Stable Case BB/BC Mass Transfer to Form GW190425-like Massive Binary Neutron Star Mergers

Ying Qin, Jin-Ping Zhu, Georges Meynet, Bing Zhang, Fa-Yin Wang, Xin-Wen Shu, Han-Feng Song, Yuan-Zhu Wang, Liang Yuan, Zhen-Han-Tao Wang, Rui-Chong Hu, Dong-Hong Wu, Shuang-Xi Yi, Qing-Wen Tang, Jun-Jie Wei, Xue-Feng Wu, En-Wei Liang
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Abstract

On April 25th, 2019, the LIGO-Virgo Collaboration discovered a Gravitational-wave (GW) signal from a binary neutron star (BNS) merger, i.e., GW190425. Due to the inferred large total mass, the origin of GW190425 remains unclear. We perform detailed stellar structure and binary evolution calculations that take into account mass-loss, internal differential rotation, and tidal interactions between a He-rich star and a NS companion. We explore the parameter space of the initial binary properties, including initial NS and He-rich masses and initial orbital period. We find that the immediate post-common-envelope progenitor system, consisting of a primary $\sim2.0\,M_\odot$ ($\sim1.7\,M_\odot$) NS and a secondary He-rich star with an initial mass of $\sim3.0-5.5\,M_\odot$ ($\sim5.5-6.0\,M_\odot$) in a close binary with an initial period of $\sim0.08-0.5\,{\rm{days}}$ ($\sim 0.08-0.4\,{\rm{days}}$), that experiences stable Case BB/BC mass transfer (MT) during binary evolution, can reproduce the formation of GW190425-like BNS events. Our studies reveal that the secondary He-rich star of the GW190425's progenitor before its core collapse can be efficiently spun up through tidal interaction, finally remaining as a NS with rotational energy even reaching $\sim10^{52}\,{\rm{erg}}$, which is always much higher than the neutrino-driven energy of the supernova (SN) explosion. If the newborn secondary NS is a magnetar, we expect that GW190425 can be the remnant of a magnetar-driven SN, e.g., a magnetar-driven ultra-stripped SN, a superluminous SN, or a broad-line Type Ic SN. Our results show that GW190425 could be formed through the isolated binary evolution, which involves a stable Case BB/BC MT just after the common envelope phase. On top of that, we show the He-rich star can be tidally spun up, potentially forming a spinning magnetized NS (magnetar) during the second SN explosion.
稳定情况下BB/BC质量转移形成类似GW190425的大质量双中子星合并
2019年4月25日,LIGO-Virgo合作组织发现了双中子星(BNS)合并产生的引力波(GW)信号,即GW190425。由于推断的总质量很大,GW190425 的起源仍然不清楚。我们进行了详细的恒星结构和双星演化计算,其中考虑到了质量损失、内部差转以及富氦恒星和NS伴星之间的潮汐相互作用。我们探索了初始双星特性的参数空间,包括初始 NS 星和富氦星的质量以及初始轨道周期。我们发现,紧随其后的共包层原生星系统由一颗主星$\sim2.0\,M_\odot$($\sim1.7\,M_\odot$)NS和一颗富氦次星组成,富氦次星的初始质量为$\sim3.0-5.5\,M_\odot$($\sim5.5-6.我们的研究发现,GW190425的原生星在其核心坍缩之前的富氦次生星可以通过潮汐相互作用有效地旋转起来,最终保持为NS,其旋转能量甚至达到$/sim10^{52}/\,{\rm{erg}}$,始终远高于超新星(SN)爆炸的中微子驱动能量。如果新生的次级NS是磁星,那么我们预计GW190425可能是磁星驱动的SN的残余,例如磁星驱动的超条纹SN、超光SN或宽线Ic型SN。我们的研究结果表明,GW190425可能是通过孤立双星演化形成的,这涉及到一个稳定的Case BB/BC MT,就在共同包膜阶段之后。此外,我们还发现富氦恒星可能会发生潮汐旋转,从而有可能在第二SN爆发过程中形成一个旋转的磁化NS(磁星)。
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