Semidetached Mass-transfer Massive Binaries in the Nearby Galaxy M31
Semidetached Mass-transfer Massive Binaries in the Nearby Galaxy M31
复制标题
附近星系 M31 中的半分离质量转移大质量双星
DOI：
10.3847/1538-3881/ac5685
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发表时间：
2022-04
期刊：
影响因子：
--
通讯作者：
Liao W. -P.
中科院分区：
文献类型：
--
作者：
Li F. -X.;Qian S. -B.;Liao W. -P.
半独立双星提供了一个有价值的测试相互作用的双星的质量从一个组件转移到另一个的演化模型，两个组件的演化将被改变。在银河系中，半独立双星的研究已经取得了很多成果，而在仙女座星系（M31）中的研究却很少。通过分析Vilardell等人观测到的12颗食双星的光变曲线，我们使用Wilson和Devinney方法确定了这些系统的基本参数。发现它们是半独立双星，其中质量较小的部分充满了它们的洛希叶，而质量较大的部分则从洛希叶中分离出来。我们第一次计算了它们的光极小期。这些半独立双星中的主星具有不同的质量比和填充因子，是研究M31双星演化的良好源星。结果表明，质量比与初级填充因子有关。具有较高质量比的系统往往具有较低的填充因子。这些结果可以解释质量较小组分向质量较大组分的质量转移。此外，光度的解决方案显示，二次组件比主要的，表明它们是由原来分离的二元系统通过一个案例A的质量转移形成的演变。这些双星经历了质量反转演化，处于附近星系M31的A类演化的晚期。
Semidetached binaries provide a valuable test of the evolutionary models of interacting binaries where the mass is transferring from one component to the other, and the evolutions of both components will be changed. Many results of semidetached binaries have been obtained in the Milky Way, while there are few studies in the Andromeda galaxy (M31). By analyzing the light curves of 12 eclipsing binaries observed by Vilardell et al., we determined the fundamental parameters of these systems using the Wilson and Devinney method. It is discovered that they are semidetached binaries where the less massive components have filled their Roche lobes, while the more massive ones are detached from the lobes. We calculated their times of light minimum for the first time. The primary stars in those semidetached binaries have different mass ratios and fill-out factors and they are good sources to investigate the binary evolution in M31. It is found that the mass ratio is correlated with the fill-out factor of the primary. Systems with higher mass ratios tend to have lower fill-out factors. These results can be explained that the mass transfer from the less massive component to the more massive one. Moreover, the photometric solutions reveal that the secondary components are more evolved than the primary ones indicating that they are formed from originally detached binary systems via a case A mass transfer. These binaries have experienced the mass-reverse evolution and are at the late stage of a case A evolution in the nearby galaxy M31.
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