The Relation between Gas Density and Velocity Power Spectra in Galaxy Clusters: Qualitative Treatment and Cosmological Simulations
Irina Zhuravleva,E. M. Churazov,Alexander Schekochihin,Erwin T. Lau,Daisuke Nagai,Massimo Gaspari,Steven W. Allen,Steven W. Allen,Kaylea Nelson,Ian J. Parrish +9 more
TLDR
In this article, the power spectrum of the velocity field of the intracluster medium using only information on the plasma density fluctuations, which can be measured today by Chandra and XMM-Newton observatories, is evaluated.Abstract:
We address the problem of evaluating the power spectrum of the velocity field of the intracluster medium using only information on the plasma density fluctuations, which can be measured today by Chandra and XMM-Newton observatories. We argue that for relaxed clusters there is a linear relation between the rms density and velocity fluctuations across a range of scales, from the largest ones, where motions are dominated by buoyancy, down to small, turbulent scales: , where δρ k /ρ is the spectral amplitude of the density perturbations at wavenumber k, is the mean square component of the velocity field, cs is the sound speed, and η1 is a dimensionless constant of the order of unity. Using cosmological simulations of relaxed galaxy clusters, we calibrate this relation and find η1 1 ± 0.3. We argue that this value is set at large scales by buoyancy physics, while at small scales the density and velocity power spectra are proportional because the former are a passive scalar advected by the latter. This opens an interesting possibility to use gas density power spectra as a proxy for the velocity power spectra in relaxed clusters across a wide range of scales.read more
Citations
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Turbulent heating in galaxy clusters brightest in X-rays
Irina Zhuravleva,E. Churazov,Alexander Schekochihin,Steven W. Allen,Steven W. Allen,P. Arévalo,P. Arévalo,Andrew C. Fabian,William R. Forman,Jeremy S. Sanders,Aurora Simionescu,R. A. Sunyaev,Alexey Vikhlinin,Norbert Werner +13 more
TL;DR: It is found that turbulent heating is sufficient to offset radiative cooling and indeed appears to balance it locally at each radius—it may be the key element in resolving the gas cooling problem in cluster cores and, more universally, in the atmospheres of X-ray-emitting, gas-rich systems on scales from galaxy clusters to groups and elliptical galaxies.
Journal ArticleDOI
Laboratory evidence of dynamo amplification of magnetic fields in a turbulent plasma
Petros Tzeferacos,Petros Tzeferacos,A. Rigby,A. F. A. Bott,Anthony R. Bell,Robert Bingham,Robert Bingham,Alexis Casner,Fausto Cattaneo,Eugene Churazov,J. Emig,Frederico Fiuza,Cary Forest,John Foster,Carlo Graziani,Joseph Katz,Michel Koenig,Chikang Li,J. Meinecke,R. D. Petrasso,H-S Park,Bruce Remington,J. S. Ross,Dongsu Ryu,D. Ryutov,Thomas G. White,Brian Reville,F. Miniati,Alexander Schekochihin,Donald Q. Lamb,Dustin Froula,Gianluca Gregori,Gianluca Gregori +32 more
TL;DR: In this paper, the authors demonstrate that turbulence is indeed capable of rapidly amplifying seed fields to near equipartition with the turbulent fluid motions, and support the notion that turbulent dynamo is a viable mechanism responsible for the observed present-day magnetization.
Journal ArticleDOI
The relation between gas density and velocity power spectra in galaxy clusters: High-resolution hydrodynamic simulations and the role of conduction
TL;DR: In this article, the velocity field and its intimate relation with the ICM thermodynamic perturbations were studied using high-resolution 3D plasma simulations, and it was shown that the variance of density perturbation is comparable to the 1D Mach number, M 1D ~ δρ /ρ.
Journal ArticleDOI
Gas density fluctuations in the Perseus Cluster: clumping factor and velocity power spectrum
Irina Zhuravleva,E. M. Churazov,P. Arévalo,Alexander Schekochihin,Steven W. Allen,Steven W. Allen,A. C. Fabian,William R. Forman,Jeremy S. Sanders,Aurora Simionescu,R. A. Sunyaev,Alexey Vikhlinin,Norbert Werner +12 more
TL;DR: In this article, the amplitude of gas density fluctuations on different scales is measured in a set of radial annuli, using a statistical linear relation between the observed amplitude of density fluctuations and predicted velocity, the characteristic velocity of gas motions on each scale is calculated.
Journal ArticleDOI
The Matryoshka Run. II. Time-dependent Turbulence Statistics, Stochastic Particle Acceleration, and Microphysics Impact in a Massive Galaxy Cluster
TL;DR: In this article, the authors used the Matryoshka run to study the time-dependent statistics of structure-formation-driven turbulence in the intracluster medium of a 1015 M galaxy cluster.
References
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