发表机构
University of Hamburg; Goethe Universität; University of Idaho; INAF-Osservatorio di Astrofisica e Scienza dello Spazio; University of Ferrara; INFN, Sezione di Ferrara; INAF - Osservatorio Astronomico d’Abruzzo; New Uzbekistan University; Trinity College（汉堡大学; 法兰克福歌德大学; 爱达荷大学; 意大利国家天体物理研究所天文与空间科学观测站; 费拉拉大学; 意大利国家核物理研究所费拉拉分部; 意大利国家天体物理研究所阿布鲁佐天文台; 新乌兹别克斯坦大学; 三一学院）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
研究具有高自旋和大质量不对称性的黑洞 - 中子星双星系统，通过广义相对论磁流体动力学模拟，结合核反应网络和辐射传输代码，探究喷射物质性质及电磁特征，计算千新星光变曲线并与数据比较，结果总体一致。
AI 中文摘要
由黑洞（BH）和中子星（NS）组成的致密双星系统有望在引力波和电磁通道中提供可探测信号，是多信使天文学的理想源。在本系列的第三篇论文中，我们报告了在广义相对论磁流体动力学模拟中，针对由大质量比和高BH自旋组成的综合双星参数空间内，纯动力学喷射成分的几何和热力学性质。通过监测能量和角动量向物质的转移来研究潮汐瓦解和动态质量喷射，扩展了低质量比、无旋转BHNS双星的已知结果。通过改变双星参数，研究其对喷射物质几何、热力学和运动学性质的影响。还利用核反应网络SkyNet获得喷射物中r过程产生的元素丰度，并研究其如何依赖于前身天体的性质。最后，使用辐射传输代码POSSIS根据模拟结果计算千新星光变曲线，讨论其热辐射和光学/近红外演化，并与AT2017gfo数据和S190814bv的上限进行比较，总体结果一致。
英文摘要
Compact binary systems consisting of a black hole (BH) and a neutron star (NS) are expected to provide detectable signals both in the gravitational wave and in the electromagnetic channels, thus representing excellent sources for multi-messenger astronomy. In this third paper in a series, we report on the geometric and thermodynamic properties of the purely dynamical ejecta component modeled in our general-relativistic magnetohydrodynamical simulations of BHNS systems over a comprehensive binary parameter space consisting of large mass ratio and high BH spin. The tidal disruption and dynamical mass ejection is studied by monitoring the transfer of energy and angular momentum to matter for the particular case of a highly unequal-mass binary with large BH spin, extending known results for low-mass-ratio, irrotational BHNS binaries. By varying the binary parameters, we investigate their influence on the geometric, thermodynamic, and kinematic properties of the ejected matter. Furthermore, we employ the nuclear-reaction network SkyNet to obtain the elemental abundances resulting from the r-process active in the ejecta and study how they depend on the properties of the progenitor objects. Finally, using the radiative-transfer code POSSIS, we compute the kilonova light-curves from the results of our simulations, discuss their bolometric and optical/near-infrared evolution, and compare them with the AT2017gfo data and upper-limits for S190814bv, finding overall consistency.
Comments29 pages, 18 figures, replaced outdated figure; matches the version accepted by PRD
