黑洞-中子星并合的相对论模拟：黑洞自旋的影响
Relativistic Simulations of Black Hole-Neutron Star Mergers: Effects of black-hole spin
摘要：
黑洞-中子星（BHNS）双星合并是产生短硬伽马射线暴（SGRB）和可探测的引力波的候选引擎。使用我们最新的共形薄夹层BHNS初始数据和我们的完全广义相对论流体动力学代码，这是现在AMR的能力，我们能够有效地和准确地模拟这些二进制文件从大分离通过inspiral，合并，和ringdown。我们发展的度量使用BSSN制定标准的移动穿刺计的条件和处理的流体力学与高分辨率的冲击捕获计划。我们探索BH自旋（与轨道角动量对齐和反对齐）的影响，通过演化三组初始数据，BH：NS质量比q=3：数据集几乎相同，除了BH自旋在a/M = -0.5（反对齐），0.0和0.75之间变化。合并前的轨道数随着a/M的增加而增加，正如预期的那样。我们还研究了非自旋BH的情况下，更详细地，不同的q之间的1，3，和5。我们计算引力波形的情况下，我们模拟和比较它们的二元黑洞波形。对于反取向自旋情况（a/M = -0.5）和最极端的质量比情况（q=5），只有一个小的盘（< 0.01 M_sun）形成。相比之下，在快速旋转（a/M = 0.75）排列的BH情况下，形成了一个大质量（M_disk约为0.2 M_sun）的热盘。这样的盘可以驱动SGRB，可能通过例如，产生大量的中微子-反中微子对
英文摘要：
Black hole-neutron star (BHNS) binary mergers are candidate engines for generating both short-hard gamma-ray bursts (SGRBs) and detectable gravitational waves. Using our most recent conformal thin-sandwich BHNS initial data and our fully general relativistic hydrodynamics code, which is now AMR-capable, we are able to efficiently and accurately simulate these binaries from large separations through inspiral, merger, and ringdown. We evolve the metric using the BSSN formulation with the standard moving puncture gauge conditions and handle the hydrodynamics with a high-resolution shock-capturing scheme. We explore the effects of BH spin (aligned and anti-aligned with the orbital angular momentum) by evolving three sets of initial data with BH:NS mass ratio q=3: the data sets are nearly identical, except the BH spin is varied between a/M = -0.5 (anti-aligned), 0.0, and 0.75. The number of orbits before merger increases with a/M, as expected. We also study the nonspinning BH case in more detail, varying q between 1, 3, and 5. We calculate gravitational waveforms for the cases we simulate and compare them to binary black-hole waveforms. Only a small disk (< 0.01 M_sun) forms for the anti-aligned spin case (a/M = -0.5) and for the most extreme mass ratio case (q=5). By contrast, a massive (M_disk is about 0.2 M_sun), hot disk forms in the rapidly spinning (a/M = 0.75) aligned BH case. Such a disk could drive a SGRB,possibly by, e.g., producing a copious flux of neutrino-antineutino pairs.
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