Revisiting the maximum mass of differentially rotating neutron stars in general relativity: Übermassive stars with realistic equations of state
arXiv:1901.05479 · doi:10.1103/PhysRevD.99.083017
Abstract
We study the solution space of general relativistic, axisymmetric, equilibria of differentially rotating neutron stars with realistic, nuclear equations of state. We find that different types of stars, which were identified by earlier works for polytropic equations of state, arise for realistic equations of state, too. Scanning the solution space for the sample of realistic equations of state we treat, we find lower limits on the maximum rest masses supported by cold, differentially rotating stars for each type of stars. We often discover equilibrium configurations that can support more than 2 times the mass of a static star. We call these equilibria "übermassive", and in our survey we find übermassive stars that can support up to 2.5 times the maximum rest mass that can be supported by a cold, non-rotating star with the same equation of state. This is nearly two times larger than what previous studies employing realistic equations of state had found, and which did not uncover übermassive neutron stars. Moreover, we find that the increase in the maximum rest mass with respect to the non-spinning stellar counterpart is larger for moderately stiff equations of state. These results may have implications for the lifetime and the gravitational wave and electromagnetic counterparts of hypermassive neutron stars formed following binary neutron star mergers.
16 pages, 6 figures, 8 tables
References in corpus (23)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Shapiro delay measurement of a two solar mass neutron star
- A Massive Pulsar in a Compact Relativistic Binary
- Multi-messenger Observations of a Binary Neutron Star Merger
- Constraints on a phenomenologically parameterized neutron-star equation of state
- Constraining the Maximum Mass of Neutron Stars From Multi-Messenger Observations of GW170817
- Modeling GW170817 based on numerical relativity and its implications
- Merger of binary neutron stars to a black hole: Disk mass, short gamma-ray bursts, and quasinormal mode ringing
- Binary Neutron Star Mergers: Dependence on the Nuclear Equation of State
- Properties of hypermassive neutron stars formed in mergers of spinning binaries
- Evolution of magnetized, differentially rotating neutron stars: Simulations in full general relativity
- General relativistic simulations of compact binary mergers as engines of short gamma-ray bursts
- Unexpected Dynamical Instabilities In Differentially Rotating Neutron Stars
- Importance of cooling in triggering the collapse of hypermassive neutron stars
- Dynamical Capture Binary Neutron Star Mergers
- On the stability and maximum mass of differentially rotating relativistic stars
- Equation of state effects and one-arm spiral instability in hypermassive neutron stars formed in eccentric neutron star mergers
- Modeling differential rotations of compact stars in equilibriums
- Universal relations for differentially rotating relativistic stars at the threshold to collapse
- Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars
- A new view on the maximum mass of differentially rotating neutron stars
- On a role of corotation radius in the low dynamical instability of differentially rotating stars
- Unstable normal modes of low T/W dynamical instabilities in differentially rotating stars