一种在X射线双星系统中再现完全相对论光谱的简化方法：应用于天鹅座X-1
A simplified approach for reproducing fully relativistic spectra in X-ray binary systems: Application to Cygnus X-1
AI总结：
本文提出仅移动吸积盘内半径并结合伪牛顿势与kerrbb辐射效率的简化方法，以再现含黑洞自旋的完全相对论X射线光谱，并成功拟合天鹅座X-1。
摘要：
在X射线双星的黑洞附近，广义相对论效应很强，并显著影响最内侧吸积盘区域释放的总能量。我们的目标是在保持标准吸积盘模型简洁性的同时，充分纳入黑洞自旋以及来自X射线双星系统的观测光谱所受到的所有广义相对论效应。这可以通过仅适当地移动吸积盘内半径来实现。我们采用Kerr黑洞周围若干最高效的伪牛顿势，并推导了两个广义吸积盘温度分布，从而将自旋对热光谱的贡献纳入其中。随后，我们将观测到的辐射效率与包含kerrbb模型中全部相对论效应的辐射模式相关联，得到关于修正后吸积盘内半径的表达式。此外，我们通过拟合天鹅座X-1在高/软光谱态和硬/低光谱态期间获得的观测数据，将该方法应用于该源。完全相对论光谱以非常好的近似得到再现，误差范围为0.03–4%。吸积盘由位于(0.2–2)R_ISCO范围内的修正最内半径参数化，具体取决于源的视角和黑洞自旋。黑洞附近的相对论效应会使一个倾角θ<60°的原本标准的吸积盘，在遥远观测者看来似乎被截断到更大的半径。另一方面，侧向观测吸积盘则会产生其比相应ISCO半径更靠近中心天体的视角。此外，我们表明，通过采用相当简单的轻子—强子喷流模型、混合热/非热日冕以及经Kerr调整的标准吸积盘，可以令人满意地拟合天鹅座X-1的观测数据。
英文摘要：
General relativistic effects are strong near the black hole of an X-ray binary and significantly impact the total energy released at the innermost accretion disk's region. Our goal is to fully incorporate the black hole's spin and all the general relativistic effects on the observed spectra coming from X-ray binary systems while maintaining the simplicity of the standard disk model. That is possible by appropriately shifting only the disk's inner radius. We employ some of the most efficient pseudo-Newtonian potentials around Kerr black holes and derive two generalized disk temperature profiles, thus incorporating the spin's contribution to the thermal spectra. Then, we associate the observed radiative efficiency with the emission pattern featuring all the relativistic effects included in the kerrbb model, obtaining an expression about the modified inner radius of the disk. Moreover, we apply this method to Cygnus X-1 by fitting the observational data obtained during its high/soft and hard/low spectral states. The fully relativistic spectra are reproduced to a very good approximation with an error margin of 0.03-4%. The disk is parameterized by a modified innermost radius within the range of $(0.2-2)R_{ISCO}$, depending on the source's viewing angle and black hole spin. Relativistic effects near the black hole make an otherwise standard accretion disk with inclination $θ<60^{\circ}$ seem truncated to larger radii to a distant observer. On the other hand, an edge-on view of the disk gives the perspective of being pulled closer to the central object than the respective ISCO radius. In addition, we show that the observational data of Cygnus X-1 can be satisfactorily fitted by employing a reasonably simple lepto-hadronic jet model and a hybrid thermal/non-thermal corona along with the Kerr-adjusted standard accretion disk.
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