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arXiv 1702.04532gr-qc
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球状Proca星的数值演化

Numerical evolutions of spherical Proca stars

Nicolas Sanchis-Gual, Carlos Herdeiro, Eugen Radu, Juan Carlos Degollado, José A. Font

发表信息：
Phys. Rev. D 95, 104028 (2017)
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摘要：

矢量玻色子星，或$\textit{Proca stars}$，最近已获得完全非线性数值解的爱因斯坦-（复杂）-Proca系统。它们是一个大质量矢量场的自引力、处处非奇异、无水平的玻色-爱因斯坦凝聚体，在许多方面（但不是全部）类似于它们的标量表亲，即著名的（标量）$\textit{boson stars}$。在本文中，我们报告Proca星的完全非线性数值演化，专注于球对称的情况下，其目标是评估其稳定性和不稳定的恒星演化的终点。线性微扰理论的结果表明，在ADM质量最大时，稳定构型和不稳定构型发生分离。我们的模拟证实了这一结果。不断发展的数值不稳定的解决方案，我们发现，根据该解决方案的结合能的符号和扰动，三种不同的结果：$(i)$迁移到稳定的分支，$(ii)$总色散的标量场，或$(iii)$崩溃的史瓦西黑洞。在后一种情况下，由准束缚态组成的长寿Proca场残余物-$\textit{Proca wig}$ -在其形成后可能会在视界之外看到，其寿命与Proca质量成反比。我们评论的相似性/差异与标量的情况下，以及与中子星。

英文摘要：

Vector boson stars, or $\textit{Proca stars}$, have been recently obtained as fully non-linear numerical solutions of the Einstein-(complex)-Proca system. These are self-gravitating, everywhere non-singular, horizonless Bose-Einstein condensates of a massive vector field, which resemble in many ways, but not all, their scalar cousins, the well-known (scalar) $\textit{boson stars}$. In this paper we report fully-non linear numerical evolutions of Proca stars, focusing on the spherically symmetric case, with the goal of assessing their stability and the end-point of the evolution of the unstable stars. Previous results from linear perturbation theory indicate the separation between stable and unstable configurations occurs at the solution with maximal ADM mass. Our simulations confirm this result. Evolving numerically unstable solutions, we find, depending on the sign of the binding energy of the solution and on the perturbation, three different outcomes: $(i)$ migration to the stable branch, $(ii)$ total dispersion of the scalar field, or $(iii)$ collapse to a Schwarzschild black hole. In the latter case, a long lived Proca field remnant -- a $\textit{Proca wig}$ -- composed by quasi-bound states, may be seen outside the horizon after its formation, with a life-time that scales inversely with the Proca mass. We comment on the similarities/differences with the scalar case as well as with neutron stars.

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