On the maximum mass of differentially rotating neutron stars

Thomas W. Baumgarte, Stuart L. Shapiro, Masaru Shibata

Research output: Contribution to journalArticle

Abstract

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 that 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.

Original languageEnglish (US)
Pages (from-to)L29-L32
JournalAstrophysical Journal
Volume528
Issue number1 PART 2
StatePublished - Jan 1 2000

Keywords

  • Black hole physics
  • Relativity
  • Stars: neutron
  • Stars: rotation

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Baumgarte, T. W., Shapiro, S. L., & Shibata, M. (2000). On the maximum mass of differentially rotating neutron stars. Astrophysical Journal, 528(1 PART 2), L29-L32.