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Magnetically Induced Rotating Rayleigh-Taylor Instability
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Fast Rotating Relativistic Stars: Spectra and Stability without Approximation
Christian J Krüger1,2, Kostas D Kokkotas1
1Theoretical Astrophysics, IAAT, University of Tübingen, 72076 Tübingen, Germany.
Physical Review Letters
|September 25, 2020
Summary
This study explores neutron star oscillations and instabilities using general relativity. We propose universal relations for gravitational wave asteroseismology to constrain neutron star properties.
Area of Science:
- Astrophysics
- General Relativity
- Nuclear Physics
Background:
- Neutron stars are extreme astrophysical objects governed by general relativity.
- Understanding their oscillations and instabilities is crucial for probing their internal structure.
- Dynamic spacetime effects are essential for accurate modeling.
Purpose of the Study:
- To investigate oscillations and instabilities of relativistic stars.
- To determine the oscillation spectrum and critical values for secular CFS instability.
- To propose universal relations for gravitational wave asteroseismology.
Main Methods:
- Perturbation theory in general relativity.
- Incorporation of dynamic spacetime contributions.
- Analysis of oscillation spectra and instability thresholds.
Main Results:
- The oscillation spectrum of relativistic stars was determined.
- Critical values for the secular CFS instability of neutron stars were calculated.
- Universal relations for gravitational wave asteroseismology were proposed.
Conclusions:
- The proposed relations can help constrain neutron star radius and/or the nuclear equation of state.
- Results are applicable to all life stages of neutron stars, particularly post-merger objects.
- This work advances the field of neutron star asteroseismology.
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