The Wolf–Rayet + Black Hole Binary NGC 300 X-1: What is the Mass of the Black Hole?
The Wolf–Rayet + Black Hole Binary NGC 300 X-1: What is the Mass of the Black Hole?
复制标题
沃尔夫-拉叶 + 黑洞双星 NGC 300 X-1：黑洞的质量是多少？
DOI：
10.3847/1538-4357/abe6a9
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发表时间：
2021
期刊：
影响因子：
--
通讯作者：
B. Williams
中科院分区：
文献类型：
--
作者：
B. Binder;Janelle M. Sy;M. Eracleous;D. Christodoulou;S. Bhattacharya;R. Cappallo;S. Laycock;P. Plucinsky;B. Williams
本文介绍了利用钱德拉X射线天文台和哈勃空间望远镜宇宙起源光谱仪对沃尔夫-拉叶+黑洞（BH）双星系统NGC 300 X-1进行的新的X射线和紫外观测。当与档案X射线观测相结合时，我们的X射线和紫外线观测对整个双星轨道进行采样，为BH吸积盘和施主星星风之间的系统几何形状和相互作用提供线索。我们测量的双星轨道周期为32.7921 ± 0.0003小时，与以前的研究一致，并使用X射线数据进行相位分辨光谱学。X射线光变曲线揭示了一个深食，与倾角i = 60°-75°一致，以及与吸积流撞击盘边缘一致的食前过剩。我们进一步测量了几个突出的远紫外光谱线的径向速度变化，最值得注意的是H ii λ1640和C iv λ1550。我们发现He ii的发射线系统地滞后于预期的沃尔夫-拉叶星星轨道运动，相差Δ v λ 1550，而C iv λ1550与预期的沃尔夫-拉叶施主径向速度曲线的相位相匹配。我们假设C iv λ1550发射线遵循正弦径向速度曲线（半振幅= 250 km s−1），并推断BH质量为17 ± 4 M。我们的观察结果是一致的风洛希瓣溢出吸积盘的存在下，吸积流的形式从引力集中的风材料和影响的BH吸积盘的边缘。
We present new X-ray and UV observations of the Wolf–Rayet + black hole (BH) binary system NGC 300 X-1 with the Chandra X-ray Observatory and the Hubble Space Telescope Cosmic Origins Spectrograph. When combined with archival X-ray observations, our X-ray and UV observations sample the entire binary orbit, providing clues to the system geometry and interaction between the BH accretion disk and the donor star wind. We measure a binary orbital period of 32.7921 ± 0.0003 hr, in agreement with previous studies, and perform phase-resolved spectroscopy using the X-ray data. The X-ray light curve reveals a deep eclipse, consistent with inclination angles of i = 60°–75°, and a pre-eclipse excess consistent with an accretion stream impacting the disk edge. We further measure radial velocity variations for several prominent far-UV spectral lines, most notably H ii λ1640 and C iv λ1550. We find that the He ii emission lines systematically lag the expected Wolf–Rayet star orbital motion by a phase difference of Δϕ ∼ 0.3, while C iv λ1550 matches the phase of the anticipated radial velocity curve of the Wolf–Rayet donor. We assume the C iv λ1550 emission line follows a sinusoidal radial velocity curve (semi-amplitude = 250 km s−1) and infer a BH mass of 17 ± 4 M ⊙. Our observations are consistent with the presence of a wind-Roche lobe overflow accretion disk, where an accretion stream forms from gravitationally focused wind material and impacts the edge of the BH accretion disk.
影响因子：
6.5
作者：
Ben Bekhti, N.;Floer, L.;Staveley-Smith, L.
通讯作者：
Staveley-Smith, L.