Damping of density oscillations in neutrino-transparent nuclear matter
Damping of density oscillations in neutrino-transparent nuclear matter
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DOI：
10.1103/physrevc.100.035803
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发表时间：
2019-07
影响因子：
3.1
通讯作者：
M. Alford;S. Harris
中科院分区：
文献类型：
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作者：
M. Alford;S. Harris
我们计算了核物质中绝热密度振荡的体粘性耗散时间，密度为核饱和密度的 1-7 倍，温度范围为 1 MeV，其中对先前低温计算的修正变得很重要，高达 10 MeV，中微子透明度的假设不再有效。在这些预计会在中子星合并中发生的条件下，密度振荡的阻尼是通过弱相互作用由β平衡引起的。我们发现，对于 1 kHz 振荡，最短耗散时间在 5 到 20 ms 范围内，具体取决于状态方程，这意味着体粘性阻尼可能会影响中子星合并的动力学。对于更高的频率，耗散时间甚至可以更短。
We calculate the bulk-viscous dissipation time for adiabatic density oscillations in nuclear matter at densities of 1-7 times nuclear saturation density and at temperatures ranging from 1 MeV, where corrections to previous low-temperature calculations become important, up to 10 MeV, where the assumption of neutrino transparency is no longer valid. Under these conditions, which are expected to occur in neutron star mergers, damping of density oscillations arises from beta equilibration via weak interactions. We find that for 1 kHz oscillations the shortest dissipation times are in the 5 to 20 ms range, depending on the equation of state, which means that bulk viscous damping could affect the dynamics of a neutron star merger. For higher frequencies the dissipation time can be even shorter.