双星的绝热质量损失- I。计算方法
Adiabatic Mass Loss in Binary Stars - I. Computational Method
摘要：
相互作用双星系统中的施主星对快速质量损失的渐近响应的特征是整个内部的绝热膨胀。在这个极限下，恒星内部的能量产生和热流可以忽略不计。我们通过构建模型序列来模拟这种响应，首先是在其演化过程中的任意点填充其罗氏瓣的供体星，保持其特定的熵和成分分布固定，因为质量从表面移除。恒星内部保持流体静力平衡。在这些绝热模型中的光度分布的质量损失的恒星可以重建的特定的熵轮廓和它们的梯度。这些近似值通过与时间相关的二元传质计算的比较进行了验证。我们描述了如何绝热质量损失序列可以用来量化阈值条件的动态时间尺度的质量转移，并建立范围内的后共同信封二进制的允许大力。
英文摘要：
The asymptotic response of donor stars in interacting binary systems to very rapid mass loss is characterized by adiabatic expansion throughout their interiors. In this limit, energy generation and heat flow through the stellar interior can be neglected. We model this response by constructing model sequences, beginning with a donor star filling its Roche lobe at an arbitrary point in its evolution, holding its specific entropy and composition profiles fixed as mass is removed from the surface. The stellar interior remains in hydrostatic equilibrium. Luminosity profiles in these adiabatic models of mass-losing stars can be reconstructed from the specific entropy profiles and their gradients. These approximations are validated by comparison with time-dependent binary mass transfer calculations. We describe how adiabatic mass loss sequences can be used to quantify threshold conditions for dynamical time scale mass transfer, and to establish the range of post-common envelope binaries that are allowed energetically.
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