General relativistic magnetohydrodynamics simulations of prompt-collapse neutron star mergers: The absence of jets
General relativistic magnetohydrodynamics simulations of prompt-collapse neutron star mergers: The absence of jets
复制标题
瞬发中子星合并的广义相对论磁流体动力学模拟：不存在喷流
DOI：
10.1103/physrevd.96.084063
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发表时间：
2017
影响因子：
5
通讯作者：
Shapiro, Stuart L.
中科院分区：
文献类型：
--
作者：
Ruiz, Milton;Shapiro, Stuart L.
吸引并合中子星不仅是引力波的重要来源，也是符合电磁波的候选者。这些系统被认为是短伽马射线暴（sGRB）的祖先。我们先前已经证明，双中子星星合并，在延迟坍缩到一个黑洞周围的可怕的磁化吸积盘可以驱动磁力喷流。我们现在进行磁流体动力学模拟，在完全广义相对论的双中子星合并，undergoentcollapse探索喷流形成的可能性，从黑洞光吸积盘遗迹。我们发现，（是ADM质量）后，迅速黑洞形成，没有证据表明质量外流或磁场准直。合并后黑洞的快速形成阻止了磁能接近磁极上方的无力值，这是通常的布兰德福德-兹纳杰克机制发射喷流所必需的。与sGRB重合的引力波的检测可能会对核状态方程（EOS）提供约束：NSNS合并延迟或即时崩溃的命运，因此sGRB的出现或不出现取决于双星总质量的临界值，并且该值对EOS敏感。
Inspiraling and merging binary neutron stars are not only important source of gravitational waves, but also promising candidates for coincident electromagnetic counterparts. These systems are thought to be progenitors of short gamma-ray bursts (sGRBs). We have shown previously that binary neutron star mergers that undergodelayedcollapse to a black hole surrounded by aweightymagnetized accretion disk can drive magnetically powered jets. We now perform magnetohydrodynamic simulations in full general relativity of binary neutron stars mergers that undergopromptcollapse to explore the possibility of jet formation from black hole-lightaccretion disk remnants. We find that after(is the ADM mass) following prompt black hole formation, there is no evidence of mass outflow or magnetic field collimation. The rapid formation of the black hole following merger prevents magnetic energy from approaching force-free values above the magnetic poles, which is required for the launching of a jet by the usual Blandford-Znajek mechanism. Detection of gravitational waves in coincidence with sGRBs may provide constraints on the nuclear equation of state (EOS): the fate of an NSNS merger–delayed or prompt collapse, and hence the appearance or nonappearance of an sGRB–depends on a critical value of the total mass of the binary, and this value is sensitive to the EOS.