中子星合并中相对论性npeμ物质的体粘度

M. Alford, A. Harutyunyan, A. Sedrakian
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引用次数: 7

摘要

讨论了由弱相互作用直接Urca过程产生的热致密npem物质的体粘度。我们考虑两种感兴趣的机制:(a) T≤Ttr的中微子透明机制(Ttr≃5÷10 MeV是中微子捕获温度);(b) T≥Ttr的中微子俘获区。采用密度依赖参数化的相对论密度泛函方法对核物质进行了建模。当温度为T≃5÷6 MeV时,材料的体积粘度达到最大值;当温度较高时,材料的体积粘度迅速下降,产生中微子俘获。作为天体物理学的应用,我们通过中子星合并中的体粘度估计密度振荡的阻尼时间尺度,发现在振荡频率f=10 kHz时,在4≤T≤7 MeV的温度下,体粘度可能会影响合并后物体的演化,阻尼将非常有效。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Bulk Viscosity of Relativistic npeμ Matter in Neutron-Star Mergers
We discuss the bulk viscosity of hot and dense npeμ matter arising from weak-interaction direct Urca processes. We consider two regimes of interest: (a) the neutrino-transparent regime with T≤Ttr (Ttr≃5÷10 MeV is the neutrino-trapping temperature); and (b) the neutrino-trapped regime with T≥Ttr. Nuclear matter is modeled in relativistic density functional approach with density-dependent parametrization DDME2. The maximum of the bulk viscosity is achieved at temperatures T≃5÷6 MeV in the neutrino-transparent regime, then it drops rapidly at higher temperatures where neutrino-trapping occurs. As an astrophysical application, we estimate the damping timescales of density oscillations by the bulk viscosity in neutron star mergers and find that, e.g., at the oscillation frequency f=10 kHz, the damping will be very efficient at temperatures 4≤T≤7 MeV where the bulk viscosity might affect the evolution of the post-merger object.
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