Effect of shocks on interstellar turbulence and cosmic-ray dynamics

Bykov, A. M.; Топтыгин, И. Н.

doi:10.1007/bf00637855

Cited by 53 publications

(45 citation statements)

References 24 publications

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“…Other types of spectra frequently used to describe the interstellar turbulence are W (k) ∝ k −2 for the shock-dominated turbulence, see e.g. the model by Bykov and Toptygin (1987), and spectrum W (k) ∝ k −3/2 suggested by Iroshnikov (1964) and Kraichnan (1965) in their phenomenological theory of MHD turbulence. Comprehensive reviews of MHD turbulence with application to the interstellar conditions have been given by Zhou et al (2004), Elmegreen and Scalo (2004), and Scalo and Elmegreen (2004).…”

Section: Kinetic Theory Of Cosmic Ray Diffusion In Galactic Magnetic mentioning

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: Kinetic Theory Of Cosmic Ray Diffusion In Galactic Magnetic mentioning

confidence: 99%

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

et al. 2011

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“…This mechanism has been studied by Bykov & Toptygin (1987), Bykov & Fleishman (1992), Bykov (1995Bykov ( , 2001), and we only give here an outline of its main features.…”

Section: Turbulent Acceleration Inside Sbsmentioning

confidence: 99%

Superbubbles and energetic particles in the Galaxy

Parizot¹,

Marcowith

Swaluw

et al. 2004

A&A

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203

194

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Abstract.Observations indicate that most massive stars in the Galaxy appear in groups, called OB associations, where their strong wind activity generates large structures known as superbubbles, inside which the subsequent supernovae (SNe) explode, with a tight space and time correlation. We investigate four main questions: 1) does the clustering of massive stars and SN explosions influence the particle acceleration process usually associated with SNe, and induce collective effects which would not manifest around isolated supernova remnants?; 2) does it make a difference for the general phenomenology of Galactic Cosmic Rays (GCRs), notably for their energy spectrum and composition?; 3) Can this help alleviate some of the problems encountered within the standard GCR source model?; and 4) Is the link between superbubbles and energetic particles supported by observational data, and can it be further tested and constrained? We argue for a positive answer to all these questions. Theoretical, phenomenological and observational aspects are treated in separate papers. Here, we discuss the interaction of massive stellar winds and SN shocks inside superbubbles and indicate how this leads to specific acceleration effects. We also show that due to the high SN explosion rate and low diffusion coefficient, low-energy particles experience repeated shock acceleration inside superbubbles.

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“…Its statistical analysis, including that of interstellar turbulence, is complicated by the multiphase structure, where the diversity of physical processes predominant in different phases causes strong inhomogeneity. Furthermore, interstellar turbulence is transonic or supersonic (Bykov & Toptygin 1987;Vázquez-Semadeni 2015). The compressibility and abundance of random shock waves lead to spatial and temporal intermittency of the random velocity and magnetic fields and of the density fluctuations.…”

Section: Introductionmentioning

confidence: 99%

Supernova-regulated ISM. V. Space and Time Correlations

Hollins

Sarson

Shukurov

et al. 2017

ApJ

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We apply correlation analysis to random fields in numerical simulations of the supernova-driven interstellar medium (ISM) with the magnetic field produced by dynamo action. We solve the magnetohydrodynamic (MHD) equations in a shearing Cartesian box representing a local region of the ISM, subject to thermal and kinetic energy injection by supernova explosions, and parameterized, optically thin radiative cooling. We consider the cold, warm, and hot phases of the ISM separately; the analysis mostly considers the warm gas, which occupies the bulk of the domain. Various physical variables have different correlation lengths in the warm phase: 40, 50, and 60 pc for the random magnetic field, density, and velocity, respectively, in the midplane. The correlation time of the random velocity is comparable to the eddy turnover time, about 10 year 7 , although it may be shorter in regions with a higher star formation rate. The random magnetic field is anisotropic, with the standard deviations of its components b b b x y z having approximate ratios 0.5 0.6 0.6 in the midplane. The anisotropy is attributed to the global velocity shear from galactic differential rotation and locally inhomogeneous outflow to the galactic halo. The correlation length of Faraday depth along the z axis, 120 pc, is greater than for electron density, 60 90 pc -, and the vertical magnetic field, 60 pc. Such comparisons may be sensitive to the orientation of the line of sight. Uncertainties of the structure functions of synchrotron intensity rapidly increase with the scale. This feature is hidden in a power spectrum analysis, which can undermine the usefulness of power spectra for detailed studies of interstellar turbulence.

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Effect of shocks on interstellar turbulence and cosmic-ray dynamics

Cited by 53 publications

References 24 publications

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Cosmic Rays in Galactic and Extragalactic Magnetic Fields

Superbubbles and energetic particles in the Galaxy

Supernova-regulated ISM. V. Space and Time Correlations

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