Nonlinear theory of diffusive acceleration of particles by shock waves

By M. Malkov, L. Drury. 2001

707 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/602869a97abeec4566c4d4fe2c45565c7962a73d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. A. Spitkovsky
2. D. Caprioli
3. P. Blasi
4. L. Sironi
5. A. Bykov
6. D. Ellison
7. G. Morlino
8. E. Orlando

In Nuclear and High Energy Physics

1. A. Spitkovsky
2. D. Caprioli
3. P. Blasi
4. L. Sironi
5. A. Bykov
6. D. Ellison
7. G. Morlino
8. E. Orlando

Citations in the corpus

• Non-linear particle acceleration at non-relativistic shock waves in the presence of self-generated turbulence (2006, background): “…that the temperature of the downstream gas is expected to be lower than predicted through the usual RankineHugoniot relations at an unmodified shock front (see Drury (1983); Blandford & Eichler (1987); Jones & Ellison (1991); Malkov & Drury (2001) for reviews on different aspects of the subject).”
• Analytical solutions for energy spectra of electrons accelerated by nonrelativistic shock-waves in shell type supernova remnants (2006, background): “Although the basic concepts of diffusive shock acceleration are deeply studied and well understood (see e.g. Malkov and Drury 2001), many important details remain unexplored.”
• Cosmological Shock Waves and Their Role in the Large-Scale Structure of the Universe (2003, background): “At the same time, due to incomplete plasma thermalization at collisionless shocks, a sizeable portion of the shock energy can be converted into cosmic ray (CR) energy (mostly ionic) via diffusive shock acceleration (DSA) (for reviews, see, e.g., Blandford & Eichler 1987; Malkov & Drury 2001).”
• SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. II. MAGNETIC FIELD AMPLIFICATION (2014, background): “Even if the shock modification induced by CRs is prominent, in our simulations we do not expect CR spectra to become (A color version of this figure is available in the online journal.) visibly concave as predicted by the nonlinear DSA theory (see, e.g., Malkov & Drury 2001).”
• Relativistic Shocks: Particle Acceleration and Magnetization (2015, background): “…shocks is believed to be responsible for the production of non-thermal distributions of energetic particles in many astronomical systems (Blandford and Eichler 1987; Malkov and Drury 2001, but see, e.g. Arons and Tavani (1994) for a discussion of alternative shock acceleration processes).”
• NONTHERMAL RADIATION OF YOUNG SUPERNOVA REMNANTS: THE CASE OF RX J1713.7−3946 (2010, background): “Over the last 30 years a significant progress has been achieved in the development of theoretical models and understanding of the basic features of DSA (see, e.g., Malkov & Drury 2001 for a review).”
• On the spectrum of high-energy cosmic rays produced by supernova remnants in the presence of strong cosmic-ray streaming instability and wave dissipation (2004, background): “[Using the test particle approximation for not modified shock, Drury et al. (2003) found that the spectrum of accelerated particles is somewhat steeper if the diffusion coefficient is increasing with time compared to the case of constant D.”
• ROLE OF LINE-OF-SIGHT COSMIC-RAY INTERACTIONS IN FORMING THE SPECTRA OF DISTANT BLAZARS IN TeV GAMMA RAYS AND HIGH-ENERGY NEUTRINOS (2010, background): “…(Aharonian et al. 2006b; Mazin & Raue 2007; Finke & Razzaque 2009), combined with much harder intrinsic spectra of distant blazars (Stecker et al. 2007) than those predicted by earlier models (Peacock 1981; Kirk & Schneider 1987; Heavens & Drury 1988; Bednarz & Ostrowski 1998; Malkov & Drury 2001).”
• Superbubbles and energetic particles in the Galaxy. I. Collective effects of particle acceleration (2004, background): “Non linear effects have also been taken into account, to improve on the test-particle treatment of diffusive shock acceleration (e.g. Ellison 2001; Malkov & Drury 2001).”
• On the role of injection in kinetic approaches to non‐linear particle acceleration at non‐relativistic shock waves (2005, background): “Detailed discussions of the current status of the investigations can be found in some excellent reviews (Drury 1983; Blandford & Eichler 1987; Berezhko & Krimsky 1988; Jones & Ellison 1991; Malkov & Drury 2001).”