THE MATRYOSHKA RUN. II. TIMEDEPENDENT TURBULENCE STATISTICS, STOCHASTIC PARTICLE ACCELERATION, AND MICROPHYSICS IMPACT IN A MASSIVE GALAXY CLUSTER
Abstract
We use the Matryoshka run to study the timedependent statistics of structureformationdriven turbulence in the intracluster medium of a 10{sup 15} M {sub ☉} galaxy cluster. We investigate the turbulent cascade in the inner megaparsec for both compressional and incompressible velocity components. The flow maintains approximate conditions of fully developed turbulence, with departures thereof settling in about an eddyturnover time. Turbulent velocity dispersion remains above 700 km s{sup –1} even at low mass accretion rate, with the fraction of compressional energy between 10% and 40%. The normalization and the slope of the compressional turbulence are susceptible to large variations on short timescales, unlike the incompressible counterpart. A major merger occurs around redshift z ≅ 0 and is accompanied by a long period of enhanced turbulence, ascribed to temporal clustering of mass accretion related to spatial clustering of matter. We test models of stochastic acceleration by compressional modes for the origin of diffuse radio emission in galaxy clusters. The turbulence simulation model constrains an important unknown of this complex problem and brings forth its dependence on the elusive microphysics of the intracluster plasma. In particular, the specifics of the plasma collisionality and the dissipation physics of weak shocks affect the cascade of compressionalmore »
 Authors:
 Physics Department, WolfgangPauliStrasse 27, ETHZürich, CH8093 Zürich (Switzerland)
 Publication Date:
 OSTI Identifier:
 22364215
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: Astrophysical Journal; Journal Volume: 800; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATION; APPROXIMATIONS; COMPUTERIZED SIMULATION; CORRELATIONS; DISTANCE; GALAXY CLUSTERS; INDEXES; MASS; ORIGIN; PLASMA; RED SHIFT; STAR ACCRETION; STOCHASTIC PROCESSES; TIME DEPENDENCE; TURBULENCE; UNIVERSE; VELOCITY
Citation Formats
Miniati, Francesco, Email: fm@phys.ethz.ch. THE MATRYOSHKA RUN. II. TIMEDEPENDENT TURBULENCE STATISTICS, STOCHASTIC PARTICLE ACCELERATION, AND MICROPHYSICS IMPACT IN A MASSIVE GALAXY CLUSTER. United States: N. p., 2015.
Web. doi:10.1088/0004637X/800/1/60.
Miniati, Francesco, Email: fm@phys.ethz.ch. THE MATRYOSHKA RUN. II. TIMEDEPENDENT TURBULENCE STATISTICS, STOCHASTIC PARTICLE ACCELERATION, AND MICROPHYSICS IMPACT IN A MASSIVE GALAXY CLUSTER. United States. doi:10.1088/0004637X/800/1/60.
Miniati, Francesco, Email: fm@phys.ethz.ch. 2015.
"THE MATRYOSHKA RUN. II. TIMEDEPENDENT TURBULENCE STATISTICS, STOCHASTIC PARTICLE ACCELERATION, AND MICROPHYSICS IMPACT IN A MASSIVE GALAXY CLUSTER". United States.
doi:10.1088/0004637X/800/1/60.
@article{osti_22364215,
title = {THE MATRYOSHKA RUN. II. TIMEDEPENDENT TURBULENCE STATISTICS, STOCHASTIC PARTICLE ACCELERATION, AND MICROPHYSICS IMPACT IN A MASSIVE GALAXY CLUSTER},
author = {Miniati, Francesco, Email: fm@phys.ethz.ch},
abstractNote = {We use the Matryoshka run to study the timedependent statistics of structureformationdriven turbulence in the intracluster medium of a 10{sup 15} M {sub ☉} galaxy cluster. We investigate the turbulent cascade in the inner megaparsec for both compressional and incompressible velocity components. The flow maintains approximate conditions of fully developed turbulence, with departures thereof settling in about an eddyturnover time. Turbulent velocity dispersion remains above 700 km s{sup –1} even at low mass accretion rate, with the fraction of compressional energy between 10% and 40%. The normalization and the slope of the compressional turbulence are susceptible to large variations on short timescales, unlike the incompressible counterpart. A major merger occurs around redshift z ≅ 0 and is accompanied by a long period of enhanced turbulence, ascribed to temporal clustering of mass accretion related to spatial clustering of matter. We test models of stochastic acceleration by compressional modes for the origin of diffuse radio emission in galaxy clusters. The turbulence simulation model constrains an important unknown of this complex problem and brings forth its dependence on the elusive microphysics of the intracluster plasma. In particular, the specifics of the plasma collisionality and the dissipation physics of weak shocks affect the cascade of compressional modes with strong impact on the acceleration rates. In this context radio halos emerge as complex phenomena in which a hierarchy of processes acting on progressively smaller scales are at work. Stochastic acceleration by compressional modes implies statistical correlation of radio power and spectral index with merging cores distance, both testable in principle with radio surveys.},
doi = {10.1088/0004637X/800/1/60},
journal = {Astrophysical Journal},
number = 1,
volume = 800,
place = {United States},
year = 2015,
month = 2
}

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