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首页> 外文期刊>Physical review, D >Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles
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Simulating the magnetorotational collapse of supermassive stars: Incorporating gas pressure perturbations and different rotation profiles

机译：模拟超大分子恒星的磁热塌陷：纳入气体压力扰动和不同的旋转轮廓

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Collapsing supermassive stars (SMSs) with masses M ? 10~(4-6)M_⊙ have long been speculated to be the seeds that can grow and become supermassive black holes (SMBHs). We previously performed general relativistic magnetohydrodynamic (GRMHD) simulations of marginally stable Γ = 4/3 polytropes uniformly rotating at the mass-shedding limit and endowed initially with a dynamically unimportant dipole magnetic field to model the direct collapse of SMSs. These configurations are supported entirely by thermal radiation pressure and reliably model SMSs with M ? 10~6M_⊙. We found that around 90% of the initial stellar mass forms a spinning black hole (BH) remnant surrounded by a massive, hot, magnetized torus, which eventually launches a magnetically-driven jet. SMSs could be therefore sources of ultra-long gamma-ray bursts (ULGRBs). Here we perform GRMHD simulations of Γ ? 4/3, polytropes to account for the perturbative role of gas pressure in SMSs with M ? 10~6M_⊙.We also consider different initial stellar rotation profiles. The stars are initially seeded with a dynamically weak dipole magnetic field that is either confined to the stellar interior or extended from its interior into the stellar exterior. We calculate the gravitational wave burst signal for the different cases. We find that the mass of the black hole remnant is 90%-99% of the initial stellar mass, depending sharply on Γ - 4=3 as well as on the initial stellar rotation profile. After t ～ 250-550M ≈ 1 - 2 × 10~3(M/10~6M_⊙) s following the appearance of the BH horizon, an incipient jet is launched and it lasts for ～10~4-10~5(M/10~6M_⊙) s, consistent with the duration of long gamma-ray bursts. Our numerical results suggest that the Blandford-Znajek mechanism powers the incipient jet. They are also in rough agreement with our recently proposed universal model that estimates accretion rates and electromagnetic (Poynting) luminosities that characterize magnetized BH-disk remnant systems that launch a jet.
机译：用群众折叠超级分类星（SMSS）？长期以来10〜（4-6）M_∞已经推测是可以生长并成为超姿态黑洞（SMBH）的种子。我们以前进行了一般相对论的磁性信息动力学（GRMHD）模拟的边缘稳定γ= 4/3多条均匀旋转在大规模脱落极限上，并且最初用动态不重要的偶极磁场赋予，以模拟SMS的直接崩溃。这些配置完全由热辐射压力和可靠地模拟SMS与M？ 10〜6m_‖。我们发现大约90％的初始恒星质量形成旋转黑洞（BH）残余物，其被大量的热磁化的圆环包围，最终发动磁力驱动的喷射。因此，SMS可能是超长伽马射线爆发（ULGRB）的来源。在这里，我们执行γ的grmhd模拟？ 4/3，伟大的聚四门术考虑了气体压力在SMS中的扰动作用吗？ 10〜6m_‖.我们还考虑了不同的初始恒星旋转型材。恒星最初用动态弱的偶极磁场播种，其局限于恒星内部或从其内部延伸到恒星外部。我们计算不同情况的引力波突发信号。我们发现黑洞残余物的质量是初始恒星质量的90％-99％，急剧上γ - 4 = 3以及初始恒星旋转轮廓。在BH Horizo​​ n外观后T〜250-550米的≈1 - 2×10〜3（m / 10〜6m_ν），推出初期喷射，持续〜10〜4-10〜5（m / 10〜6m_ν）S，与长伽马射线爆发的持续时间一致。我们的数值结果表明，Blandford-Znajek机构为初期喷射提供了贡献。它们也与我们最近提出的通用模型达成粗略的协议，估计具有发射喷射器的磁化BH圆盘残留系统的磁化BH磁盘残留系统的吸收率和电磁（Poynting）发光。

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