β equilibrium in neutron-star mergers

被引：51

作者：

Alford, Mark G. ^{[1
]}

Harris, Steven P. ^{[1
]}

机构：

[1] Washington Univ, Dept Phys, St Louis, MO 63130 USA

来源：

PHYSICAL REVIEW C | 2018年 / 98卷 / 06期

关键词：

BULK VISCOSITY; URCA PROCESSES; CORES;

D O I：

10.1103/PhysRevC.98.065806

中图分类号：

O57 [原子核物理学、高能物理学];

学科分类号：

070202 ;

摘要：

We show that the commonly used criterion for beta equilibrium in neutrino-transparent dense nuclear matter becomes invalid as temperatures rise above 1 MeV. Such temperatures are attained in neutron-star mergers. By numerically computing the relevant weak-interaction rates we find that the correct criterion for beta equilibrium requires an isospin chemical potential that can be as large as 10-20 MeV, depending on the temperature at which neutrinos become trapped.

引用

页数：12

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