Cosmic ray acceleration and escape from supernova remnants

By A. Bell, K. Schure, B. Reville, G. Giacinti. 2013

240 citations recorded by the source corpus.

Galactic cosmic ray (CR) acceleration to the knee in the spectrum at a few PeV is only possible if the magnetic field ahead of a supernova remnant (SNR) shock is strongly amplified by CR escaping the SNR. A model formulated in terms of the electric charge carried by escaping CR predicts the maximum CR energy and the energy spectrum of CR released into the surrounding medium. We find that historical SNR such as Cas A, Tycho and Kepler may be expanding too slowly to accelerate CR to the knee at the present time.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2b4c63167c12742d7ea17b13ed118334f07993ab

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Citations in the corpus

SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. I. ACCELERATION EFFICIENCY (2013, methodology): “A novel approach to DSA exploiting Vlasov–Fokker–Plank simulations has also been recently proposed by Bell et al. (2013); such a method does not include a self-consistent description of the injection physics, but it represents a powerful tool for studying accelerated particles on large scales.”
Interpretation of AMS-02 electrons and positrons data (2014, methodology): “Moreover, fixing a typical magnetic field of B = 30μG (adopted in the following of our analysis) [45, 50, 52–58], and employing Eq.”
THE FIRST FERMI LAT SUPERNOVA REMNANT CATALOG (2015, background): “On a more macroscopic level, ECR,max can depend on the SNR hydrodynamics, namely the shock velocity and size, as well as on the ambient density (Lagage & Cesarsky 1983; Bell & Lucek 2001; Bell 2004; Ptuskin & Zirakashvili 2003, 2005; Blasi et al. 2007; Zirakashvili & Ptuskin 2008; Bell et al. 2013).”
SIMULATIONS OF ION ACCELERATION AT NON-RELATIVISTIC SHOCKS. II. MAGNETIC FIELD AMPLIFICATION (2014, methodology): “For relativistic CRs in the ISM, we have b∗ 3 √ c/vA ≈ 20–30, which means that CRs escaping from a SNR might be able to pre-amplify the ISM field by more than one order of magnitude before being isotropized (see also Bell et al. 2013).”
Massive stars as major factories of Galactic cosmic rays (2018, methodology): “hanicalpowerof thestellarwindsinunitsof 1039 erg/s, andf is the efﬁciency of conversion of the wind kinetic energy to relativistic protons with energy larger than 10 TeV. Substituting R0 = RD into Eq.(3), we obtain f(≥ 10 TeV) ≈ 1w0D30L−1 39 , (6) Eq.(6) provides a direct link between two fundamenta”
Open Questions in Cosmic-Ray Research at Ultrahigh Energies (2019, unknown): “However, whether SNRs are actually able to accelerate up to the knee energy (3 PeV) remains an open question.”
The origin of galactic cosmic rays (2013, unknown): “…consists in a possibly self-consistent scenario in which the highest energy particles (whichever that may be) generate turbulence on the scale of their own Larmor radius, thereby allowing particles of the same energy to return to the shock and sustain DSA (Bell et al. 2013; Reville and Bell 2013).”