On the stability and maximum mass of differentially rotating relativistic stars
Abstract
The stability properties of rotating relativistic stars against prompt gravitational collapse to a black hole are rather well understood for uniformly rotating models. This is not the case for differentially rotating neutron stars, which are expected to be produced in catastrophic events such as the merger of binary system of neutron stars or the collapse of a massive stellar core. We consider sequences of differentially rotating equilibrium models using the j-constant law and by combining them with their dynamical evolution, we show that a sufficient stability criterion for differentially rotating neutron stars exists similar to the one of their uniformly rotating counterparts. Namely: along a sequence of constant angular momentum, a dynamical instability sets in for central rest-mass densities slightly below the one of the equilibrium solution at the turning point. In addition, following Breu & Rezzolla, we show that 'quasi-universal' relations can be found when calculating the turning-point mass. In turn, this allows us to compute the maximum mass allowed by differential rotation, M_(max,dr), in terms of the maximum mass of the non-rotating configuration, M_(TOV), finding that M_(max,dr) ≃ (1.54 ± 0.05)M_(TOV) for all the equations of state we have considered.
Additional Information
© 2017 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. We thank G. Bozzola and C. Breu for useful discussions. This research is supported in part by the ERC synergy grant 'BlackHoleCam: Imaging the Event Horizon of Black Holes' (Grant No. 610058), by 'NewCompStar', COST Action MP1304, by the LOEWE-Program in the Helmholtz International Center (HIC) for FAIR, and by the European Union's Horizon 2020 Research and Innovation Programme (Grant 671698) (call FETHPC-1-2014, project ExaHyPE). The simulations were performed on the SuperMUC cluster at the LRZ in Garching, on the LOEWE cluster in CSC in Frankfurt, and on the HazelHen cluster at the HLRS in Stuttgart.Attached Files
Published - slx178.pdf
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Additional details
- Eprint ID
- 121237
- Resolver ID
- CaltechAUTHORS:20230501-297567000.62
- 610058
- European Research Council (ERC)
- MP1304
- European Cooperation in Science and Technology (COST)
- Helmholtz International Center for FAIR
- 671698
- European Research Council (ERC)
- Created
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2023-05-25Created from EPrint's datestamp field
- Updated
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2023-05-25Created from EPrint's last_modified field