Supernova Remnant Crossing a Density Jump: A Thin Shell Model

Abstract

The environments of supernova explosion are often inhomogeneous and there may be jumps in their density structure. We have developed a semi-analytic model under the thin-shell approximation for supernova remnants that evolve crossing a density jump in the ambient medium. The generic evolutionary relations are presented for the blast wave after impacting on a cavity wall, which may be produced by the energetic stellar wind from the supernova progenitor. The relations can also be extended to the case that the blast waves break out from a dense cloud if different density contrast is used. This model is applied to N132D, a well-known cavity-born supernova remnant whose evolution has not yet been quantitively estimated in a cavity scenario due to lack of model formulae, and self-consistent physical parameters are obtained.

aastex, 20 pages (including 6 figures), to appear in the v595 n1 ApJ Sep. 20, 2003 issue, a reference added and a few typos corrected

References in corpus (1)

• High-resolution X-ray spectroscopy and imaging of supernova remnant N132D

Cited by in corpus (22)

• Linear relation for wind-blown bubble sizes of main-sequence OB stars in a molecular environment and implication for supernova progenitors
• The 3D Structure of N132D in the LMC: A Late-Stage Young Supernova Remnant
• Chandra view of Kes 79: a nearly isothermal SNR with rich spatial structure
• Discovery of molecular shells associated with supernova remnants. (II) Kesteven 75
• The Thermal Composite Supernova Remnant Kes 27 as Viewed by CHANDRA: Shock Reflection from a Cavity Wall
• Discovery of Molecular Shells Associated with Supernova Remnants. I. Kesteven 69
• Fermi-LAT Observations of Supernova Remnant Kesteven 79
• Three-Dimensional Kinematic Reconstruction of the Optically-Emitting, High-Velocity, Oxygen-Rich Ejecta of Supernova Remnant N132D
• The Metal-enriched Thermal Composite Supernova Remnant Kesteven 41 (G337.8-0.1) in a Molecular Environment
• ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large Magellanic Cloud: Possible Evidence for Shocked Molecular Clouds Illuminated by Cosmic-Ray Protons
• Interaction between the Supernova Remnant HB 3 and the Nearby Star-Forming Region W3
• Molecular Environments of SNRs
• Spatially Resolved Chandra Spectroscopy of the Large Magellanic Cloud Supernova Remnant N132D
• Plasma Diagnostics of the Supernova Remnant N132D Using Deep XMM-Newton Observations with the Reflection Grating Spectrometer
• LMC N132D: A mature supernova remnant with a power-law gamma-ray spectrum extending beyond 8 TeV
• A Preliminary Chandra X-ray Spectroscopy of the Supernova Remnant N132D
• HST Proper Motion Measurements of Supernova Remnant N132D: Center of Expansion and Age
• Energy Conservation in the thin layer approximation: I. The spherical classic case for supernovae remnants
• Measurement of the Forward Shock Velocities of the Supernova Remnant N132D Based on the Thermal X-ray Emission
• XMM-Newton Observations of the High Temperature Plasma in the Large Magellanic Cloud Supernova Remnant N132D
• Chandra and XMM-Newton X-ray Study on the Core-collapse Supernova Remnant N63A in an H II Region
• Energy Conservation in the thin layer approximation: II. The asymmetric classic case for supernovae remnants