Hydrodynamical instabilities and mixing in SN 1987A - Two-dimensional simulations of the first 3 months
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)
Results are presented from numerical simulations of the early stages of the explosion of SN 1987A. Using a two-dimensional cylindrical geometry version of a smooth particle hydrodynamics code, the explosion is followed for three months to investigate both the early hydrodynamical instabilities and the effect of the subsequent radioactive decay of Ni-56 and Co-56 with half-lives of 6.1 and 77.8 days, respectively. It is shown that the mixing induced by hydrodynamical instabilities occurring during the first few hours is substantially modified at later time by the radioactive decay of Ni-56 and Co-56. The inner cavity of the expanding supernova remnant fills up with nickel, its decay products thus forming a giant 'nickel bubble'. The peak velocity of the nickel increases by approximately 30 percent after the decays. While these results adequately model the core of the observed Fe line profiles, they fail to reproduce the high velocity wings of the spectra. 34 refs.
- Research Organization:
- Harvard-Smithsonian Center for Astrophysics, Cambridge, MA (USA)
- OSTI ID:
- 5544521
- Journal Information:
- Astrophysical Journal; (USA), Vol. 370; ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
Similar Records
Very Deep inside the SN 1987A Core Ejecta: Molecular Structures Seen in 3D
Gamma-ray lines produced by low-energy cosmic rays in SN 1987A
Related Subjects
GENERAL PHYSICS
SUPERNOVAE
COMPUTERIZED SIMULATION
COBALT ISOTOPES
COMPUTER CODES
DECAY
EXPLOSIONS
MAGELLANIC CLOUDS
MAGNETOHYDRODYNAMICS
MIXING
NICKEL ISOTOPES
STABILITY
STAR MODELS
SUPERNOVA REMNANTS
TWO-DIMENSIONAL CALCULATIONS
COSMIC RADIO SOURCES
ERUPTIVE VARIABLE STARS
FLUID MECHANICS
GALAXIES
HYDRODYNAMICS
ISOTOPES
MATHEMATICAL MODELS
MECHANICS
SIMULATION
STARS
VARIABLE STARS
640102* - Astrophysics & Cosmology- Stars & Quasi-Stellar
Radio & X-Ray Sources