Dissipative superfluid relativistic magnetohydrodynamics of a multicomponent fluid: the combined effect of particle diffusion and vortices

TL;DR

This paper develops a comprehensive set of dissipative relativistic magnetohydrodynamic equations for superfluid and superconducting multicomponent fluids, incorporating particle diffusion and vortex effects relevant to neutron star phenomena.

Contribution

It introduces a unified framework relating phenomenological transport coefficients to microscopic mutual friction and vortex dynamics in relativistic superfluid mixtures.

Findings

Derived equations applicable to neutron star dynamics

Connected transport coefficients with microscopic vortex interactions

Facilitated studies of neutron star evolution and instabilities

Abstract

We formulate dissipative magnetohydrodynamic equations for finite-temperature superfluid and superconducting charged relativistic mixtures, taking into account the effects of particle diffusion and possible presence of Feynman-Onsager and/or Abrikosov vortices in the system. The equations depend on a number of phenomenological transport coefficients, which describe, in particular, relative motions of different particle species and their interaction with vortices. We demonstrate how to relate these transport coefficients to the mutual friction parameters and momentum transfer rates arising in the microscopic theory. The resulting equations can be used to study, in a unified and coherent way, a very wide range of phenomena associated with dynamical processes in neutron stars, e.g., the magnetothermal evolution, stellar oscillations and damping, as well as development and suppression of various hydrodynamic instabilities in neutron stars.