ \sun $ yr$ ^{-1} $. The total luminosity of the accretion disk around the secondary is estimated to be at least 300 L$ \sun $，约为整个系统光度的5%。（节略）
英文摘要：
The proto-planetary Red Rectangle nebula is powered by HD 44179, a spectroscopic binary (P = 318 d), in which a luminous post-AGB component is the primary source of both luminosity and current mass loss. Here, we present the results of a seven-year, eight-orbit spectroscopic monitoring program of HD 44179, designed to uncover new information about the source of the Lyman/far-ultraviolet continuum in the system as well as the driving mechanism for the bipolar outflow producing the current nebula. Our observations of the H-alpha line profile around the orbital phase of superior conjunction reveal the secondary component to be the origin of the fast (max. v~560$ km s$^{-1}$) bipolar outflow in the Red Rectangle. The variation of total H-alpha flux from the central H II region with orbital phase also identifies the secondary or its surroundings as the source of the far-ultraviolet ionizing radiation in the system. The estimated mass of the secondary (~0.94 M$\sun$) and the speed of the outflow suggest that this component is a main sequence star and not a white dwarf, as previously suggested. We identify the source of the Lyman/far-ultraviolet continuum in the system as the hot, inner region (T$_{max} \ge 17,000$ K) of an accretion disk surrounding the secondary, fed by Roche lobe overflow from the post-AGB primary at a rate of about $2 - 5\times10^{-5}$ M$\sun$ yr$^{-1}$. The total luminosity of the accretion disk around the secondary is estimated to be at least 300 L$\sun$, about 5% of the luminosity of the entire system. (abridged)
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