Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Berezhko, E. G.; Völk, H. J.

doi:10.1051/0004-6361/200913312

Cited by 39 publications

(42 citation statements)

References 36 publications

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“…However, Ellison et al (2010) argue that if the TeV γ -ray emission were hadronic in origin, thermal X-ray emission would be detected, though the model used there is for a constant ambient medium density of 0.2 cm −3 , for the hadronic scenario. In the model developed by Berezhko & Völk (2010), the SNR blast wave has been expanding through a low-density (n H ≈ 0.0008 cm −3 ) bubble and has recently encountered the bubble wall, with n H = 0.25 cm −3 at present. From their model, we estimate that the shock began encountering the bubble wall ∼800 years ago, as determined by the curve for N g in the top panel of their Figure 1 (Berezhko & Völk 2010).…”

Section: Comparisons To Recent Calculations For Limits On the Thermalmentioning

confidence: 99%

“…From their model, we estimate that the shock began encountering the bubble wall ∼800 years ago, as determined by the curve for N g in the top panel of their Figure 1 (Berezhko & Völk 2010). They assume that the thermal X-ray emission as determined for the Sedov solution by Hamilton et al (1983) is reduced by an amount equivalent to the ratio of the bubble emission measure to the Sedov emission measure, here equal to 0.46 (Berezhko & Völk 2010). Additionally, they assume a value of η = 8 × 10 49 , where η = n 2 E SN (Hamilton et al 1983).…”

Section: Comparisons To Recent Calculations For Limits On the Thermalmentioning

confidence: 99%

“…Their chosen value of η corresponds to an explosion energy of 1.3 × 10 51 erg and an ambient medium density of 0.25 cm −3 . They use the value of η and an assumed electron temperature of 1 keV to estimate the thermal X-ray emission from the recently shocked bubble wall, and they find that, at 1 keV, the thermal X-ray emission is approximately half the nonthermal flux (Berezhko & Völk 2010).…”

Section: Comparisons To Recent Calculations For Limits On the Thermalmentioning

confidence: 99%

“…We find that the results differ, mainly at lower energies. Finally in Section 4, we discuss the recent result by Berezhko & Völk (2010) and show that the absence of thermal X-ray emission does not naturally lead to the interpretation that the TeV gamma-ray emission is hadronic in origin. We argue that if the blast wave has only recently hit the circumstellar shell, then the shocked gas, though at X-ray-emitting temperatures, will be underionized.…”

Section: Introductionmentioning

confidence: 99%

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The Role of Diffusive Shock Acceleration on Nonequilibrium Ionization in Supernova Remnant Shocks. Ii. Emitted Spectra

Patnaude

Slane

Raymond

et al. 2010

ApJ

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We present a grid of nonequilibrium ionization models for the X-ray spectra from supernova remnants undergoing efficient diffusive shock acceleration. The calculation follows the hydrodynamics of the blast wave as well as the time-dependent ionization of the plasma behind the shock. The ionization state is passed to a plasma emissivity code to compute the thermal X-ray emission, which is combined with the emission from nonthermal synchrotron emission to produce a self-consistent model for the thermal and nonthermal emission from cosmic-ray dominated shocks. We show how plasma diagnostics such as the G -ratio of He-like ions, defined as the ratio of the sum of the intercombination, forbidden, and satellite lines to the resonance line, can vary with acceleration efficiency, and discuss how the thermal X-ray emission, when the time-dependent ionization is not calculated self-consistently with the hydrodynamics, can differ from the thermal X-ray emission from models which do account for the hydrodynamics. Finally, we compare the thermal X-ray emission from models which show moderate acceleration (∼35%) to the thermal X-ray emission from test-particle models.

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Section: Comparisons To Recent Calculations For Limits On the Thermalmentioning

confidence: 99%

Section: Comparisons To Recent Calculations For Limits On the Thermalmentioning

confidence: 99%

Section: Comparisons To Recent Calculations For Limits On the Thermalmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

The Role of Diffusive Shock Acceleration on Nonequilibrium Ionization in Supernova Remnant Shocks. Ii. Emitted Spectra

Patnaude

Slane

Raymond

et al. 2010

ApJ

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“…The nonthermal emission of these remnants has a welldefined shell structure and there is evidence that the relative mean thickness of the emitting shell varies from remnant to remnant (Aharonian et al 2006. Previously 1D modeling of particle acceleration in SNRs has been used to study the radial brightness profile in the hadronic scenario (Berezhko & Völk 2010). A detailed study of the source structure with magnetohydrodynamic (MHD) simulations has not been carried out.…”

Section: Introductionmentioning

confidence: 99%

The structure of TeV-bright shell-type supernova remnants

Yang

Liu

Fang

et al. 2014

A&A

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Aims. Two-dimensional magnetohydrodynamic (MHD) simulations are used to model the emission properties of TeV-bright shelltype supernova remnants (SNRs) and to explore their nature. Methods. In the leptonic scenario for the TeV emission, the γ-ray emission is produced via inverse Compton scattering of background soft photons by high-energy electrons accelerated by the shocks of the SNRs. In a previous paper, we showed that since the energy densities of the cosmic microwave background radiation and that of the IR/optical background photons are much higher than that of the photons produced by the same high-energy electrons via the synchrotron process, the observed correlation between X-ray and TeV brightness of SNR RX J1713.7-3946 can be readily explained with the assumption that the energy density of relativistic electrons is proportional to that of the magnetic field. The TeV emissivity is therefore proportional to the magnetic field energy density and MHD simulations can be used to model the TeV structure of such remnants directly. Two-dimensional MHD simulations for SNRs are then performed under the assumption that the ambient interstellar medium is turbulent with the magnetic field and density fluctuations, following a Kolmogorov-like power-law spectrum. Results. (1) As expected, these simulations confirm early 1D and 2D modelings of these sources, namely the hydrodynamical evolution of the shock waves and amplification of magnetic field by Rayleigh-Taylor convective flows and by shocks propagating in a turbulent medium; (2) we reproduce rather complex morphological structure for γ-rays, for example, the bright thin rim and significant asymmetry, suggesting intrinsic variations of the source morphology not related to the structure of the progenitor and environment; and (3) the observed radial profile of several remnants are well reproduced with an ambient medium density of 0.1−1 cm −3 . An even lower ambient density leads to a sharper drop of the TeV brightness with radius than what is observed near the outer edge of these remnants. Conclusions. In a turbulent background medium, we can reproduce the observed characteristics of several shell-type TeV SNRs with reasonable parameters except for a higher ambient density than that inferred from X-ray observations.

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Observational Signatures of Particle Acceleration in Supernova Remnants

Helder¹,

Vink²,

Bykov³

et al. 2012

Particle Acceleration in Cosmic Plasmas

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We evaluate the current status of supernova remnants as the sources of Galactic cosmic rays. We summarize observations of supernova remnants, covering the whole electromagnetic spectrum and describe what these observations tell us about the acceleration processes by high Mach number shock fronts. We discuss the shock modification by cosmic rays, the shape and maximum energy of the cosmic-ray spectrum and the total energy budget of

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Nonthermal and thermal emission from the supernova remnant RX J1713.7-3946

Cited by 39 publications

References 36 publications

The Role of Diffusive Shock Acceleration on Nonequilibrium Ionization in Supernova Remnant Shocks. Ii. Emitted Spectra

The Role of Diffusive Shock Acceleration on Nonequilibrium Ionization in Supernova Remnant Shocks. Ii. Emitted Spectra

The structure of TeV-bright shell-type supernova remnants

Observational Signatures of Particle Acceleration in Supernova Remnants

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