Effects of non-uniform interstellar magnetic field on synchrotron X-ray and inverse-Compton gamma-ray morphology of SNRs
arXiv:1011.1847 · doi:10.1051/0004-6361/201015505
Abstract
Observations of SNRs in X-ray and gamma-ray bands promise to contribute with important information in our understanding on the nature of galactic cosmic rays. The analysis of SNRs images collected in different energy bands requires the support of theoretical modeling of synchrotron and inverse Compton (IC) emission. We develop a numerical code (REMLIGHT) to synthesize, from MHD simulations, the synchrotron radio, X-ray and IC gamma-ray emission from SNRs expanding in non-uniform interstellar medium (ISM) and/or non-uniform interstellar magnetic field (ISMF). As a first application, the code is used to investigate the effects of non-uniform ISMF on the SNR morphology in the non-thermal X-ray and gamma-ray bands. We perform 3D MHD simulations of a spherical SNR shock expanding through a magnetized ISM with a gradient of ambient magnetic field strength. The model includes an approximate treatment of upstream magnetic field amplification and the effect of shock modification due to back reaction of accelerated cosmic rays. From the simulations, we synthesize the synchrotron radio, X-ray and IC gamma-ray emission with REMLIGHT, making different assumptions about the details of acceleration and injection of relativistic electrons. A gradient of the ambient magnetic field strength induces asymmetric morphologies in radio, X-ray and gamma-ray bands independently from the model of electron injection if the gradient has a component perpendicular to the line-of-sight. The degree of asymmetry of the remnant morphology depends on the details of the electron injection and acceleration and is different in the radio, X-ray, and gamma-ray bands. The non-thermal X-ray morphology is the most sensitive to the gradient, showing the highest degree of asymmetry. The IC gamma-ray emission is weakly sensitive to the non-uniform ISMF, the degree of asymmetry of the SNR morphology being the lowest in this band.
16 pages, 13 Figures; accepted for publication on A&A. Version with full resolution images can be found at http://www.astropa.unipa.it/~orlando/PREPRINTS/sorlando_15505.pdf
References in corpus (10)
- Primary particle acceleration above 100 TeV in the shell-type Supernova Remnant RX J1713.7-3946 with deep H.E.S.S. observations
- H.E.S.S. observations of the supernova remnant RX J0852.0-4622: shell-type morphology and spectrum of a widely extended VHE gamma-ray source
- First detection of VHE gamma-rays from SN 1006 by H.E.S.S
- On the Origin of Asymmetries in Bilateral Supernova Remnants
- Evidence of a Curved Synchrotron Spectrum in the Supernova Remnant SN 1006
- Diffusive Shock Acceleration in Test-Particle Regime
- Simulation of the growth of the 3D Rayleigh-Taylor instability in Supernova Remnants using an expanding reference frame
- Aspect angle for interstellar magnetic field in SN 1006
- Hadronic versus leptonic origin of the gamma-ray emission from Supernova Remnant RX J1713.7-3946
- Some properties of synchrotron radio and inverse-Compton gamma-ray images of supernova remnants
Cited by in corpus (15)
- Role of ejecta clumping and back-reaction of accelerated cosmic rays in the evolution of Type Ia supernova remnants
- 3D MHD modeling of the expanding remnant of SN 1987A. Role of magnetic field and non-thermal radio emission
- Evidence for past interaction with an asymmetric circumstellar shell in the young SNR Cassiopeia A
- Constraints on local interstellar magnetic field from non-thermal emission of SN1006
- 3D Simulations of the Thermal X-ray Emission from Young Supernova Remnants Including Efficient Particle Acceleration
- Electron and Ion Acceleration in Relativistic Shocks with Applications to GRB Afterglows
- Observational constraints on the modeling of SN1006
- Modeling the shock-cloud interaction in SN 1006: unveiling the origin of nonthermal X-ray and gamma-ray emission
- Post-adiabatic supernova remnants in an interstellar magnetic field: oblique shocks and non-uniform environment
- Radio, X-ray and gamma-ray surface brightness profiles as powerful diagnostic tools for non-thermal SNR shells
- Radio polarization maps of shell-type SNRs II. Sedov models with evolution of turbulent magnetic field
- Hadronic gamma-ray images of Sedov supernova remnants
- Modeling particle acceleration and non-thermal emission in supernova remnants
- Tree-based solvers for adaptive mesh refinement code FLASH -- IV: An X-ray radiation scheme to couple discrete and diffuse X-ray emission sources to the thermochemistry of the interstellar medium
- Long-term evolution of a supernova remnant hosting a double neutron star binary