Statistics – Computation
Scientific paper
Jun 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992natur.357..388h&link_type=abstract
Nature (ISSN 0028-0836), vol. 357, no. 6377, June 4, 1992, p. 388, 389.
Statistics
Computation
20
Gamma Ray Bursts, Neutron Stars, Stellar Mass Accretion, Computational Astrophysics, Electromagnetic Radiation, Kelvin-Helmholtz Instability, Stellar Magnetic Fields, Stellar Radiation
Scientific paper
It is shown here that, if slow accretion onto high-velocity neutron stars from the interstellar medium is to be the origin of gamma-ray bursts, the accretion physics is very different from what applies for local low-velocity neutron stars. For halo neutron stars with high magnetic fields and velocities, electromagnetic dipole radiation pressure prevents accretion unless the period is longer than tens of seconds; the centrifugal barrier will then prevent accretion until the period reaches several thousand seconds. For periods as long as this, accretion may proceed through Kelvin-Helmholtz instability at the magnetopause boundary. At interstellar densities and neutron-star magnetic fields of about 10 exp 12 G, the accretion rate by this process can be much larger than the Bondi-Hoyle accretion rate, but is still well below what is needed for slow-accretion burst models. It is concluded that slow accretion onto high-velocity neutron stars in the halo cannot be the origin of gamma-ray bursts.
Harding Alice K.
Leventhal Marvin
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