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arXiv 0704.0280astro-ph
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通用信封进化版

Common Envelope Evolution Redux

Ronald F. Webbink

备注：
25 pages, 6 figures. To appear in "Short Period Binary Stars", ed. E.F. Milone, D.A. Leahy, & D.W. Hobill (Springer)
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摘要：

在动力学时间尺度的质量交换中，当一颗施主星的包层吞没了一颗密度更大的伴星，施主星的核心加上密度更大的伴星螺旋向内穿过这个耗散的包层时，就会形成共同的包层。正如Paczynski和Ostriker所设想的，这个过程一定是产生具有简并成分的短周期双星的原因，事实上，它已经被证明能够解释包含一个白矮星成分的短周期双星。然而，试图重建近距离双星白矮星的演化历史已被证明是更有问题的，并指出需要加强系统的质量损失，无论是在关闭的第一个，缓慢的插曲质量转移，产生了第一个白矮星，或在分离阶段之前的最后，共同的信封插曲。长周期相互作用的双星与大质量的白矮星，如经常性的新星T CrB和RS Oph的生存，也提出了简单的能量治疗共同的信封演变的解释困难。它们的存在意味着，主要条款是从通常的配方共同包络演变的能量预算失踪。最合理的缺失能量项是在共同包络中复合释放的能量，实际上，一个简单的重新表述明确包括复合的能量预算解决了这个问题。

英文摘要：

Common envelopes form in dynamical time scale mass exchange, when the envelope of a donor star engulfs a much denser companion, and the core of the donor plus the dense companion star spiral inward through this dissipative envelope. As conceived by Paczynski and Ostriker, this process must be responsible for the creation of short-period binaries with degenerate components, and, indeed, it has proven capable of accounting for short-period binaries containing one white dwarf component. However, attempts to reconstruct the evolutionary histories of close double white dwarfs have proven more problematic, and point to the need for enhanced systemic mass loss, either during the close of the first, slow episode of mass transfer that produced the first white dwarf, or during the detached phase preceding the final, common envelope episode. The survival of long-period interacting binaries with massive white dwarfs, such as the recurrent novae T CrB and RS Oph, also presents interpretative difficulties for simple energetic treatments of common envelope evolution. Their existence implies that major terms are missing from usual formulations of the energy budget for common envelope evolution. The most plausible missing energy term is the energy released by recombination in the common envelope, and, indeed, a simple reformulation the energy budget explicitly including recombination resolves this issue.

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