Hydrodynamic simulations of the interaction of supernova shock waves with a clumpy environment: the case of the RX J0852.0-4622 (Vela Jr) supernova remnant

Abstract

Observations in all electromagnetic bands show that many supernova remnants (SNRs) have a very aspherical shape. This can be the result of asymmetries in the supernova explosion or a clumpy circumstellar medium. We study the generation of inhomogeneities and the mixing of elements arising from these two sources in multidimensional hydrodynamic simulations of the propagation of a supernova blast wave into a cloudy environment. We model a specific SNR, Vela Jr (RX J0852.0-4622). By comparing our results with recent observations, we can constrain the properties of the explosion. We find that a very energetic explosion of several 10^{51} erg occurring roughly about 800 years ago is consistent with the shape and emission of the SNR, as well as a supernova with an energy closer to the canonical value of 10^{51} erg a few thousand years ago.

arXiv comment18 pages, 13 figures

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Cited by in corpus (11)

• On the Expansion Rate, Age, and Distance of the Supernova Remnant G266.2-1.2 (Vela Jr.)
• Deeper H.E.S.S. observations of Vela Junior (RX J0852.0$-$4622): Morphology studies and resolved spectroscopy
• Impacts of Rotation on Three-dimensional Hydrodynamics of Core-collapse Supernovae
• The turbulent destruction of clouds - III. Three dimensional adiabatic shock-cloud simulations
• Linear Theory of the Rayleigh-Taylor Instability at a Discontinuous Surface of a Relativistic Flow
• Abundance anomalies in metal-poor stars from Population III supernova ejecta hydrodynamics
• Numerical Simulations of a Shock Interacting with Multiple Magnetized Clouds
• Simulating TeV gamma-ray morphologies of shell-type supernova remnants
• The structure of TeV-bright shell-type supernova remnants
• Titanium hidden in dust
• A method for computing synchrotron and inverse-Compton emission from hydrodynamic simulations of supernova remnants