Modeling supernova remnants: effects of diffusive cosmic-ray acceleration on the evolution, application to observations

Abstract

We present numerical models for supernova remnant evolution, using a new version of the hydrodynamical code SUPREMNA. We added cosmic ray diffusion equation to the code scheme, employing two-fluid approximation. We investigate the dynamics of the simulated supernova remnants with different values of cosmic ray acceleration efficiency and diffusion coefficient. We compare the numerical models with observational data of Tycho's and SN1006 supernova remnants. We find models which reproduce the observed locations of the blast wave, contact discontinuity, and reverse shock for the both remnants, thus allowing us to estimate the contribution of cosmic ray particles into total pressure and cosmic-ray energy losses in these supernova remnants. We derive that the energy losses due to cosmic rays escape in Tycho's supernova remnant are 10-20% of the kinetic energy flux and 20-50% in SN1006.

9 pages, 6 figures, A&A accepted

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• Supernova remnants: the X-ray perspective
• Observational signatures of particle acceleration in supernova remnants
• Three-dimensional numerical investigations of the morphology of type Ia SNRs
• Shock Corrugation by Rayleigh-Taylor Instability in GRB Afterglow Jets
• 3D Simulations of the Thermal X-ray Emission from Young Supernova Remnants Including Efficient Particle Acceleration
• 3D simulations of the non-thermal broad-band emission from young supernova remnants including efficient particle acceleration
• Exploring the Gamma-Ray Emissivity of Young Supernova Remnants I: Hadronic Emission
• Parametric studies of cosmic ray acceleration in supernova remnants
• Time Evolution of the Reverse Shock in SN 1006
• Distance Estimate of Tycho's SNR
• The Advanced X-ray Imaging Satellite
• Oxygen emission in remnants of thermonuclear supernovae as a probe for their progenitor system
• Radio afterglow of magnetars' giant flares