The multimessenger picture of compact object encounters: binary mergers versus dynamical collisions
The multimessenger picture of compact object encounters: binary mergers versus dynamical collisions
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DOI：
10.1093/mnras/sts708
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发表时间：
2012-04
影响因子：
4.8
通讯作者：
S. Rosswog;S. Rosswog;S. Rosswog;T. Piran;E. Nakar
中科院分区：
文献类型：
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作者：
S. Rosswog;S. Rosswog;S. Rosswog;T. Piran;E. Nakar
我们探讨了两颗中子星（ns 2）和一颗中子星星与一个恒星质量黑洞（nsbh）相遇的多信使信号。我们专注于引力波驱动的双星合并和动力学碰撞，例如，在球状星团之间的diepheros。我们的讨论是基于牛顿流体力学模拟，将核状态方程和多avour中微子治疗。对于这两种类型的遭遇，我们比较了引力波和中微子发射特性。我们还计算了几乎未绑定的质量被送回中央残留物的弹道回落plusviscous磁盘模型的速率，我们分析了动态喷出的物质的属性。最后但并非最不重要的是，我们解决电磁瞬变，伴随着每种类型的遭遇。我们发现，动力学碰撞至少和双星合并一样有希望产生（短）伽马射线暴，但它们也有同样的重子污染的可能性。所有遇到的遗迹产生峰值中微子光度至少为10 - 53 erg/s，一些碰撞的情况下超过这个值超过一个数量级。典型的ns 2合并的情况下，激发了超过1%的太阳质量的极端中子丰富（叶0：03）的材料，这是一致的双中子星星合并是一个主要来源的r-过程中的星系。nsbh碰撞喷射出非常大量的物质（0：15 M），这严重限制了它们的可接受发生率。因此，紧凑型天体的碰撞率（ns 2和nsbh的总和）一定小于ns 2合并率的10%，很可能要小得多。放射性衰变喷出物产生的光学UV\macronova”，其中，典型的合并的情况下，峰值后0：4天的光度为5 - 10 - 41 erg/s。NS 2（NSBH）碰撞达到2（4）倍大的峰值亮度。动态喷出物存款动能相当于周围介质中的超新星。典型的合并情况下释放约2 10 50尔格，最极端（但可能罕见）的情况下存款动能高达10 52尔格。这种温和的相对论性物质被周围的介质减速，产生了持久的射电战神。在先进的LIGO/Virgo的探测视界处的规范ns 2合并产生了一个无线电
We explore the multi-messenger signatures of encounters between two neutron stars (ns 2 ) and between a neutron star and a stellar-mass black hole (nsbh). We focus on the dierences between gravitational wave driven binary mergers and dynamical collisions that occur, for example, in globular clusters. Our discussion is based on Newtonian hydrodynamics simulations that incorporate a nuclear equation of state and a multiavour neutrino treatment. For both types of encounters we compare the gravitational wave and neutrino emission properties. We also calculate the rates at which nearly unbound mass is delivered back to the central remnant in a ballistic-fallback-plusviscous-disk model and we analyze the properties of the dynamically ejected matter. Last but not least we address the electromagnetic transients that accompany each type of encounter. We nd that dynamical collisions are at least as promising as binary mergers for producing (short) gamma-ray bursts, but they also share the same possible caveats in terms of baryonic pollution. All encounter remnants produce peak neutrino luminosities of at least 10 53 erg/s, some of the collision cases exceed this value by more than an order of magnitude. The canonical ns 2 merger case ejects more than 1% of a solar mass of extremely neutron-rich (Ye 0:03) material, an amount that is consistent with double neutron star mergers being a major source of r-process in the galaxy. nsbh collisions eject very large amounts of matter ( 0:15 M ) which seriously constrains their admissible occurrence rates. The compact object collision rate (sum of ns 2 and nsbh) must therefore be less, likely much less, than 10% of the ns 2 merger rate. The radioactively decaying ejecta produce optical-UV \macronova" which, for the canonical merger case, peak after 0:4 days with a luminosity of 5 10 41 erg/s. ns 2 (nsbh) collisions reach up to 2 (4) times larger peak luminosities. The dynamic ejecta deposit a kinetic energy comparable to a supernova in the ambient medium. The canonical merger case releases approximately 2 10 50 erg, the most extreme (but likely rare) cases deposit kinetic energies of up to 10 52 erg. The deceleration of this mildly relativistic material by the ambient medium produces long lasting radio ares. A canonical ns 2 merger at the detection horizon of advanced LIGO/Virgo produces a radio