论文标题
GW190521作为Proca星星的合并：潜在的新向量玻色子$ 8.7 \ times 10^{ - 13} $ ev
GW190521 as a merger of Proca stars: a potential new vector boson of $8.7 \times 10^{-13}$ eV
论文作者
论文摘要
先进的Ligo-Virgo报道了一个短引力波信号（GW190521）被解释为黑洞的准圆形合并，一个填充了配对的超级nova间隙，形成了$ M_F \ sim 142 m_ \ odot $ odot $的剩余黑洞，$ d _ 3 $ d $ d_5 $ gp。但是，GW190521几乎看不见的前结合发射，值得进一步研究合并前动力学甚至碰撞物体本质的研究。我们表明，GW190521与数值模拟信号一致571^{+348} _ { - 181} $ mpc。 Proca星的超光矢量玻色子组成的质量为$μ_ {\ rm V} = 8.72^{+0.73} _ { - 0.82} \ times10^{ - 13} $ ev。这提供了这两个理论模型之间紧密堕落的首次证明，以实现真正的重力波事件。确认Proca星星的解释，我们发现统计学上有略有优势，将为长期寻求的暗物质粒子提供第一个证据。
Advanced LIGO-Virgo reported a short gravitational-wave signal (GW190521) interpreted as a quasi-circular merger of black holes, one populating the pair-instability supernova gap, forming a remnant black hole of $M_f\sim 142 M_\odot$ at a luminosity distance of $d_L \sim 5.3$ Gpc. With barely visible pre-merger emission, however, GW190521 merits further investigation of the pre-merger dynamics and even of the very nature of the colliding objects. We show that GW190521 is consistent with numerically simulated signals from head-on collisions of two (equal mass and spin) horizonless vector boson stars (aka Proca stars), forming a final black hole with $M_f = 231^{+13}_{-17}\,M_\odot$, located at a distance of $d_L = 571^{+348}_{-181}$ Mpc. The favoured mass for the ultra-light vector boson constituent of the Proca stars is $μ_{\rm V}= 8.72^{+0.73}_{-0.82}\times10^{-13}$ eV. This provides the first demonstration of close degeneracy between these two theoretical models, for a real gravitational-wave event. Confirmation of the Proca star interpretation, which we find statistically slightly preferred, would provide the first evidence for a long sought dark matter particle.
