当前位置：
X-MOL 学术
›
Astron. Astrophys.
›
论文详情
Our official English website, www.x-mol.net, welcomes your feedback! (Note: you will need to create a separate account there.)
Spectroscopic searches for evolutionary orbital period changes in WR+OB binaries: The case of WR 127 (Hen 3-1772)
Astronomy & Astrophysics ( IF 6.5 ) Pub Date : 2024-03-22 , DOI: 10.1051/0004-6361/202449736 I. A. Shaposhnikov , A. M. Cherepashchuk , A. V. Dodin , K. A. Postnov
Astronomy & Astrophysics ( IF 6.5 ) Pub Date : 2024-03-22 , DOI: 10.1051/0004-6361/202449736 I. A. Shaposhnikov , A. M. Cherepashchuk , A. V. Dodin , K. A. Postnov
Aims. We aim to determine the secular evolution of the orbital period of the short-period binary system WR 127 (WN3b+O9.5V, P ≈ 9.555d).Methods. We performed new low-resolution spectroscopic observations of WR 127 with the 2.5 m CMO SAI telescope to construct the radial velocity curves of the components. Our results suggest component masses of MWRsin3(i) = 11.8 ± 1.4 M⊙ and MOsin3(i) = 17.2 ± 1.4 M⊙. By comparing these values with archival radial velocity curves we were able to create an (O − C) plot with an accuracy sufficient to search for the orbital period change in WR 127.Results. We report the reliable detection of a secular increase in the orbital period of WR 127 at a rate of Ṗ = 0.83 ± 0.14 s yr−1, which corresponds to a dynamical mass-loss rate from the Wolf-Rayet (WR) star of ĖWR = (2.6 ± 0.5) × 10−5 M⊙ yr−1.Conclusions. The mass-loss rate from WR stars in three Wolf-Rayet+OB binaries (WR 127, CX Cep, and V444 Cyg) as inferred from spectroscopic and photometric measurements suggests a preliminary empirical correlation between a WR star’s mass and its dynamical mass-loss rate of . This relation is important for the understanding of the evolution of massive close binaries that include WR stars as such an evolution is a precursor of gravitational-wave binary merging events with neutron stars and black holes.
中文翻译：
光谱搜索 WR+OB 双星演化轨道周期变化：以 WR 127 (Hen 3-1772) 为例
目标。我们的目标是确定短周期双星系统 WR 127 (WN3b+O9.5V, P ≈ 9.555 d ) 轨道周期的长期演化。方法。我们使用 2.5 m CMO SAI 望远镜对 WR 127 进行了新的低分辨率光谱观测，以构建组件的径向速度曲线。我们的结果表明M WR sin 3 ( i ) = 11.8 ± 1.4 M ⊙和M O sin 3 ( i ) = 17.2 ± 1.4 M ⊙的组成质量。通过将这些值与档案径向速度曲线进行比较，我们能够创建一个 ( O − C ) 图，其精度足以搜索 WR 127结果中的轨道周期变化。我们报告可靠地探测到 WR 127 的轨道周期以Ṗ = 0.83 ± 0.14 s yr -1的速率长期增加，这对应于Ė的沃尔夫-拉叶 (WR) 星的动态质量损失率WR = (2.6 ± 0.5) × 10 −5 M ⊙ yr −1 。结论。从光谱和光度测量中推断出的三个 Wolf-Rayet+OB 双星（WR 127、CX Cep 和 V444 Cyg）中 WR 恒星的质量损失率表明 WR 恒星的质量与其动态质量损失之间存在初步的经验相关性比率 。这种关系对于理解包括WR星在内的大质量紧密双星的演化非常重要，因为这种演化是引力波双星与中子星和黑洞合并事件的前兆。
更新日期：2024-03-22
中文翻译：
光谱搜索 WR+OB 双星演化轨道周期变化：以 WR 127 (Hen 3-1772) 为例
目标。我们的目标是确定短周期双星系统 WR 127 (WN3b+O9.5V, P ≈ 9.555 d ) 轨道周期的长期演化。方法。我们使用 2.5 m CMO SAI 望远镜对 WR 127 进行了新的低分辨率光谱观测，以构建组件的径向速度曲线。我们的结果表明M WR sin 3 ( i ) = 11.8 ± 1.4 M ⊙和M O sin 3 ( i ) = 17.2 ± 1.4 M ⊙的组成质量。通过将这些值与档案径向速度曲线进行比较，我们能够创建一个 ( O − C ) 图，其精度足以搜索 WR 127结果中的轨道周期变化。我们报告可靠地探测到 WR 127 的轨道周期以Ṗ = 0.83 ± 0.14 s yr -1的速率长期增加，这对应于Ė的沃尔夫-拉叶 (WR) 星的动态质量损失率WR = (2.6 ± 0.5) × 10 −5 M ⊙ yr −1 。结论。从光谱和光度测量中推断出的三个 Wolf-Rayet+OB 双星（WR 127、CX Cep 和 V444 Cyg）中 WR 恒星的质量损失率表明 WR 恒星的质量与其动态质量损失之间存在初步的经验相关性比率 。这种关系对于理解包括WR星在内的大质量紧密双星的演化非常重要，因为这种演化是引力波双星与中子星和黑洞合并事件的前兆。
京公网安备 11010802027423号