Differentially Rotating Hypermassive Neutron Stars

University of Illinois at Urbana-Champaign



We construct relativistic equilibrium models of differentially rotating neutron stars and show that they can support significantly more mass than their nonrotating or uniformly rotating counterparts. We dynamically evolve such ``hypermassive'' models in full general relativity and show that there do exist configurations which are dynamically stable against radial collapse and bar formation. Our results suggest that the remnant of binary neutron star coalescence may be temporarily stabilized by differential rotation, leading to delayed collapse and a delayed gravitational wave burst.

Introduction to Hypermassive Maximally Rotating Neutron Stars

A Stable Hypermassive Neutron Star: T/W ~ 0.23

A Bar-Unstable Hypermassive Neutron Star: T/W ~ 0.25

A Bar-Unstable Hypermassive Neutron Star (Spiral Arms):
T/W ~ 0.26

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University of Illinois at Urbana-Champaign
last updated 08 Jun 00 by hpa
Center for Theoretical Astrophysics---University of Illinois at Urbana-Champaign

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