双星的绝热质量损失。IV.低质量和中等质量氦双星

Lifu Zhang, Hongwei Ge, Xuefei Chen, Zhanwen Han
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引用次数: 0

摘要

双星系统中不稳定的质量转移情况会逐渐导致供体星的绝热膨胀,并最终导致共同包层阶段。一旦氦供体恒星填满其罗氏环,这一过程就可能发生在氦双星系统中。我们计算了裸氦星的绝热质量损失模型,其质量范围为0.35 M⊙-10 M⊙,每个质量序列都从氦-零年龄主序列演化到白矮星或碳点燃的冷却轨道。考虑到恒星风的影响,本文不考虑大质量氦星。在保守质量转移的假设下,比较恒星半径和罗氏环的演化,我们给出了临界质量比qcrit = MHe/Maccretor作为中低质量氦双星的双星稳定性标准。在氦主序上,结果显示1.0 < qcrit < 2.6,比多向性模型qcrit = 3的经典结果更不稳定。在早期氦赫兹普隆缺口之后,qcrit迅速增大,甚至超过了10(与广泛使用的qcrit = 4的结果相比更加稳定),这主要是由于辐射包层的膨胀。我们的结果可能对这些快速质量转移双星系统(如AM CVns、超紧凑X射线双星和氦新星)很有帮助,它可以指导双星群体合成,以形成Ia型超新星和引力波源等特殊天体。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Adiabatic Mass Loss in Binary Stars. IV. Low- and Intermediate-mass Helium Binary Stars
The unstable mass transfer situation in binary systems will asymptotically cause the adiabatic expansion of the donor star and finally lead to the common envelope phase. This process could happen in helium binary systems once the helium donor star fills its Roche-lobe. We have calculated the adiabatic mass-loss model of naked helium stars with a mass range of 0.35 M –10 M , and every mass sequence evolved from the helium-zero-age main sequence to the cooling track of white dwarf or carbon ignition. In consideration of the influence of stellar wind, massive helium stars are not considered in this paper. Comparing the stellar radius with the evolution of the Roche-lobe under the assumption of conservative mass transfer, we give the critical mass ratio q crit = M He/M accretor as the binary stability criteria of low- and intermediate-mass helium binary stars. On the helium main sequence, the result shows 1.0 < q crit < 2.6, which is more unstable than the classical result of polytropic model q crit = 3. After the early helium Hertzsprung Gap, the q crit quickly increases even larger than 10 (more stable compared with the widely used result of q crit = 4), which is dominated by the expansion of the radiative envelope. Our result could be useful for these quick mass transfer binary systems such as AM CVns, ultra-compact X-ray binaries, and helium novae, and it could guide the binary population synthesis for the formation of special objects such as type Ia supernova and gravitational wave sources.
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