Computer Science – Numerical Analysis
Scientific paper
Feb 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980nyasa.336..389b&link_type=abstract
In: Texas Symposium on Relativistic Astrophysics, 9th, Munich, West Germany, December 14-19, 1978, Proceedings. (A80-42502 18-90
Computer Science
Numerical Analysis
5
Neutron Stars, Stellar Evolution, Stellar Magnetic Fields, Stellar Models, Stellar Rotation, Supernovae, Angular Momentum, Approximation, Magnetohydrodynamics, Numerical Analysis, Pulsars, Stellar Envelopes, Thermal Stability
Scientific paper
In order to explain the formation of the neutron star-pulsar as a result of the strong supernovae explosion, a magnetorotational (MGR) model is presented in which the rotational energy of the system transforms into the kinetic energy of the outbursting matter. Attention is given to magnetohydrodynamical calculations made in the one-dimensional cylindrical model. Numerical results show that the transformation coefficient for the change from rotational to radial kinetic energy changes very slowly and the outbursting mass changes very little. It is also noted that the magnetic pressure is important for the MGR explosion, and that in the cylindrical model the finite amount of matter cannot flow to infinity because of the divergence of the cylindrical gravitational potential, thus, the outflowing part of the matter is stored far from the core and performs the MGR oscillations.
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