Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000astl...26..572z&link_type=abstract
Astronomy Letters, vol. 26, p. 572-581 (2000)
Astronomy and Astrophysics
Astronomy
5
Scientific paper
We further investigate the two-dimensional hydrodynamic explosion model for rapidly rotating and collapsing supernovae (Aksenov et al. 1997), in which the initial energy release inside a fragmenting low-mass neutron star of critical mass approximately equal to 0.1 M_solar moving in a circular orbit at a velocity of 18000 km/s is reduced considerably. This velocity closely corresponds to a pulsar escape velocity of about 1000 km/s (at a total mass of 1.9 M_solar for the binary of neutron stars). Compared to our previous study (Zabrodina and Imshennik 1999), this energy release was reduced by more than a half. Otherwise, the model in question does not differ from the explosion model with a self-consistent chemical composition of nuclides investigated in the above paper. In particular, the initial energy release was carefully reconciled with a chemical composition. Our numerical solution shows that the reduction in energy release due to the time scales of processes and neutrino energy losses being finite does not alter the qualitative results of our previous studies (Aksenov et al. 1997; Imshennik and Zabrodina 1999). An intense undamped diverging shock wave (with a total post-shock energy equal to or exceeding 1051 erg at a front radius of about 10000 km) is formed; a large asymmetry of explosion with a narrow cone (with a solid angle of about pi/4) around the leading direction, which coincides with the velocity direction of the low-mass neutron star at the instant of its explosive fragmentation in the two-dimensional model, emerges. A jet of synthesized radioactive nickel, whose mass is estimated by using simple threshold criteria to be M_Ni = (0.02-0.03) M_solar, is concentrated inside this cone. This appears to be the integrated parameter that is most sensitive to the specified reduction in initial energy release; it is also reduced by almost a half compared to our previous estimate (Imshennik and Zabrodina 1999). The time of propagation of the shock wave inferred in our model to the presupernova surface was estimated for SN1987A to be 0.5-1.0 h, in agreement with observations.
Imshennik Vladimir S.
Zabrodina E. A.
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