Magnetic Field Amplification and Rapid Time Variations in SNR RX J1713.7-3946

Ellison, Donald C.; Vladimirov, Andrey

doi:10.1086/527359

Cited by 35 publications

(33 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…the minimum of E size max and E age max ) is lower than the previous estimate of Bell & Lucek (2001), E p max ∼ 3 × 10 17 eV. Moreover, we did not take into account the nonlinear effects recently pointed out by Ellison & Vladimirov (2008), which could further reduce E p max . However, it is likely that SN 1993J has accelerated protons above 3 × 10 15 eV, i.e.…”

Section: Sn 1993j and The Origin Of Cosmic Raysmentioning

confidence: 73%

Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J

Tatischeff¹

2009

A&A

105

View full text Add to dashboard Cite

Aims. The extensive observations of the supernova SN 1993J at radio wavelengths make this object a unique target for the study of particle acceleration in a supernova shock. Methods. To describe the radio synchrotron emission we use a model that couples a semianalytic description of nonlinear diffusive shock acceleration with self-similar solutions for the hydrodynamics of the supernova expansion. The synchrotron emission, which is assumed to be produced by relativistic electrons propagating in the postshock plasma, is worked out from radiative transfer calculations that include the process of synchrotron self-absorption. The model is applied to explain the morphology of the radio emission deduced from high-resolution VLBI imaging observations and the measured time evolution of the total flux density at six frequencies.Results. Both the light curves and the morphology of the radio emission indicate that the magnetic field was strongly amplified in the blast wave region shortly after the explosion, possibly via the nonresonant regime of the cosmic-ray streaming instability operating in the shock precursor. The amplified magnetic field immediately upstream from the subshock is determined to be B u ≈ 50(t/1 day) −1 G. The turbulent magnetic field was not damped behind the shock but carried along by the plasma flow in the downstream region. Cosmicray protons were efficiently produced by diffusive shock acceleration at the blast wave. We find that during the first ∼8.5 years after the explosion, about 19% of the total energy processed by the forward shock was converted to cosmic-ray energy. However, the shock remained weakly modified by the cosmic-ray pressure. The high magnetic field amplification implies that protons were rapidly accelerated to energies well above 10 15 eV. The results obtained for this supernova support the scenario that massive stars exploding into their former stellar wind are a major source of Galactic cosmic-rays of energies above ∼10 15 eV. We also calculate the flux from SN 1993J of gamma-rays arising from collisions of accelerated cosmic rays with ambient material and the result suggests that type II supernovae could be detected in π 0 -decay gamma-rays with the Fermi Gamma-ray Space Telescope out to a maximum distance of only ∼1 Mpc.

show abstract

Section: Sn 1993j and The Origin Of Cosmic Raysmentioning

confidence: 73%

Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J

Tatischeff¹

2009

A&A

105

View full text Add to dashboard Cite

show abstract

“…[9], E p,max ∼ 3 × 10 17 eV. Moreover, we did not take into account the nonlinear effects recently pointed out by Ellison & Vladimirov [31], which could further reduce E p,max . However, SN 1993J may well have accelerated protons above the knee energy of 3 × 10 15 eV (Fig.…”

Section: Pos(supernova)028mentioning

confidence: 99%

“…These authors have derived an upper limit of ∼ 8 × 10 14 eV on the maximum proton energy, E p,max , and have suggested that an additional CR component is required to explain the CR data above the knee energy. Recently, Ellison & Vladimirov [31] have pointed out that the average magnetic field that determines the maximum proton energy can be substantially less than the field that determines the maximum electron energy. This is because electrons remain in the vicinity of the shock where the magnetic field can be strongly amplified, whereas protons of energies E p > E e,max diffuse farther in the shock precursor region where the field is expected to be weaker (E p,max > E e,max because radiation losses affect the electrons only).…”

Section: Pos(supernova)028mentioning

confidence: 99%

See 1 more Smart Citation

Cosmic-ray acceleration in supernova remnants

Tatischeff¹

2008

Proceedings of Supernovae: Lights in the Darkness — PoS(SUPERNOVA)

View full text Add to dashboard Cite

Galactic cosmic rays are widely believed to be accelerated in expanding shock waves initiated by supernova explosions. The theory of diffusive shock acceleration of cosmic rays is now well established, but two fundamental questions remain partly unanswered: what is the acceleration efficiency, i.e. the fraction of the total supernova energy converted to cosmic-ray energy, and what is the maximum kinetic energy achieved by particles accelerated in supernova explosions? Recent observations of supernova remnants, in X-rays with the Chandra and XMM-Newton satellites and in very-high-energy γ rays with several ground-based atmospheric Cerenkov telescopes, have provided new pieces of information concerning these two questions. After a review of these observations and their current interpretations, I show that complementary information on the diffusive shock acceleration process can be obtained by studying the radio emission from extragalactic supernovae. As an illustration, a nonlinear model of diffusive shock acceleration is applied to the radio light curves of the supernova SN 1993J, which exploded in the nearby galaxy M81. The results of the model suggest that most of the Galactic cosmic rays may be accelerated during the early phase of interaction between the supernova ejecta and the wind lost from the progenitor star.

show abstract

“…The γ-ray spectrum of a single pulsar is preferred to be explained by a leptonic model rather than hadronic one [28]. The spectral index of γ-ray produced from pion-decay emission [55] of hadronic interactions should be harder than that through the Inverse-Compton scattering by leptons in a pulsar. Observation of RX J1713.7-3946 supports the latter one.…”

Section: A Astro-physical Backgroundmentioning

confidence: 99%

Dark Matter Search in Space: Combined Analysis of Cosmic-Ray Antiproton-to-proton Flux Ratio and Positron Flux Measured by AMS-02

Feng

Zhang

2018

ApJ

View full text Add to dashboard Cite

Dark matter search in space has been carried out for many years. Measurements of cosmic ray photons, charged antiparticles and neutrinos are useful tools for dark matter indirect search. The antiparticle energy spectra of cosmic rays have several exciting features such as the unexpected positron excess at E ∼ 10 -500 GeV and the remarkably flattening antiproton/proton at E ∼ 60-450 GeV precisely measured by the AMS-02 experiment, which can not be explained simultaneously by secondary production in interstellar medium. In this work, we report a combined analysis of cosmic ray antiproton and positron spectra arising from dark matter on the top of a secondary production in a spatial-dependent propagation model. We discuss the systematic uncertainties from antiproton production cross section using the two latest Monte Carlo generators, i.e. EPOS LHC and QGSJET-II-04m, respectively. We compare their results. In the case of EPOS LHC, we find that the dark matter pair annihilating into τ leptons channel with 100% branching ratio and p-wave annihilation cross section assumption is the only possible one channel scenario to explain data. On the other hand, there is not a single possible channel in the case of QGSJET-II-04m. We also propose possible two-channel scenarios based on these two Monte Carlo generators.

show abstract

Magnetic Field Amplification and Rapid Time Variations in SNR RX J1713.7-3946

Cited by 35 publications

References 22 publications

Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J

Radio emission and nonlinear diffusive shock acceleration of cosmic rays in the supernova SN 1993J

Cosmic-ray acceleration in supernova remnants

Dark Matter Search in Space: Combined Analysis of Cosmic-Ray Antiproton-to-proton Flux Ratio and Positron Flux Measured by AMS-02

Contact Info

Product

Resources

About