Black hole to breakout: 3D GRMHD simulations of collapsar jets reveal a wide range of transients
Black hole to breakout: 3D GRMHD simulations of collapsar jets reveal a wide range of transients
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黑洞到爆发：塌缩星喷流的 3D GRMHD 模拟揭示了各种瞬态现象
DOI：
10.1093/mnras/stab3784
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发表时间：
2022
影响因子：
4.8
通讯作者：
Tchekhovskoy, Alexander
中科院分区：
文献类型：
--
作者：
Gottlieb, Ore;Lalakos, Aretaios;Bromberg, Omer;Liska, Matthew;Tchekhovskoy, Alexander
我们提出了一套第一个3D GRMHD Eksar模拟，从自洽射流发射的吸积克尔黑洞（BH）的爆发从星星。我们确定了三种类型的外流，取决于角动量，l，崩溃的材料和磁场，B，在BH地平线上：（i）subrelativistic外流（低地高B），（ii）固定吸积激波不稳定性（SASI;高地低B），（iii）相对论射流（高地高B）。在没有喷流的情况下，恒星包层的自由落体为BH吸积速率提供了一个很好的估计。喷流可以大大抑制吸积率，其持续时间可以限制在星星的磁化剖面。我们发现，具有大的（陡峭的）内部密度幂律指数（1002）的祖先，由于过度的亮度，在整个爆发和短爆发时间的光变曲线中的全球时间演化，与观测不一致，伽马射线暴（GRB）祖先面临着极端的挑战。我们的研究结果表明，各种各样的观测到的爆炸外观（超新星/超新星+伽玛暴/低光度伽玛暴）和发射相对论流出的特性（亮度和持续时间）可以自然地解释的祖先结构的差异。我们的模拟揭示了几个重要的喷流功能：（一）强磁耗散内的星星，导致弱磁化射流突破，可能有显着的光球发射和（ii）自发出现的倾斜吸积盘喷流，即使在没有任何倾斜的祖。
We present a suite of the first 3D GRMHD collapsar simulations, which extend from the self-consistent jet launching by an accreting Kerr black hole (BH) to the breakout from the star. We identify three types of outflows, depending on the angular momentum,l, of the collapsing material and the magnetic field,B, on the BH horizon: (i)subrelativistic outflow(lowland highB), (ii)stationary accretion shock instability(SASI; highland lowB), (iii)relativistic jets(highland highB). In the absence of jets, free-fall of the stellar envelope provides a good estimate for the BH accretion rate. Jets can substantially suppress the accretion rate, and their duration can be limited by the magnetization profile in the star. We find that progenitors with large (steep) inner density power-law indices (≳ 2), face extreme challenges as gamma-ray burst (GRB) progenitors due to excessive luminosity, global time evolution in the light curve throughout the burst and short breakout times, inconsistent with observations. Our results suggest that the wide variety of observed explosion appearances (supernova/supernova + GRB/low-luminosity GRBs) and the characteristics of the emitting relativistic outflows (luminosity and duration) can be naturally explained by the differences in the progenitor structure. Our simulations reveal several important jet features: (i) strong magnetic dissipation inside the star, resulting in weakly magnetized jets by breakout that may have significant photospheric emission and (ii) spontaneous emergence of tilted accretion disc-jet flows, even in the absence of any tilt in the progenitor.