Confirmation of strong magnetic field amplification and nuclear cosmic ray acceleration in SN 1006
By E. Berezhko, L. Ksenofontov, H. Völk. 2003
142 citations recorded by the source corpus.
It is shown that the nonlinear kinetic model of cosmic ray (CR) acceleration in supernova remnants (SNRs) fits the shell-type nonthermal X-ray morphology, obtained in Chandra observations, in a satisfactory way. The set of empirical parameters is the same which reproduces the dynamical properties of the SNR and the spectral characteristics of the emission produced by CRs. The extremely small spatial scales of the observed X-ray distribution are due to the large effective magnetic field Bd ∼ 100 µG in the interior, which is also required to give a good fit for the spatially integrated radio and X-ray synchrotron spectra. The only reasonably thinkable condition for the production of such a large effective field strength is an efficiently accel- erated nuclear CR component. Therefore the Chandra data confirm the inference that SN 1006 indeed accelerates nuclear CRs with the high efficiency required for SNRs to be considered as the main Galactic CR sources.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/a2f5ec7646c1a0da31befb6fd22b5c393bb80c6e
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Citations in the corpus
- Radio signature of cosmological structure formation shocks (2006, background): “Cosmic rays with energies up to ∼ 1015eV are presumably accelerated at the shock fronts of supernova remnants (e. g. Berezhko et al. 2003; Vink & Laming 2003).”
- Nonlinear Diffusive Shock Acceleration with Magnetic Field Amplification (2006, background): “…the Berezhko et al. model can easily be missed, particularly since the titles of some of these papers, e.g., ‘‘Confirmation of StrongMagnetic Field Amplification andNuclear Cosmic-Ray Acceleration in SN 1006’’ (Berezhko et al. 2003), might suggest that the model does contain B-field amplification.”
- Cosmic ray acceleration and escape from supernova remnants (2013, background): “…can be raised significantly beyond 0.01PeV, but there remains the question of why the fields are amplified to the observed magnitude, up to 100’s µG in the historical SNR (Vink & Laming 2003, Berezhko et al 2003, Völk et al 2005), and why CR are accelerated to a few PeV rather than 0.1 or 10 PeV.”
- Magnetic field amplification in Tycho and other shell-type supernova remnants (2004, methodology): “8 shows a plot of B2d/(8πρ0V 2 s ) vs.”
- Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “It was soon recognized that these widths indicate high magnetic fields near the shock front (Vink and Laming, 2003; Berezhko et al., 2003a; Bamba et al., 2004; Ballet, 2006).”
- Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays (2004, background): “Fields as large as 1 mG are indicated by radio observations (Longair 1994) in some parts of some young SNR. Recent analysis of the morphology of X-ray emission close to the outer shocks of SN1006 (Berezhko et al. 2003) and Cas A (Vink & Laming 2003) imply that strong magnetic fields are needed for r”
- Superbubbles and energetic particles in the Galaxy. I. Collective effects of particle acceleration (2004, background): “…for large fluctuations of the magnetic field around the SN shock (up to 100 times the ambient field or more; Lucek & Bell 2000; Bell & Luceck 2001; Berezhko et al. 2003; Ptuskin & Zirakashvili 2003) does help to reach energies around or even above the knee (3 × 1015 eV), but the ankle energy…”