In this work, we study the properties of dissipative shocks for fully relativistic accretion flows around spinning black holes. In an accretion flow harbouring a dissipative shock (formally known as radiative shock), a significant portion of the thermal energy may get released from the post-shock corona. A stellar-mass black hole may therefore emit hard X-rays from the inner edge of the disc. If the bulk energy loss is significant, post-shock pressure drops, and shock moves forward towards the black hole compressing the size of the post-shock corona, resulting an enhancement of the corona temperature and compression ratio. The dynamical properties of the radiative shocks are therefore systematically investigated to understand accurately the radiative loss processes, temporal variations, and the spectral properties. We notice that the range of flow parameters (e.g. energy and angular momentum) responsible for the formation of ‘shocks in accretion (SA)’ is identical for both the cases of standing and dissipative shocks. The spin of the black hole enhances the dissipation further. We estimate the maximum energy release, which is observed close to |$100{{\ \rm per\ cent}}$| in the extreme cases. This could be useful in explaining various observed phenomena namely the formation and the systematic evolution of quasi-periodic oscillations, and the time lags in between hard and soft X-ray photons (e.g. XTE J1550−564, GRO J1655−40, etc.) during their outbursts.

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相对论吸积流中耗散冲击的性质

在这项工作中，我们研究了围绕旋转黑洞的相对论性吸积流的耗散冲击性质。在具有耗散冲击（正式称为辐射冲击）的积积流中，很大一部分热能可能会从电击后的电晕中释放出来。因此，恒星质量的黑洞可能会从光盘的内边缘发出硬X射线。如果大量能量损失显着，则电击后压力会降低，并且冲击会朝黑洞前进，从而压缩电击后电晕的大小，从而提高电晕温度和压缩比。因此，系统地研究了辐射冲击的动力学特性，以准确地理解辐射损耗过程，时间变化和光谱特性。我们注意到，引起“吸积激增（SA）”形成的流动参数范围（例如，能量和角动量）对于立式和耗散冲击两种情况都是相同的。黑洞的旋转进一步增强了耗散。我们估算了最大能量释放，该能量释放接近| $ 100 {{\\ rm per \ cent}} $ | 在极端情况下。这可能有助于解释各种观察到的现象，即准周期振荡的形成和系统演化，以及硬X射线和软X射线光子之间的时间差（例如，XTE J1550-564，GRO J1655-40等）。在爆发期间