Computer Science – Numerical Analysis
Scientific paper
Oct 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ans..conf...19w&link_type=abstract
Presented at the Accreting Neutron Star Conf., Garching, West Germany, 19-24 Jul. 1982
Computer Science
Numerical Analysis
Gamma Ray Bursts, Neutron Stars, Nuclear Models, Thermonuclear Reactions, X Rays, Helium, Hydrogen, Magnetic Field Configurations, Numerical Analysis, Stellar Envelopes, Stellar Luminosity
Scientific paper
Different regimes of nuclear burning are reviewed, each appropriate to a given range of (steady state) accretion rate. Accretion rates in the range 10 to the -14th power to 10 to the -10th power Msub solar/y all appear capable of producing X-ray transients of various durations and intervals. Modifications introduced by radiatively driven mass loss, the thermal inertial of the envelope, different burning mechanisms, and two dimensional considerations are discussed as are difficulties encountered when the thermonuclear model is confronted with observations of rapidly recurrent bursts, and super-Eddington luminosities and temperatures. Results from a numerical simulation of a combined hydrogen-helium runaway initiated at pycnonuclear density are presented. The thermonuclear model for gamma ray bursts is reviewed and updated, particularly with regard to the breakdown of the steady state hypothesis employed in previous work. Solely on the basis of nuclear instability, gamma ray bursts of various types appear possible for a very broad variety of accretion rates although other considerations may restrict this range.
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