在黑暗中低语：与OB型伴星成对的黑洞的微弱X射线辐射
Whispering in the dark: Faint X-ray emission from black holes with OB star companions
AI总结：
本文通过MESA双星演化模型和星族合成，预测OB型星伴星黑洞的微弱非热X射线辐射，发现大麦哲伦云中至少28个此类系统可被钱德拉望远镜观测到，为揭示X射线暗黑洞星族及引力波并合前身提供约束。
摘要：
研究背景。近期对OB型星的天体测量和光谱巡天揭示了一些恒星质量黑洞，其轨道周期短至10天。由于黑洞周围缺乏辐射高效的吸积盘，未探测到X射线对应体。然而，黑洞周围高温、稀薄且强磁化等离子体（即所谓黑洞冕）中的耗散过程仍可产生非热X射线辐射（如同步辐射）。研究目标。我们确定了轨道周期长达数千天的BH+OB型星双星的X射线光度分布。研究方法。我们使用MESA计算的详细双星演化模型，初始主星质量为10-90太阳质量，轨道周期为1-3000天。针对广泛的辐射效率范围计算X射线光度。研究结果。我们表明，通过磁重联进行的粒子加速可以加热黑洞冕。吸积等离子体引力势能的相当大一部分被转化为非热X射线辐射。我们的星族合成分析预测，大麦哲伦云中至少有28个（最多72个）BH+OB型星双星产生的X射线光度高于10的31次方尔格每秒，可通过聚焦的钱德拉X射线天文台观测到。我们在大麦哲伦云中识别出一批SB1系统，并在银河系中识别出HD96670，它们包含O型星及其质量超过2.3太阳质量的不可见伴星，与我们的预测吻合良好。这些发射X射线的黑洞的OB型伴星的预测光度为10的4.5至5.5次方太阳光度。结论。这些结果为对围绕OB型星识别的恒星质量黑洞候选体进行长时间X射线曝光提供了依据。这将约束X射线暗黑洞的潜在星族、从单简并到双简并双星的演化，以及引力波并合的前身天体。（有删节）
英文摘要：
Context. Recent astrometric and spectroscopic surveys of OB stars have revealed a few stellar-mass black holes (BHs) with orbital periods as low as 10 days. No X-ray counterpart has been detected, due to the absence of a radiatively efficient accretion disk around the BH. Yet, dissipative processes in the hot, dilute and strongly magnetized plasma around the BH (so-called BH corona) can still lead to non-thermal X-ray emission (e.g. synchrotron). Aims. We determine the X-ray luminosity distribution from BH+OB star binaries up to orbital periods of a few thousand days. Methods. We use detailed binary evolution models computed with MESA for initial primary masses of 10-90 $M_{\odot}$ and orbital periods from 1-3000 d. The X-ray luminosity is computed for a broad range of radiative efficiencies. Results. We show that particle acceleration through magnetic reconnection can heat the BH corona. A substantial fraction of the gravitational potential energy from the accreted plasma is converted into non-thermal X-ray emission. Our population synthesis analysis predicts at least 28 (up to 72) BH+OB star binaries in the Large Magellanic Cloud (LMC) to produce X-ray luminosity above 10$^{31}$ erg$\,$s$^{-1}$, observable through focused Chandra observations. We identify a population of SB1 systems in the LMC and HD96670 in the Milky Way comprising O stars with unseen companions of masses above 2.3 $M_{\odot}$ that aligns well with our predictions. The predicted luminosities of the OB companions to these X-ray-emitting BHs are 10$^{4.5-5.5}$ $L_{\odot}$. Conclusions. These results make the case for long-time exposure in X-rays of the stellar-mass BH candidates identified around OB stars. It will constrain the underlying population of X-ray-faint BHs, the evolution from single to double degenerate binaries, and the progenitors of gravitational wave mergers. (Abridged)
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