An approximate solver for Riemann and Riemann-like Ellipsoidal Configurations

Abstract

We introduce a new technique for constructing three-dimensional (3D) models of incompressible Riemann S-type ellipsoids and compressible triaxial configurations that share the same velocity field as that of Riemann S-type ellipsoids. Our incompressible models are exact steady-state configurations; our compressible models represent approximate steady-state equilibrium configurations. Models built from this method can be used to study a variety of relevant astrophysical and geophysical problems.

25 pages, 10 figures, ApJ accepted, refereed version

References in corpus (2)

• Nonlinear Development of the Secular Bar-mode Instability in Rotating Neutron Stars
• Numerical evolution of secular bar-mode instability induced by the gravitational radiation reaction in rapidly rotating neutron stars

Cited by in corpus (1)

• Further Evidence for an Elliptical Instability in Rotating Fluid Bars and Ellipsoidal Stars