Relativistic Models for Binary Neutron Stars with Arbitrary Spins

Abstract

We introduce a new numerical scheme for solving the initial value problem for quasiequilibrium binary neutron stars allowing for arbitrary spins. The coupled Einstein field equations and equations of relativistic hydrodynamics are solved in the Wilson-Mathews conformal thin sandwich formalism. We construct sequences of circular-orbit binaries of varying separation, keeping the rest mass and circulation constant along each sequence. Solutions are presented for configurations obeying an n=1 polytropic equation of state and spinning parallel and antiparallel to the orbital angular momentum. We treat stars with moderate compaction ((m/R) = 0.14) and high compaction ((m/R) = 0.19). For all but the highest circulation sequences, the spins of the neutron stars increase as the binary separation decreases. Our zero-circulation cases approximate irrotational sequences, for which the spin angular frequencies of the stars increases by 13% (11%) of the orbital frequency for (m/R) = 0.14 ((m/R) = 0.19) by the time the innermost circular orbit is reached. In addition to leaving an imprint on the inspiral gravitational waveform, this spin effect is measurable in the electromagnetic signal if one of the stars is a pulsar visible from Earth.

arXiv comment21 pages, 14 figures. A few explanatory sentences added and some typos corrected. Accepted for publication in Phys. Rev. D

References in corpus (27)

• Gamma-Ray Bursts as the Death Throes of Massive Binary Stars
• Gravitational radiation from compact binary systems: gravitational waveforms and energy loss to second post-Newtonian order
• Relativistic Numerical Method for Close Neutron Star Binaries
• Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. I. Method and tests
• Initial Data for Numerical Relativity
• Numerical Relativity and Compact Binaries
• Numerical models of irrotational binary neutron stars in general relativity
• General Relativistic Models of Binary Neutron Stars in Quasiequilibrium
• A relativistic formalism to compute quasi-equilibrium configurations of non-synchronized neutron star binaries
• Thermodynamics of binary black holes and neutron stars
• Binary Neutron Stars in General Relativity: Quasi-Equilibrium Models
• A new numerical method for constructing quasi-equilibrium sequences of irrotational binary neutron stars in general relativity
• Quasiequilibrium sequences of synchronized and irrotational binary neutron stars in general relativity. III. Identical and different mass stars with gamma=2
• Testing a Simplified Version of Einstein's Equations for Numerical Relativity
• Hydrodynamic Simulations in 3+1 General Relativity
• Properties of general relativistic, irrotational binary neutron stars in close quasiequilibrium orbits : Polytropic equations of state
• Irrotational Binary Neutron Stars in Quasiequilibrium in General Relativity
• Irrotational binary neutron stars in quasiequilibrium
• A relativistic formalism for computation of irrotational binary stars in quasi equilibrium states
• Relativistic Hydrodynamics in Close Binary Systems: Analysis of Neutron-Star Collapse
• The Stability of Relativistic Neutron Stars in Binary Orbit
• Binary Neutron-Star Systems: From the Newtonian Regime to the Last Stable Orbit
• Formulation for the internal motion of quasi-equilibrium configurations in general relativity
• Tidal interaction in binary black hole inspiral
• Computing the Complete Gravitational Wavetrain from Relativistic Binary Inspiral
• A new numerical scheme to compute 3D configurations of quasiequilibrium compact stars in general relativity -- Application to synchronously rotating binary star systems --
• Quasiequilibrium sequences of synchronously rotating binary neutron stars with constant rest masses in general relativity -- Another approach without using the conformally flat condition --

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• Gravitational waves from neutron star mergers and their relation to the nuclear equation of state
• Spin-orbit interactions in black-hole binaries
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• On the black hole from merging binary neutron stars: how fast can it spin?
• Gravitomagnetic resonant excitation of Rossby modes in coalescing neutron star binaries
• Constructing quasi-equilibrium initial data for binary neutron stars with arbitrary spins
• A new numerical method to construct binary neutron star initial data
• Various features of quasiequilibrium sequences of binary neutron stars in general relativity
• Initial data for binary neutron stars with arbitrary spins
• Binary Neutron Stars with Arbitrary Spins in Numerical Relativity
• Dynamical Determination of the Innermost Stable Circular Orbit of Binary Neutron Stars
• Constructing Binary Neutron Star Initial Data with High Spins, High Compactness, and High Mass-Ratios
• A post-Newtonian diagnosis of quasiequilibrium configurations of neutron star-neutron star and neutron star-black hole binaries
• The initial value problem as it relates to numerical relativity
• Initial data for neutron star binaries with arbitrary spins
• Binary Neutron Stars in Quasi-equilibrium
• Are neutron stars crushed? Gravitomagnetic tidal fields as a mechanism for binary-induced collapse
• Constant circulation sequences of binary neutron stars and their spin characterization
• Conservation laws and evolution schemes in geodesic, hydrodynamic and magnetohydrodynamic flows
• A formalism for the construction of binary neutron stars with arbitrary circulation
• Bouncing Dirac particles: compatibility between MIT boundary conditions and Thomas precession
• Numerical experiments of adjusted BSSN systems for controlling constraint violations
• Hamiltonian Relaxation
• Methods for relativistic self-gravitating fluids: From binary neutron stars to black hole-disks and magnetized rotating neutron stars
• Effect of spin in binary neutron star mergers
• Source term method for binary neutron stars initial data
• Momentum constraint relaxation