论文标题
二进制中子星合并残留物和2017年8月的蓝色Kilonova的磁性驱动的Baryon风
Magnetically driven baryon winds from binary neutron star merger remnants and the blue kilonova of August 2017
论文作者
论文摘要
在引力波中检测到的与第一二元中子星（BNS）合并相关的放射性基洛诺瓦的观察证明，这些事件是生产重型R过程元素的理想场所。但是，仍辩论了该基洛诺娃的早期（“蓝色”）和后期（“红色”）组件的弹出材料的物理起源。在这里，我们调查了早期/蓝色Kilonova起源于在亚稳态中子恒星Remnant合并后发射的磁性Baryon风。利用超过250毫秒的合并后进化，利用磁化的BNS合并模拟，我们可以首次遵循直至最终下降的全部质量弹出过程。我们发现，重子风带有$ \ simeq \！0.010 \！ - \！0.028 \，m_ \ odot $ of Unbound材料，证明可以实现蓝色Kilonova的高质量。我们还发现，与观测估计的下端一致的最高$ \ sim \！0.2 \，C $的膨胀速度，我们在这里讨论了可能进一步提高最终喷射速度的可能效果。总体而言，我们的结果表明，磁性驱动的重子风是解释蓝色基洛诺瓦的可行渠道。
The observation of a radioactively-powered kilonova associated with the first binary neutron star (BNS) merger detected in gravitational waves proved that these events are ideal sites for the production of heavy r-process elements. However, the physical origin of the ejected material responsible for the early ("blue") and late ("red") components of this kilonova is still debated. Here, we investigate the possibility that the early/blue kilonova originated from the magnetically driven baryon wind launched after merger by the metastable neutron star remnant. Exploiting a magnetized BNS merger simulation with over 250 ms of post-merger evolution, we can follow for the first time the full mass ejection process up to its final decline. We find that the baryon wind carries $\simeq\!0.010\!-\!0.028\,M_\odot$ of unbound material, proving that the high mass estimated for the blue kilonova can be achieved. We also find expansion velocities of up to $\sim\!0.2\,c$, consistent with the lower end of the observational estimates, and we discuss possible effects neglected here that could further increase the final ejecta velocity. Overall, our results show that the magnetically driven baryon wind represents a viable channel to explain the blue kilonova.
