A two-dimensional hydrodynamic model for asymmetric explosions of collapsing supernovae with rapid initial rotation

Details A two-dimensional hydrodynamic model for asymmetric explosions of collapsing supernovae with rapid initial rotation A two-dimensional hydrodynamic model for asymmetric explosions of collapsing supernovae with rapid initial rotation

Nov 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997astl...23..677a&link_type=abstract

Astronomy Letters, Volume 23, Issue 6, November 1997, pp.677-689; Pis'ma v Astronomicheskii Zhurnal, Vol. 23, p. 779

Astronomy and Astrophysics

Astronomy

10

Scientific paper

In accordance with the rotational model of the explosions of collapsing supernovae, the main energy release (~ 10^51 erg) arises from the hydrodynamic transformation of a low-mass neutron star of critical mass ~0.1M_solar into a hydrodynamically expanding "iron" star. We consider a two-dimensional, axially symmetric hydrodynamic model for the explosion of such a low-mass neutron star. This star is assumed to move in a circular orbit in a binary system, together with a more massive neutron star, which turns into a pulsar (or a black hole?). The binary system of neutron stars is embedded in a relatively rarified gas (the outer shell of the iron core of the presupernova) of total mass 0.1M_solar with initial density that is uniformly distributed in space. The numerical calculation of the axisymmetric explosion is performed by two independent finite-difference methods: (1) by the Lagrangian method (LM) developed by Godunov et al. (1976), which singles out both the contact boundary between the region of energy release and the surrounding medium and the front of an outgoing shock wave; and (2) by the Eulerian parabolic piecewise method (PPM) (Colella and Woodword, 1984; Colella and Glas, 1985) that has been previously applied by Aksenov and Imshennik (1994) to a similar problem. The results obtained by the two methods for the shock front configuration and for the high-temperature gas behind it are in good agreement. The equation of state was taken in the simplest but adequate form for the problem under consideration - an ideal gas with blackbody radiation. The numerical model has one essential parameter - the kick velocity of the pulsar (or the black hole?) v_p . The main result of the calculations is that for a high kick velocity of the pulsar (v_p ~ 1000 km s^-1) that is typical of the rotational mechanism there is a strong asymmetry of the explosion, which turns out to be concentrated in a cone with an opening angle ~ 120 (the solid angle ~ pi) whose direction is opposite to that of the velocity vector of the pulsar. Such an explosion is capable of producing a jet of radioactive ^56Ni of mass ~ 0.1M_solar, in qualitative and quantitative agreement with the observations of SN 1987A. An appreciable asymmetry of the explosion is also retained for more moderate kick velocities of the pulsar - down to the mean observed velocity ~500 km s^-1 (Lyne and Lorimer, 1994).

Affiliated with

Also associated with

No associations

Rating

A two-dimensional hydrodynamic model for asymmetric explosions of collapsing supernovae with rapid initial rotation does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with A two-dimensional hydrodynamic model for asymmetric explosions of collapsing supernovae with rapid initial rotation, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A two-dimensional hydrodynamic model for asymmetric explosions of collapsing supernovae with rapid initial rotation will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1686690