具有偏心轨道的相互作用双星II。非保守质量转移引起的长期轨道演化
Interacting Binaries with Eccentric Orbits II. Secular Orbital Evolution Due To Non-Conservative Mass Transfer
摘要：
我们调查的长期演变的轨道半长轴和偏心率，由于在偏心双星的质量转移，允许从系统的质量和角动量损失。采用δ函数描述双星轨道近星点的质量转移率，发现质量转移开始时双星的初始性质决定了轨道半长轴和偏心率的增加或减小，其速率与近星点质量转移率的大小成线性关系.导致轨道半长轴和偏心率增加的初始双星质量比和偏心率的范围随着系统质量损失程度的增加而变宽，随着双星轨道角动量损失的增加而变窄。与潮汐演化时间尺度的比较表明，通常的假设快速循环在偏心双星的质量转移的发病是不合理的，无论系统的质量和角动量损失的程度。这项工作扩展了我们之前关于偏心双星中保守质量传递的结果，并且可以纳入双星进化和种群合成代码中来模拟偏心双星中的非保守质量传递。
英文摘要：
We investigate the secular evolution of the orbital semi-major axis and eccentricity due to mass transfer in eccentric binaries, allowing for both mass and angular momentum loss from the system. Adopting a delta function mass transfer rate at the periastron of the binary orbit, we find that, depending on the initial binary properties at the onset of mass transfer, the orbital semi-major axis and eccentricity can either increase or decrease at a rate linearly proportional to the magnitude of the mass transfer rate at periastron. The range of initial binary mass ratios and eccentricities that leads to increasing orbital semi-major axes and eccentricities broadens with increasing degrees of mass loss from the system and narrows with increasing orbital angular momentum loss from the binary. Comparison with tidal evolution timescales shows that the usual assumption of rapid circularization at the onset of mass transfer in eccentric binaries is not justified, irrespective of the degree of systemic mass and angular momentum loss. This work extends our previous results for conservative mass transfer in eccentric binaries and can be incorporated into binary evolution and population synthesis codes to model non-conservative mass transfer in eccentric binaries.
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