Cosmic-ray acceleration and escape from supernova remnants

Bell, A. R.; Schure, K. M.; Reville, Brian; Giacinti, Gwenael

doi:10.1093/mnras/stt179

Cited by 283 publications

(373 citation statements)

References 63 publications

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“…In order to have an effective amplification of the field, an efficient acceleration of CR hadrons is required [11,12]. This finding received strong observational support with the detection of thin X-ray synchrotron filaments from several SNR shocks.…”

Section: Evidence For Magnetic Field Amplificationmentioning

confidence: 99%

Gamma-ray emission from young supernova remnants: Hadronic or leptonic?

Gabici

Aharonian

2016

EPJ Web of Conferences

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Abstract. The debate on the nature of the gamma-ray emission from young supernova remnants is still open. Ascribing such emission to hadronic rather than leptonic processes would provide an evidence for the acceleration of protons and nuclei, and this fact would fit with the very popular (but not proven) paradigm that supernova remnants are the sources of Galactic cosmic rays. Here, we discuss this issue with a particular focus on the best studied gamma-ray-bright supernova remnant: RX J1713.7-3946.

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Section: Evidence For Magnetic Field Amplificationmentioning

confidence: 99%

Gamma-ray emission from young supernova remnants: Hadronic or leptonic?

Gabici

Aharonian

2016

EPJ Web of Conferences

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“…[25] and [10], starting with a wavenumber k much larger than the particle gyroradius but then forming fluctuations on larger scales allowing resonant scattering, grow in a very short time. This kind of instability may allow to reach the knee if applied to the case of supernovae expanding in the wind of their red super-giant (RSG) progenitor star [11,30], where the highest energies are reached within a few decades after the SN explosion, namely before the beginning of the ST phase of the explosion. The origin of the knee of the all-particle spectrum is a very challenging and a very important issue because it is strongly correlated with the transition between galactic and extragalactic CRs.…”

Section: Introductionmentioning

confidence: 99%

“…In particular, we investigated in detail the implications of the so called Non-Resonant Hybrid (NRH) instability described by Refs. [10,30,11] by computing the maximum energy and the overall particle spectrum produced during the whole SN expansion, both in the ED and ST phases, and comparing it with KASCADE-Grande and ARGO data [15].…”

Section: Introductionmentioning

confidence: 99%

On the cosmic ray spectrum from type II Supernovae expanding in their red giant presupernova wind

Cardillo¹,

Amato²,

Blasi³

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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One of the most important challenges for the largely accepted idea that Galactic CRs are accelerated in SNR shocks is the maximum energy at which particles can be accelerated. The resonant streaming instability, long invoked for magnetic field amplification at shocks, can not provide sufficiently high fields and efficient enough scattering so as to ensure particle acceleration up to the knee. Here we discuss the non-resonant version of this instability which, with its faster growth and larger value of the amplified field, increases the achievable maximum energy. Because of their higher explosion rate, we focus on type II SNe expanding in their red supergiant wind and we find that the transition between Ejecta Dominated (ED) and Sedov-Taylor (ST) phases takes place at very early times. In this environment, the accelerated particle spectrum shows no high energy exponential cut-off but a spectral break at the maximum energy (E M ). Moreover, the maximum energy of protons can easily reach PeV energies. With this model, we tried to fit KASCADEGrande and ARGO -YBJ data but failed to find a parameter combination that can explain both data sets. We discuss the different scenarios implied by the two data sets.

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“…In a variation of this suggestion, the knee is caused by the maximal energy of a single nearby source such as Monogem [5]. While it is very natural to expect that differences in supernovae types and their environments lead to a distribution of reachable maximal rigidities, this proposal does not predict the exact energy of the knee or the strength of the flux suppression, without a better knowledge of CR confinement and escape [6].…”

mentioning

confidence: 97%

Explaining the spectra of cosmic ray groups above the knee by escape from the Galaxy

Giacinti

Kachelrieß²,

Semikoz

2014

Phys. Rev. D

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We investigate the possibility that the cosmic ray (CR) knee is entirely explained by the energydependent CR leakage from the Milky Way. We test this hypothesis calculating the trajectories of individual CRs with energies between E/Z = 10 14 eV and 10 17 eV propagating them in the regular and turbulent Galactic magnetic field. We find a knee-like structure of the CR escape time τesc(E) around E/Z = few × 10 15 eV for a coherence length lc ≃ 2 pc of the turbulent field, while the decrease of τesc(E) slows down around E/Z ≃ 10 16 eV in models with a weak turbulent magnetic field. Assuming that the injection spectra of CR nuclei are power-laws, the resulting CR intensities in such a turbulence are consistent with the energy spectra of CR nuclei determined by KASCADE and KASCADE-Grande. We calculate the resulting CR dipole anisotropy as well as the source rate in this model.

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Cosmic-ray acceleration and escape from supernova remnants

Cited by 283 publications

References 63 publications

Gamma-ray emission from young supernova remnants: Hadronic or leptonic?

Gamma-ray emission from young supernova remnants: Hadronic or leptonic?

On the cosmic ray spectrum from type II Supernovae expanding in their red giant presupernova wind

Explaining the spectra of cosmic ray groups above the knee by escape from the Galaxy

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