TL;DR
This paper reviews recent theoretical and numerical advances in modeling rotating relativistic stars, focusing on their structure, oscillations, instabilities, magnetic fields, and gravitational wave emissions.
Contribution
It provides a comprehensive overview of the latest methods and findings related to the physics of rotating relativistic stars, including nonaxisymmetric instabilities and gravitational wave sources.
Findings
Advances in modeling rotating stars with magnetic fields and hot proto-neutron stars.
Insights into nonaxisymmetric oscillations and instabilities.
Summary of gravitational wave-driven (CFS) instability developments.
Abstract
Rotating relativistic stars are receiving significant attention in recent years, because of the information they can yield about the equation of state of matter at extremely high densities and because they are one of the more possible sources of detectable gravitational waves. We review the latest theoretical and numerical methods for modeling rotating relativistic stars, including stars with a strong magnetic field and hot proto-neutron stars. We also review nonaxisymmetric oscillations and instabilities in rotating stars and summarize the latest developments regarding the gravitational wave-driven (CFS) instability in both polar and axial quasi-normal modes.
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