Merging neutron star - Black hole binaries

M Ruffert, H T Janka

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

We report on ongoing investigations of the merger model for the central engine of gamma-ray bursts and show first results of a new set of simulations for neutron star black hole binaries. The masses of the neutron star and black hole are the same in all cases, but we change the numerical resolution and the gravitational potential of the black hole by using descriptions that follow [12] and [1]. Since our code is basically Newtonian, this procedure is supposed to mimic the general relativistic effects that are associated with the existence of an innermost stable orbit and the variation of this orbit and of the horizon radius with the spin and the growing mass of the accreting black hole. The neutron star, which initially is in orbit about the black hole, is tidally disrupted but in several cases the remnant manages to temporarily move to a more eccentric orbit. A second and final episode of mass transfer follows, producing the standard outcome of a high-density torus around the black hole. Our simulations still need to be analysed with respect to the neutrino-antineutrino annihilation luminosities, but we expect similar values as in the double neutron star models.

Original languageEnglish
Title of host publicationGAMMA-RAY BURST AND AFTERGLOW ASTRONOMY 2001
EditorsGR Ricker, RK Vanderspek
Place of PublicationMELVILLE
PublisherAmerican Institute of Physics
Pages193-198
Number of pages6
ISBN (Print)0-7354-0122-5
Publication statusPublished - 2003

Keywords

  • GAMMA-RAY BURSTS
  • ADAPTIVE MESH REFINEMENT
  • NEWTONIAN HYDRODYNAMICS
  • PHYSICAL MODELS
  • EMISSION
  • SIMULATIONS
  • EQUATION
  • MERGERS
  • STEP

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