Formation of Millisecond Pulsars with Heavy White Dwarf Companions: Extreme Mass Transfer on Subthermal Timescales
Formation of Millisecond Pulsars with Heavy White Dwarf Companions: Extreme Mass Transfer on Subthermal Timescales
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DOI：
10.1086/312496
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发表时间：
2000-01
期刊：
影响因子：
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通讯作者：
T. Tauris;E. V. D. van den Heuvel;G. Savonije
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文献类型：
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作者：
T. Tauris;E. V. D. van den Heuvel;G. Savonije
我们对具有中等质量 (2.0-6.0 M☉) 供体星和 1.3 M☉ 吸积中子星的近 X 射线双星系统的非保守演化进行了详细的数值计算。我们计算了供体星对质量损失的热响应，以确定其稳定性并跟踪质量传递的演变。在“各向同性再发射模型”的假设下，我们证明，在许多情况下，如果供体星的对流包层不是太深，双星有可能在亚热时间尺度上阻止螺旋进入并在高度超爱丁顿传质阶段（1≪Ṁ/ṀEdd < 105）中幸存下来。因此，这些系统为具有重CO白矮星和相对较短轨道周期（3-50天）的二元毫秒脉冲星提供了新的形成通道。然而，我们得出的结论是，要在约 1 天的时间内产生 O-Ne-Mg 白矮星或 Porb（例如 PSR B0655+64）的双脉冲星（例如，PSR B0655+64），上述场景是行不通的，并且螺旋阶段仍然被认为是形成此类系统的最可能的场景。
We have performed detailed numerical calculations of the nonconservative evolution of close X-ray binary systems with intermediate-mass (2.0-6.0 M☉) donor stars and a 1.3 M☉ accreting neutron star. We calculated the thermal response of the donor star to mass loss in order to determine its stability and follow the evolution of the mass transfer. Under the assumption of the "isotropic reemission model," we demonstrate that in many cases it is possible for the binary to prevent a spiral-in and survive a highly super-Eddington mass transfer phase (1 ≪ Ṁ/ṀEdd < 105) on a subthermal timescale if the convective envelope of the donor star is not too deep. These systems thus provide a new formation channel for binary millisecond pulsars with heavy CO white dwarfs and relatively short orbital periods (3-50 days). However, we conclude that to produce a binary pulsar with a O-Ne-Mg white dwarf or Porb ~ 1 day (e.g., PSR B0655+64) the above scenario does not work, and a spiral-in phase is still considered the most plausible scenario for the formation of such a system.