论文标题
迷失在太空中：同伴围绕大量垂死的星星的致命舞蹈
Lost in space: companions' fatal dance around massive dying stars
论文作者
论文摘要
行星和恒星残留式脉搏的发现挑战了我们的理解，因为巨大的超新星爆炸形成了脉冲星，可能破坏了系统的稳定性。 II型超新星爆炸导致形成怪异的结合系统，自由浮动行星，中子星，脉冲星和白矮人。迄今为止，基于扰动理论的高质量损失率系统的分析和数值研究主要集中在行星明星系统上。在本文中，我们通过使用合理的弹性速度（$ 1000-10000 \，\ Mathrm {km/s} $），信封和中子星质量假设同源的包膜扩展模型，扩展了对行星星和二进制系统的命运的理解。该调查涵盖了行星1-10MJUP的次要肿块，恒星伴侣的1-20MSUN。我们进行并分析了超过250万个模拟，假设该伴侣的半轴轴（2.23-100AU），偏心率（0-0.8）和True-Anmalies（0-2PI）。在同源扩展方案中，我们确认爆炸最可能的结果是系统的稳定，而绑定系统的保留需要高度怪异的原始轨道。通常，较高的喷射速度导致偏心轨道较低，而偏心轨道独立于次级质量。近距离脉冲星行星的解释需要异国情调的形成场景，而不是通过II型超新星爆炸模型存活。即使爆炸模型是对称的，爆炸后结合的恒星系统即使爆炸模型是奇特的速度（<100 \，km/s）。应用的数值模型使我们能够得出解离系统的速度成分。自由浮动行星和恒星尸体的特殊速度在10^-6-275km/s的范围内。
Discoveries of planet- and stellar remnant-hosting pulsars challenge our understanding as the violent supernova explosion that forms the pulsar presumably destabilizes the system. Type II supernova explosions lead to the formation of eccentric bound systems, free-floating planets, neutron stars, pulsars, and white dwarfs. Analytical and numerical studies of high mass-loss rate systems based on perturbation theory so far have focused mainly on planet-star systems. In this paper, we extend our understanding of the fate of planet-star and binary systems by assuming a homologous envelope expansion model using a plausible ejection velocity ($1000-10000\,\mathrm{km/s}$), envelope- and neutron star masses. The investigation covers secondary masses of 1-10MJup for planetary, and 1-20MSun for stellar companions. We conduct and analyze over 2.5 million simulations assuming different semi-major axes (2.23 - 100au), eccentricities (0-0.8), and true-anomalies (0-2pi) for the companion. In a homologous expansion scenario, we confirm that the most probable outcome of the explosion is the destabilization of the system, while the retention of a bound system requires a highly eccentric primordial orbit. In general, a higher ejecta velocity results in a lower eccentricity orbit independent of secondary mass. The explanation of close-in pulsar planets requires exotic formation scenarios, rather than survival through the type II supernova explosion model. Post-explosion bound star systems gain a peculiar velocity (<100\,km/s), even though the explosion model is symmetric. The applied numerical model allows us to derive velocity components for dissociating systems. The peculiar velocities of free-floating planets and stellar corpses are in the range of 10^-6-275km/s.
