2010A&A...509L..10F


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.01CET20:05:48

2010A&A...509L..10F - Astronomy and Astrophysics, volume 509, L10-10 (2010/1-1)

3D simulations of supernova remnants evolution including non-linear particle acceleration.

FERRAND G., DECOURCHELLE A., BALLET J., TEYSSIER R. and FRASCHETTI F.

Abstract (from CDS):

If a sizeable fraction of the energy of supernova remnant shocks is channeled into energetic particles (commonly identified with Galactic cosmic rays), then the morphological evolution of the remnants must be distinctly modified. Evidence of such modifications has been recently obtained with the Chandra and XMM-Newton X-ray satellites. To investigate these effects, we coupled a semi-analytical kinetic model of shock acceleration with a 3D hydrodynamic code (by means of an effective adiabatic index). This enables us to study the time-dependent compression of the region between the forward and reverse shocks due to the back reaction of accelerated particles, concomitantly with the development of the Rayleigh-Taylor hydrodynamic instability at the contact discontinuity. Density profiles depend critically on the injection level η of particles: for η≲10–4 modifications are weak and progressive, for η∼10–3 modifications are strong and immediate. Nevertheless, the extension of the Rayleigh-Taylor unstable region does not depend on the injection rate. A first comparison of our simulations with observations of Tycho's remnant strengthens the case for efficient acceleration of protons at the forward shock.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - instabilities - cosmic rays - acceleration of particles - methods: numerical

Simbad objects: 2

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Number of rows : 2

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Lupus SN SNR 15 02 22.1 -42 05 49           ~ 1226 1
2 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2471 1

    Equat.    Gal    SGal    Ecl

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2021.03.01-20:05:48

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