The multi-band non-thermal emission from the supernova remnant RX J1713.7−3946

Fang, Jun; Zhang, L.; Zhang, J. F.; Tang, Yonghui; Yu, Hang

doi:10.1111/j.1365-2966.2008.14128.x

Cited by 21 publications

(24 citation statements)

References 34 publications

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“…Its TeV emission (between ∼100 GeV and ∼10 TeV) has been extensively studied by several groups [5][6][7][8][9][10][11][12][13], who have investigated two different scenarios: besides the hadronic scenario outlined above, also the inverse Compton scattering of the relativistic electrons responsible for the X-ray synchrotron emission may produce a similar signature in the TeV band (leptonic scenario). Each scenario shows strong points and apparent shortcomings, with theorists waiting for Fermi's advent in order to discriminate between them [5][6][7][8][9][10][11][12][13]. The γ-ray spectrum between ∼100 MeV and ∼10 GeV (hereafter the GeV band) is in fact expected to be significantly flatter in the leptonic scenario with respect to the hadronic one.…”

Section: Supernova Remnants Cosmic Rays and Gamma-ray Emissionmentioning

confidence: 99%

Understanding hadronic gamma-ray emission from supernova remnants

Caprioli¹

2011

J. Cosmol. Astropart. Phys.

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Abstract. We aim to test the plausibility of a theoretical framework in which the gamma-ray emission detected from supernova remnants may be of hadronic origin, i.e., due to the decay of neutral pions produced in nuclear collisions involving relativistic nuclei. In particular, we investigate the effects induced by magnetic field amplification on the expected particle spectra, outlining a phenomenological scenario consistent with both the underlying Physics and the larger and larger amount of observational data provided by the present generation of gamma experiments, which seem to indicate rather steep spectra for the accelerated particles. In addition, in order to study to study how pre-supernova winds might affect the expected emission in this class of sources, the time-dependent gamma-ray luminosity of a remnant with a massive progenitor is worked out. Solid points and limitations of the proposed scenario are finally discussed in a critical way.

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Section: Supernova Remnants Cosmic Rays and Gamma-ray Emissionmentioning

confidence: 99%

Understanding hadronic gamma-ray emission from supernova remnants

Caprioli¹

2011

J. Cosmol. Astropart. Phys.

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“…On the other hand, the electron temperature could be much lower than the ion temperature in the shock downstream (Zirakashvili & Aharonian 2010). Morlino et al (2009) and Fang et al (2009) have argued that the density in the downstream can be as high as 0.5 cm −3 , corresponding to a mass density of 8.4 × 10 −25 g cm −3 .…”

Section: Density and Turbulence Generationmentioning

confidence: 99%

Stochastic electron acceleration in the TeV supernova remnant RX J1713.7−3946: the high-energy cut-off

Fan¹,

Liu²,

Fryer³

2010

Monthly Notices of the Royal Astronomical Society

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In the leptonic scenario for TeV emission from a few well‐observed shell‐type TeV supernova remnants (STTSNRs), very weak magnetic fields are inferred. If fast‐mode waves are produced efficiently in the shock downstream, we show that they are viable agents for acceleration of relativistic electrons inferred from the observed spectra even in the subsonic phase, in spite that these waves are subject to strong damping by thermal background ions at small dissipation scales. Strong collisionless non‐relativistic astrophysical shocks are studied with the assumption of a constant Alfvén speed in the downstream. The turbulence evolution is modelled with both the Kolmogorov and Kraichnan phenomenology. Processes determining the high‐energy cut‐off of non‐thermal electron distributions are examined. The Kraichnan models lead to a shallower high‐energy cut‐off of the electron distribution and require a lower downstream density than the Kolmogorov models to fit a given emission spectrum. With reasonable parameters, the model explains observations of STTSNRs, including recent data obtained with the Fermiγ‐ray telescope. More detailed studies of the turbulence generation and dissipation processes, supernova explosions and progenitors are warranted for better understanding of the nature of supernova shocks.

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“…The spectrum can be described as (e.g. Fang et al 2009) where E ( p ) is the kinetic energy of the electrons, and the electron/proton ratio K ep is treated as a parameter. By equating the synchrotron loss time with the acceleration time, the cut‐off energy E max,e can be estimated as (Berezhko, Ksenofontov & Völk 2002) …”

Section: Model and Resultsmentioning

confidence: 99%

“…It is usually treated as a parameter limited by the comparison of the resulting flux from the model with the observations for a given source (e.g. Berezhko et al 2002; Morlino et al 2009; Fang et al 2008, 2009; Zirakashvili & Aharonian 2010). Its value can be from ∼10 −4 for young SNRs to ∼10 −2 for old SNRs (Zirakashvili & Aharonian 2010).…”

Section: Model and Resultsmentioning

confidence: 99%

“…Semi‐analytical methods for the non‐linear diffusive shock acceleration process have been widely used to investigate the non‐thermal radiative properties of SNRs (e.g. Fang et al 2009; Morlino, Amato & Blasi 2009; Ellison et al 2010). In this paper, we study the non‐thermal radiative properties of the SNR W51C, based on a semi‐analytical method for the non‐linear diffusive shock acceleration mechanism.…”

Section: Introductionmentioning

confidence: 99%

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On the non-thermal emission from the supernova remnant W51C

Fang¹,

Zhang²

2010

Monthly Notices of the Royal Astronomical Society

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The middle-aged supernova remnant W51C is an interesting source because of the interaction of the shell with a molecular cloud. The shell emits intense radio synchrotron photons, and high-energy γ -rays from the remnant have been detected using the Fermi Large Area Telescope (LAT), the High-Energy Stereoscopic System (H.E.S.S.) telescope, and the Milagro gammaray observatory. Based on a semi-analytical approach to the non-linear shock acceleration process, we investigate the multiband non-thermal emission from W51C. The result shows that the radio emission from the remnant can be explained as synchrotron radiation of the electrons accelerated by part of the shock flowing into the ambient medium. However, the high-energy γ -rays detected by the Fermi LAT are mainly produced via proton-proton collisions of the high-energy protons with the ambient matter in the molecular cloud overtaken by the other part of the shock. We propose a possible explanation for the multiband non-thermal emission from W51C. It can be concluded that a molecular cloud overtaken by a shock wave can be an important emitter in GeV γ -rays.

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The multi-band non-thermal emission from the supernova remnant RX J1713.7−3946

Cited by 21 publications

References 34 publications

Understanding hadronic gamma-ray emission from supernova remnants

Understanding hadronic gamma-ray emission from supernova remnants

Stochastic electron acceleration in the TeV supernova remnant RX J1713.7−3946: the high-energy cut-off

On the non-thermal emission from the supernova remnant W51C

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