Radio dynamical evolution of young supernova remnants

Journal Article · Fri Sep 01 04:00:00 EDT 1978 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/156395· OSTI ID:6879548

Shirkey, R C

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 yound 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.

• Research Organization: Department of Astronomy, State University of New York at Albany
• OSTI ID: 6879548
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 224:2; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC RADIO SOURCES
FLUID MECHANICS
FORCE-FREE MAGNETIC FIELDS
HYDRODYNAMICS
INSTABILITY
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
MECHANICS
RAYLEIGH-TAYLOR INSTABILITY
STAR ACCRETION
STAR EVOLUTION
SUPERNOVA REMNANTS