Roton instabilities in the superfluid outer core of neutron stars

J. A. Granados, A. M. Mateo, X. Viñas
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Abstract

We study the superfluid dynamics of the outer core of neutron stars by means of a hydrodynamic model made of a neutronic superfluid and a protonic superconductor, coupled by both the dynamic entrainment and the Skyrme SLy4 nucleon-nucleon interactions. The resulting nonlinear equations of motion are probed in the search for dynamical instabilities triggered by the relative motion of the superfluids that could be related to observed timing anomalies in pulsars. Through linear analysis, the origin and expected growth of the instabilities is explored for varying nuclear-matter density. Differently from previous findings, the dispersion of linear excitations in our model shows rotonic structures below the pair-breaking energy threshold, which lies at the origin of the dynamical instabilities, and could eventually lead to emergent vorticity along with modulations of the superfluid density.
中子星超流体外核的罗顿不稳定性
利用中子超流体和质子超导体组成的流体动力学模型,结合动力学夹带和Skyrme - sl4核子-核子相互作用,研究了中子星外核的超流体动力学。所得到的非线性运动方程用于寻找可能与观测到的脉冲星时间异常有关的超流体相对运动引发的动力学不稳定性。通过线性分析,探讨了核物质密度变化时不稳定性的来源和预期增长。与以往的发现不同,我们的模型中线性激励的色散显示出低于对破能阈值的旋转结构,这是动力不稳定性的根源,最终可能导致随超流体密度调制的涌现涡度。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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