We study low-mass binary X-ray sources involving stellar mass black holes within massive gravity. Regarding the accretion disk, we adopt the standard model for an optically thick, cool, and geometrically thin disk by Shakura–Sunyaev. For the gravitational field generated by the black hole, we consider the analogue of the Schwarzschild–de Sitter space–time of Einstein’s theory in massive gravity, for which we found an additional term linear in the radial coordinate. Then, we compute the radial velocity, the energy density and the pressure as a function of the radial coordinate, and the X-ray emission’s soft spectral component expected from the disk. We also investigated in detail the impact of this new geometry. Our result indicates that by using observed spectra from confirmed X-ray binaries involving astrophysical black holes, we can put strong constraints on alternative theories of gravity.

我们研究了低质量双星 X 射线源，涉及大质量引力中的恒星质量黑洞。关于吸积盘，我们采用 Shakura-Sunyaev 的光学厚、冷和几何薄盘的标准模型。对于黑洞产生的引力场，我们考虑了爱因斯坦大引力理论中施瓦西-德西特时空的类比，为此我们在径向坐标中发现了一个线性项。然后，我们计算径向速度、能量密度和压力作为径向坐标的函数，以及从圆盘预期的 X 射线发射的软光谱分量。我们还详细研究了这种新几何形状的影响。我们的结果表明，通过使用已确认的包含天体物理黑洞的 X 射线双星的观测光谱，