Multiwavelength Spectral Models for SNR G347.3-0.5 from Non-Linear Shock Acceleration
arXiv:astro-ph/0503079 · doi:10.1016/j.asr.2005.02.067
Abstract
The remnant G347.3-0.5 exhibits strong shell emission in the radio and X-ray bands, and has a purported detection in the TeV gamma-ray band by the CANGAROO-II telescope. The CANGAROO results were touted as evidence for the production of cosmic ray ions, a claim that has proven controversial due to constraining fluxes associated with a proximate unidentified EGRET source 3EG J1714-3857. HESS has now seen this source in the TeV band. The complex environment of the remnant renders modeling of its broadband spectrum sensitive to assumptions concerning the nature and parameters of the circumremnant medium. This paper explores a sampling of reasonable possibilities for multiwavelength spectral predictions from this source, using a non-linear model of diffusive particle acceleration at the shocked shell. The magnetic field strength, shell size and degree of particle cross-field diffusion act as variables to which the radio to X-ray to gamma-ray signal is sensitive. The modeling of the extant data constrains these variables, and the potential impact of the recent HESS detection on such parameters is addressed. Putative pion decay signals in hard gamma-rays resulting from hadronic interactions in dense molecular clouds are briefly discussed; the requisite suppression of the GeV component needed to accommodate the 3EG J1714-3857 EGRET data provides potential bounds on the diffusive distance from the shell to the proximate clouds.
arXiv comment13 pages, 2 embedded figures, Advances Space Research, in press
References in corpus (21)
- High-energy particle acceleration in the shell of a supernova remnant
- X-Ray Emission From the Shell-Type SNR G347.3-0.5
- Discovery of Non Thermal X-Rays from the Northwest Shell of the New SNR RX J1713.7-3946: The Second SN1006 ?
- Evidence for TeV gamma ray emission from Cassiopeia A
- Discovery of TeV Gamma Rays from SN1006: Further Evidence for the SNR Origin of Cosmic Rays
- Radio to Gamma-Ray Emission from Shell-type Supernova Remnants: Predictions from Non-linear Shock Acceleration Models
- Nonlinear Shock Acceleration and Photon Emission in Supernova Remnants
- A semi-analytical approach to non-linear shock acceleration
- XMM-Newton observations of the supernova remnant RX J1713.7-3946 and its central source
- Thermal X-ray Emission and Cosmic Ray Production in Young Supernova Remnants
- Gamma-ray production in supernova remnants
- A High-Resolution Study of Nonthermal Radio and X-Ray Emission from SNR G347.3-0.5
- Analytic solution for nonlinear shock acceleration in the Bohm limit
- Non-linear Particle Acceleration in Oblique Shocks
- Broad-band Observations and Modeling of the Shell-Type Supernova Remnant G347.3-0.5
- Nonlinear Particle Acceleration at Reverse Shocks in Supernova Remnants
- Diffusive Shock Acceleration Simulations: Comparison with Particle Methods and Bow Shock Measurements
- No evidence yet for hadronic TeV gamma-ray emission from SNR RX J1713.7-3946
- Supernova-Remnant Origin of Cosmic Rays?
- Upper limits to the SN1006 multi-TeV gamma-ray flux from H.E.S.S. observations
- Supernova Remnants and Plerions in the Compton Gamma-Ray Observatory Era
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- Electrostatic Potentials in Supernova Remnant Shocks
- Topical Issues for Particle Acceleration Mechanisms in Astrophysical Shocks