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RESEARCH PRODUCT
Gravitational wave content and stability of uniformly, rotating, triaxial neutron stars in general relativity
Stuart L. ShapiroVasileios PaschalidisKōji UryūLuca BaiottiMilton RuizAntonios Tsokarossubject
AstrofísicaPhysicsHigh Energy Astrophysical Phenomena (astro-ph.HE)010308 nuclear & particles physicsGravitational waveGeneral relativityFOS: Physical sciencesGeneral Relativity and Quantum Cosmology (gr-qc)Compact star01 natural sciencesGeneral Relativity and Quantum CosmologyArticleGravitational energyNumerical relativityClassical mechanicsTests of general relativity0103 physical sciencesAstronomiaTwo-body problem in general relativityAstrophysics - High Energy Astrophysical Phenomena010303 astronomy & astrophysicsAstrophysics::Galaxy AstrophysicsGravitational redshiftdescription
Targets for ground-based gravitational wave interferometers include continuous, quasiperiodic sources of gravitational radiation, such as isolated, spinning neutron stars. In this work we perform evolution simulations of uniformly rotating, triaxially deformed stars, the compressible analogues in general relativity of incompressible, Newtonian Jacobi ellipsoids. We investigate their stability and gravitational wave emission. We employ five models, both normal and supramassive, and track their evolution with different grid setups and resolutions, as well as with two different evolution codes. We find that all models are dynamically stable and produce a strain that is approximately one-tenth the average value of a merging binary system. We track their secular evolution and find that all our stars evolve towards axisymmetry, maintaining their uniform rotation, kinetic energy, and angular momentum profiles while losing their triaxiality.
| year | journal | country | edition | language |
|---|---|---|---|---|
| 2017-03-31 |