Nonlinear Shock Acceleration and Photon Emission in Supernova Remnants

By D. Ellison, E. Berezhko, M. Baring. 2000

141 citations recorded by the source corpus.

We have extended a simple model of nonlinear diffusive shock acceleration to include the injection and acceleration of electrons and the production of photons from bremsstrahlung, synchrotron, inverse-Compton, and pion-decay processes. We argue that the results of this model, which is simpler to use than more elaborate ones, offer a significant improvement over test-particle, power-law spectra which are often used in astrophysical applications of diffusive shock acceleration. With an evolutionary supernova remnant (SNR) model to obtain shock parameters as functions of ambient interstellar medium parameters and time, we predict broadband continuum photon emission from supernova remnants in general, and SN 1006 in particular, showing that our results compare well with the more complete time-dependent and spherically symmetric nonlinear model of Berezhko, Ksenofontov, & Petukhov. We discuss the implications nonlinear shock acceleration has for X-ray line emission and use our model to describe how ambient conditions determine the TeV/radio flux ratio, an important parameter for γ-ray observations of radio SNRs.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/70b4b87bfd933604e5bf5689ff505b3ec99a86eb

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Citations in the corpus

DISCREPANT HARDENING OBSERVED IN COSMIC-RAY ELEMENTAL SPECTRA (2010, background): “This could result in spectral flattening with increasing cosmic-ray energy and deviations from a pure power law (Ellison et al. 2000).”
Rayleigh-Taylor Instabilities in Young Supernova Remnants Undergoing Efficient Particle Acceleration (2001, background): “Note also that the overall temperature of the shocked gas will be substantially lower if particle acceleration is efficient and compression ratios are large than if little acceleration occurs (e.g., Ellison et al. 2000).”
On the Nature of the Variable Infrared Emission from Sagittarius A* (2004, background): “…of the accelerated particles on the shock structure) typically predict that the spectral index of accelerated particles increases (“hardens”) with increasing energy (e.g., Ellison et al. 2000); as discussed below, this kind of hardening is what we need to account for the observations of Sgr A*.”
DUST PRODUCTION AND PARTICLE ACCELERATION IN SUPERNOVA 1987A REVEALED WITH ALMA (2013, background): “The shock structure is therefore likely being modiﬁed by pressure from the accelerated particles (Ellison et al. 2000) or by an ampliﬁed tangled magnetic ﬁeld (Kirk et al. 1996).”
Small-Scale Structure of the SN 1006 Shock with Chandra Observations (2003, methodology): “We therefore must consider nonlinear effects suggested by Ellison et al. (2000) and by Berezhko et al. (2002); however, a more quantitative scenario including the nonlinear effects must be a future work.”
Reionization by Hard Photons. I. X-Rays from the First Star Clusters (2000, methodology): “Theoretical models of shock acceleration, in which e/p is a free parameter, often set e/p D 1%È5% for consistency with cosmicray experiments (Ellison & Reynolds 1991 ; Ellison et al. 2000).”
Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, unknown): “The heating of the precursor plasma by dissipation of small scale fluctuations modifies the subshock Mach number (e.g., Ellison et al. 2000), and this in turn modifies injection.”
Circumstellar Emission from Type Ib and Ic Supernovae (2006, methodology): “In another model, we include an injection spectrum appropriate to a cosmic-raydominated shock wave, as calculated by Figure 1 from Ellison et al. (2000).”
Analytical solutions for energy spectra of electrons accelerated by nonrelativistic shock-waves in shell type supernova remnants (2006, background): “Over the recent years, several numerical calculations of high energy radia- tion by particles accelerated in young SNRs have been performed with emphasis on the non-linear effects caused by protons and nuclei on the shock structure (see e.g. Ellison et al. 2000, Berezhko and Völk 2004).”