The Collapsar Model for Gamma Ray Bursts - Two-Dimensional Calculations

Details The Collapsar Model for Gamma Ray Bursts - Two-Dimensional Calculations The Collapsar Model for Gamma Ray Bursts - Two-Dimensional Calculations

May 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...192.4302m&link_type=abstract

American Astronomical Society, 192nd AAS Meeting, #43.02; Bulletin of the American Astronomical Society, Vol. 30, p.874

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We present two-dimensional hydrodynamical calculations of the ``collapsar'' model for gamma-ray bursts using a PPM hydrodynamics code and appropriate nuclear, neutrino and accretion disc physics. The collapsar model occurs in rotating massive stars which fail to eject all of their envelopes in a supernova explosion. The remaining material collapses onto the stellar core, forming a black hole which continues to accrete matter. The infalling material forms a disc around the black hole which heats due to viscous dissipation and emits neutrinos. For example, the collapse of the inner 8 Msun of a 25 Msun star with specific angular momentum of ~ 10(17) cm(2 s(-1)) forms an accretion disc with densities of ~ 10(10) g cm(-3) , temperatures of ~ 5x10(10) K, and a resultant peak integrated neutrino luminosity of nearly 10(52) erg s(-1) . These neutrinos annihilate along the polar axis to form a photon/e(+) e(-) pair plasma, which is posited to expand, break through the stellar mantle and drive a beamed gamma ray burst. Other systems containing specific angular momentum in the range 10(16) - 10(18) cm(2 s(-1)) which will produce similar black hole accretion disc configurations include the merger of black hole--white dwarf and black hole--red giant binaries. This model predicts large amounts of mildly relativistic ejecta in addition to the ultra-relativistic material producing the gamma rays. The mildly relativistic material may have important implications for afterglows in non-gamma-ray wavelengths.

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