SPECTRUM OF GALACTIC COSMIC RAYS ACCELERATED IN SUPERNOVA REMNANTS

By V. Ptuskin, V. Zirakashvili, E. Seo. 2010

166 citations recorded by the source corpus.

The spectra of high-energy protons and nuclei accelerated by supernova remnant (SNR) shocks are calculated, taking into account magnetic field amplification and Alfvénic drift both upstream and downstream of the shock for different types of SNRs during their evolution. The maximum energy of accelerated particles may reach 5 × 1018 eV for Fe ions in Type IIb SNRs. The calculated energy spectrum of cosmic rays after propagation through the Galaxy is in good agreement with the spectrum measured at the Earth.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/25fc61e3388676b5ac2b108714784850c4384307

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In Astronomy and Astrophysics

1. P. Blasi
2. A. Bykov
3. E. Amato
4. J. C. Raymond
5. J. Vink
6. J. Rachen
7. A. V. Vliet
8. Y. Ohira

In Nuclear and High Energy Physics

1. P. Blasi
2. A. Bykov
3. E. Amato
4. Kumiko Kotera
5. J. C. Raymond
6. Angela V. Olinto
7. J. Vink
8. J. Rachen

Citations in the corpus

• Diffusive propagation of cosmic rays from supernova remnants in the Galaxy. I: spectrum and chemical composition (2011, background): “As discussed in [9, 10], a qualitatively good fit to the spectra of CRs (including nuclei heavier than hydrogen) can be achieved within the context of NLDSA with finite speed of scattering centers (implying δ ≈ 0.”
• Cosmic-ray energy spectrum and composition up to the ankle - the case for a second Galactic component (2016, background): “This is incompatible with the prediction of di↵usive shock acceleration theory which predicts an index close to 2 for the strong shocks present in supernova remnants (Ptuskin et al. 2010; Caprioli et al. 2011).”
• The origin of galactic cosmic rays (2013, unknown): “Several authors (Ptuskin et al. 2010; Caprioli et al. 2010a; Caprioli 2012) suggested that appreciably steeper spectra may be obtained by assuming fast moving scattering centers in the upstream fluid, but this effect appears to be dependent on rather poorly known characteristics of the waves…”
• Ultra high energy cosmic rays: implications of Auger data for source spectra and chemical composition (2013, background): “The latter case would be favored, as far as particle acceleration is concerned [45].”
• Observational Signatures of Particle Acceleration in Supernova Remnants (2012, background): “Moreover, (Ptuskin et al., 2010) found that remnants of type IIb supernovae should be able to accelerate Fe ions up to 5× 1018 eV and Morlino and Caprioli (2011) 60 modeled the broadband emission of Tycho’s supernova remnant and found that protons were at least accelerated up to 5× 1014 eV.”
• The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, background): “Taking into account magnetic field amplification and Alfvenic drift in shocks of Type IIb SNRs, Ptuskin et al. (2010) find that Galactic cosmic ray iron can reach Emax ∼ 5 EeV, allowing extragalactic cosmic rays to begin to dominate above the ankle.”
• Diffusive propagation of cosmic rays from supernova remnants in the Galaxy. II: anisotropy (2011, background): “Only very recently [6, 8, 9] it has been proposed that steeper spectra might result from phenomenological (and in general not very well justified in terms of basic physical principles) approaches to the problem of determining the velocity of the scattering centers.”