标题： GRMHD模拟中的盘-喷流共生：解释硬态ULXs 显示英文标题

标题： Disk-Outflow Symbiosis in GRMHD Simulations: Explaining Hard-State ULXs

摘要： 超亮X射线源（ULXs）因其极高的光度和独特的光谱特征，数十年来一直吸引着研究人员的关注。 其中一些源的表现超出预期，在低硬态下相对于恒星质量源表现出超爱丁顿光度。 数值稳态计算表明，这种状态下的ULXs可以被解释为围绕恒星级黑洞的高磁化吸积源。 为了进一步探讨这一点，我们使用公开可用的代码BHAC（黑洞吸积代码）进行GRMHD模拟，以建模黑洞周围高磁化吸积流的行为。 我们的模拟显示，此类系统确实能够产生ULXs中观测到的强烈光度。 此外，我们验证了这些高强度辐射所需的磁场强度约为$10^7$ 高斯，与先前的数值稳态研究一致。 显示英文摘要

摘要： Ultraluminous X-ray sources (ULXs) have captivated researchers for decades due to their exceptionally high luminosities and unique spectral characteristics. Some of these sources defy expectations by exhibiting super-Eddington luminosities with respect to stellar mass sources even in their low-hard state. Numerical steady-state calculations suggest that ULXs in this state can be explained as highly magnetized advective accretion sources around stellar-mass black holes. To explore this further, we employ GRMHD simulations using the publicly available code, BHAC (Black Hole Accretion Code), to model the behavior of highly magnetized advective accretion flows around a black hole. Our simulations demonstrate that such systems can indeed produce the intense luminosities observed in ULXs. Additionally, we validate that the magnetic fields required for these high emissions are of the order of $10^7$ Gauss, consistent with previous numerical steady-state findings.