Cosmological Shock Waves

Bykov, A. M.; Dolag, K.; Durret, F.

doi:10.1007/s11214-008-9312-9

Cited by 66 publications

(43 citation statements)

References 76 publications

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“…Current cosmological shock simulations (e.g. Bykov et al 2008) and the nonthermal emission models (e.g. Kushnir et al 2009) are in favor of the reality of microgauss regime magnetic fields in clusters of galaxies.…”

Section: The Highest Energy Cosmic Raysmentioning

confidence: 99%

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

et al. 2011

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We briefly review sources of cosmic rays, their composition and spectra as well as their propagation in the galactic and extragalactic magnetic fields, both regular and fluctuating. A special attention is paid to the recent results of the X-ray and gamma-ray observations that shed light on the origin of the galactic cosmic rays and the challenging results of Pierre Auger Observatory on the ultra high energy cosmic rays. The perspectives of both high energy astrophysics and cosmic-ray astronomy to identify the sources of ultra high energy cosmic rays, the mechanisms of particle acceleration, to measure the intergalactic radiation fields and to reveal the structure of magnetic fields of very different scales are outlined.

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Section: The Highest Energy Cosmic Raysmentioning

confidence: 99%

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

et al. 2011

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“…Mergers can inject an amount of NT energy of the order of the infall kinetic energy, and thus they can give us a view onto out-of-equilibrium plasma conditions, where relativistic particles can be accelerated [10,11] and give rise to observed diffuse radio emission (e.g., [12,13]). Moreover, a the NT pressure support may yield signifiant deviations from the mass estimates based on the hypothesis of virial theorem and hydrostatic equilibrium, which are inferred from X-ray analysis (e.g., [14][15][16][17]).…”

Section: Introductionmentioning

confidence: 99%

On the Non-Thermal Energy Content of Cosmic Structures

et al. 2016

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(1) Background: the budget of non-thermal energy in galaxy clusters is not well constrained, owing to the observational and theoretical difficulties in studying these diluted plasmas on large scales; (2) Method: we use recent cosmological simulations with complex physics in order to connect the emergence of non-thermal energy to the underlying evolution of gas and dark matter; (3) Results: the impact of non-thermal energy (e.g., cosmic rays, magnetic fields and turbulent motions) is found to increase in the outer region of galaxy clusters. Within numerical and theoretical uncertainties, turbulent motions dominate the budget of non-thermal energy in most of the cosmic volume; (4) Conclusion: assessing the distribution non-thermal energy in galaxy clusters is crucial to perform high-precision cosmology in the future. Constraining the level of non-thermal energy in cluster outskirts will improve our understanding of the acceleration of relativistic particles and of the origin of extragalactic magnetic fields.

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“…Thus, even a moderate efficiency of particle acceleration may reduce the post-shock ion and electron temperatures (see, e.g., Eq. (18) in Bykov et al 2008), which would have implications for the X-ray emission. This effect is expected to be large for shocks with high Mach number (as, for instance, in young SNRs), but not for middle-aged SNRs (on which this paper is focused) for which no non-thermal emission has been detected.…”

Section: Limits Of the Modelmentioning

confidence: 99%

Observability and diagnostics in the X-ray band of shock-cloud interactions in supernova remnants

Orlando¹,

Bocchino²,

Miceli

et al. 2010

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Context. X-ray emitting features originating from the interaction of supernova shock waves with small interstellar gas clouds are revealed in many X-ray observations of evolved supernova remnants (e.g., Cygnus Loop and Vela), but their interpretation is not straightforward. Aims. We develop a self-consistent method for the analysis and interpretation of shock-cloud interactions in middle-aged supernova remnants, which can provide the key parameters of the system and the role of relevant physical effects such as thermal conduction, without the need to perform ad-hoc numerical simulations and bother about morphology details. Methods. We explore all the possible values of the shock speed and cloud density contrast relevant to middle-aged SNRs with a set of hydrodynamic simulations of shock-cloud interaction including the effects of thermal conduction and radiative cooling. From the simulations, we synthesize spatially and spectrally resolved focal-plane data as they would be collected with XMM-Newton/EPIC, an X-ray instrument commonly used in these studies. Results. We develop and calibrate two diagnostic tools, the first based on the mean photon energy versus count-rate scatter plot and the second on the spectral analysis of the interaction region, that can be used to highlight the effects of thermal conduction and to derive the shock speed in case of efficient conduction at work. These tools can be used to ascertain information from X-ray observations, without the need to develop detailed and ad-hoc numerical models for the interpretation of the data.

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Cosmological Shock Waves

Cited by 66 publications

References 76 publications

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

On the Non-Thermal Energy Content of Cosmic Structures

Observability and diagnostics in the X-ray band of shock-cloud interactions in supernova remnants

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