The radio dynamical evolution of young supernova remnants

Details The radio dynamical evolution of young supernova remnants The radio dynamical evolution of young supernova remnants

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224..477s&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 1, 1978, p. 477-487.

Astronomy and Astrophysics

Astronomy

14

Galactic Evolution, Magnetohydrodynamic Stability, Nebulae, Radio Sources (Astronomy), Supernova Remnants, Taylor Instability, High Energy Electrons, Interstellar Magnetic Fields, Momentum Transfer, Particle Interactions, Radiant Flux Density, Stellar Mass Ejection

Scientific paper

Numerical models of young supernova remnants (SNRs) are calculated using a spherically symmetric magnetohydrodynamic code to determine the effects of Rayleigh-Taylor instabilities on the radio properties of young SNRs. The instabilities arise from the deceleration of the remnant as it moves through an inhomogeneous medium. After accounting for momentum interactions, the resultant energy of the instability is sufficient to amplify ambient magnetic fields to strengths comparable to those found in young SNRs. The effects of varying the initial explosion energy, mass ejected, and interstellar density on the flux and surface brightness are investigated. Under the assumption that a supply of relativistic electrons is present, the temporal evolution of the flux density and surface brightness has been calculated. Graphs of surface brightness versus remnant radius are also presented, and the dynamical evolution of the radio shell is investigated as a function of the initial parameters.

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