SUPERFLUID HYDRODYNAMICS IN ROTATING NEUTRON-STARS .1. NONDISSIPATIVE EQUATIONS

被引：133

作者：

MENDELL, G

机构：

[1] Department of Physics, Montana State University, Bozeman

来源：

ASTROPHYSICAL JOURNAL | 1991年 / 380卷 / 02期

关键词：

DENSE MATTER; HYDRODYNAMICS; STARS; MAGNETIC; NEUTRON; PULSATION; ROTATION;

D O I：

10.1086/170609

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Newtonian hydrodynamic equations are developed which describe the outer-core regions of neutron stars composed of superfluid neutrons, superconducting protons, and degenerate electrons and muons. The equations include couplings to the gravitational and electromagnetic fields. They also include the effects of rotation and forces due to the elastic properties of the neutron and proton vortices. The set of equations is closed by constructing a model of the total energy density and using it to express the dependent variables in terms of the independent variables. The low-frequency-long-wavelength limit of the equations is determined. The results will be applicable to studies of the large-scale oscillations of rotating and magnetized neutron stars.

引用

页码：515 / 529

页数：15

共 54 条

[1]

Abramowitz M.., 1972, HDB MATH FUNCTIONS

[2] RAPID POSTGLITCH SPIN-UP OF THE SUPERFLUID CORE IN PULSARS [J].