MAGIC J0616+225 as delayed TeV emission of cosmic rays diffusing from the supernova remnant IC 443

Torres, D. F.; Marrero, Ana Y. Rodríguez; Pozo, E. De Cea del

doi:10.1111/j.1745-3933.2008.00485.x

Cited by 42 publications

(48 citation statements)

References 50 publications

(70 reference statements)

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“…The diffusion radius for tT pp is R dif (E ) ¼ 2½D(E )t 1 = 2 , so that at a fixed age and distance, only particles of higher energy will be able to compensate for a smaller D 10 , producing SED maxima at higher E-values. The smaller values of D 10 that we study are expected in dense regions of the ISM (e.g., Ormes et al 1988;Torres et al 2008). It is interesting to note that for many, albeit not for all, of the SEDs studied, the maximum in E 2 F space is found at energies beyond the energetic range of GLAST.…”

Section: The Role Of Diffusionmentioning

confidence: 50%

“…We assume typical values, ¼ 2:2 and ¼ 0:5. In the case of energy-dependent propagation of CRs, a large variety of -ray spectra is expected (e.g., Aharonian & Atoyan 1996;Torres et al 2008). Diffusion of CRs has also been explored as an explanation for the high-energy observations of the Galactic center (e.g., Hinton & Aharonian 2007).…”

Section: The Role Of Diffusionmentioning

confidence: 99%

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Diffusion of Cosmic Rays and theGamma‐Ray Large Area Telescope: Phenomenology at the 1–100 GeV Regime

Marrero

Torres

Pozo

et al. 2008

Astrophysical Journal

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This paper analyzes astrophysical scenarios that may be detected at the upper end of the energy range of the GammaRay Large Area Space Telescope (GLAST ), as a result of cosmic-ray (CR) diffusion in the interstellar medium (ISM). Hadronic processes are considered the source of -ray photons from localized molecular enhancements nearby accelerators. Two particular cases are presented: (1) the possibility of detecting spectral energy distributions (SEDs) with maxima above 1 GeV, which may be constrained by detection or nondetection at very high energies (VHEs) with observations by ground-based Cerenkov telescopes, and (2) the possibility of detecting V-shaped, inverted spectra, due to confusion of a nearby (to the line of sight) arrangement of accelerator/ target scenarios with different characteristic properties. We show that finding these signatures (in particular, a peak at the 1Y100 GeV energy region) indicates the underlying mechanism producing the -rays that is realized by nature, which accelerator (age and relative position to the target cloud) and under which diffusion properties CRs propagate.

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Section: The Role Of Diffusionmentioning

confidence: 50%

Section: The Role Of Diffusionmentioning

confidence: 99%

Diffusion of Cosmic Rays and theGamma‐Ray Large Area Telescope: Phenomenology at the 1–100 GeV Regime

Marrero

Torres

Pozo

et al. 2008

Astrophysical Journal

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“…Here, as indicated in Figure 9 (left), there is no connection between n x and n γ because the X-rays are produced in the SNR shell while the γ-rays are from the MC. Such a scenario has been suggested to explain the γ-rays from the source MAGIC J0616+225 as the result of energetic particles that have escaped from IC 443 and are interacting with dense clouds (Torres et al 2008), for example, and discrete TeV sources outside the remnant W28 have been suggested to originate from particles escaping the SNR and interacting with adjacent clouds ). The expected γ-ray spectrum in this scenario is complicated, however.…”

Section: Gamma-ray Observations Of Snrsmentioning

confidence: 99%

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

et al. 2014

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The giant molecular clouds (MCs) found in the Milky Way and similar galaxies play a crucial role in the evolution of these systems. The supernova explosions that mark the death of massive stars in these regions often lead to interactions between the supernova remnants (SNRs) and the clouds. These interactions have a profound effect on our understanding of SNRs. Shocks in SNRs should be capable of accelerating particles to cosmic ray (CR) energies with efficiencies high enough to power Galactic CRs. X-ray and γ-ray studies have established the presence of relativistic electrons and protons in some SNRs and provided strong evidence for diffusive shock acceleration as the primary acceleration mechanism, including strongly amplified magnetic fields, temperature and ionization effects on the shock-heated plasmas, and modifications to the dynamical evolution of some systems. Because protons dominate the overall energetics of the CRs, it is crucial to understand this hadronic component even though electrons are much more efficient radiators and it can be difficult to identify the hadronic component. However, near MCs the densities are sufficiently high to allow the γ-ray emission to be dominated by protons. Thus, these interaction sites provide some of our best opportunities to constrain the overall energetics of these particle accelerators. Here we summarize some key properties of interactions between SNRs and MCs, with an emphasis on recent X-ray and γ-ray studies that are providing important constraints on our understanding of cosmic rays in our Galaxy.

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“…For IC 443 the centroids of the GeV and TeV emission are not coinciding, a fact that could be explained as the result of the escape of high energy CRs from the SNR shell and of their interaction with the ambient medium. In this scenario, the diffusion coefficient for the multi-TeV CRs is of the order of D ≈ 10 27 ( CR/0.1) 2 cm 2 /s (with CR the efficiency of converting the SN explosion energy into CRs), a diffusion coefficient that is much smaller than the average diffusion coefficient in the Galaxy (75). While these measurement provide an important proof of the acceleration of CR protons in shock wave of SNRs, the lessons that can be learned on the acceleration of the bulk of CRs in our Galaxy are somewhat limited since the maximum particle energy is way short of the "knee" in the spectrum of CRs.…”

Section: The Origin Of Cosmic Raysmentioning

confidence: 99%

Ground- and Space-Based Gamma-Ray Astronomy

Funk

2015

Annu. Rev. Nucl. Part. Sci.

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In recent years, observational γ-ray astronomy has seen a remarkable range of exciting new results in the high-energy and very-high energy regimes. Coupled with extensive theoretical and phenomenological studies of non-thermal processes in the Universe these observations have provided a deep insight into a number of fundamental problems of high energy astrophysics and astroparticle physics. Although the main motivations of γ-ray astronomy remain unchanged, recent observational results have contributed significantly towards our understanding of many related phenomena. This article aims to review the most important results in the young and rapidly developing field of γ-ray astrophysics.

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MAGIC J0616+225 as delayed TeV emission of cosmic rays diffusing from the supernova remnant IC 443

Cited by 42 publications

References 50 publications

Diffusion of Cosmic Rays and theGamma‐Ray Large Area Telescope: Phenomenology at the 1–100 GeV Regime

Diffusion of Cosmic Rays and theGamma‐Ray Large Area Telescope: Phenomenology at the 1–100 GeV Regime

Supernova Remnants Interacting with Molecular Clouds: X-Ray and Gamma-Ray Signatures

Ground- and Space-Based Gamma-Ray Astronomy

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