Evolution and structure of magnetic fields in simulated galaxy clusters

By Klaus Dolag, M. Lesch. 2002

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We use cosmological magneto-hydrodynamic simulations to study the evolution of magnetic elds in galaxy clusters in two dierent cosmological models, a standard-CDM and a -CDM model. We show that the mag- netic eld strength proles closely follow the cluster density proles outside a core region of radius200 h 1 kpc. The magnetic eld has a correlation length of order 50 h 1 kpc and reverses on scales of100 h 1 kpc along typ- ical lines-of-sight. The power spectrum of the magnetic eld can well be approximated by a steep power law with an exponent of 2:7. The mean magnetic eld in the cluster cores grows roughly exponentially with decreasing redshift, B 10 2:5z G. Merger events have a pronounced eect on magnetic eld evolution, which is strongly reflected in measurable quantities like the Faraday rotation. The eld evolution in the two dierent cosmologies proceeds virtually identically. All our cluster models very well reproduce observed Faraday rotation measurements when starting with nG seed elds.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/44269816077fa555e2df5d5638dd8f7f0a22ef7e

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Citations in the corpus

Multi-frequency analysis of neutralino dark matter annihilations in the Coma cluster (2005, background): “…in clusters and, more specifically, for Coma (see Colafrancesco et al. 2005) and it is also predicted by numerical simulations (see, e.g., Dolag et al. 2002): thus it seems quite natural and motivated. radial dependence B(r) = B0 ( 1 + rrc1 )2 · [ 1 + ( r rc2 )2]−β with B0 = 0.55 µG , β…”
Simulations of magnetic fields in isolated disc galaxies (2012, background): “Dolag et al. (1999, 2002) have shown that the complex shear flows and large adiabatic compression involved in building up the intracluster gas lead to a sizable amplification of magnetic fields, producing an end state that is largely insensitive to the initial seed field strength and configuration,…”
Magnetic fields and Faraday rotation in clusters of galaxies (2004, background): “Moreover, detailed magneto-hydrodynamic cosmological simulations (Dolag et al. 2002) lead to magnetic fields whose strength decreases with the distance from the cluster center.”
Turbulent gas motions in galaxy cluster simulations: the role of smoothed particle hydrodynamics viscosity (2005, background): “Shear flows associated with cluster turbulence and the resulting dynamo processes could considerably amplify the magnetic fild strength in the ICM (e.g., Dolag et al. 1999, 2002).”
An MHD gadget for cosmological simulations (2008, methodology): “Figure 1 shows the result for a code implementation similar to the first implementation used to study galaxy clusters (e.g. see Dolag et al. 1999, 2002).”
Astrophysical smooth particle hydrodynamics (2009, methodology): “The most obvious approach is a straight-forward SPH discretization of the ideal MHD equations (Gingold and Monaghan, 1977; Phillips and Monaghan, 1985; Dolag et al., 2002; Price and Monaghan, 2004a,b, 2005; Price, 2004).”
Cluster magnetic fields from galactic outflows (2008, methodology): “Therefore, the final magnetic field is shaped by such processes rather than by the initial conditions, in agreement with previous findings (Dolag et al. 1999, 2002) and analytical modelling of saturated dynamos in clusters (Enßlin & Vogt 2006; Subramanian, Shukurov & Haugen 2006).”
Diffuse Radio Emission from Galaxy Clusters (2019, background): “Cosmological simulations of clusters predict µGauss-level magnetic field strengths in the cluster centers and a decrease of the magnetic field strength with radius in the outer regions (Dolag et al. 1999, 2001, 2002; Vazza et al. 2014, 2018).”
Compressible turbulence in galaxy clusters: physics and stochastic particle re-acceleration (2007, background): “Turbulence is an important ingredient in the physics of the ICM as it is necessary to understand the amplification of magnetic fields in clusters (Dolag et al. 2002; Schekochihin et al. 2005; Subramanian et al. 2006), an issue closely related to the non–thermal emission from clusters but that we…”
Acceleration of primary and secondary particles in galaxy clusters by compressible MHD turbulence: from radio haloes to gamma-rays (2010, background): “During these events a fraction of the gravitational binding–energy of Dark Matter halos that is converted into internal energy of the barionic matter can be channelled into the amplification of the magnetic fields (e.g. Dolag et al. 2002; Subramanian et al.”
The speed of the ‘bullet’ in the merging galaxy cluster 1E0657−56 (2007, background): “…fractions, the effective viscosity of the gas (Sijacki & Springel 2006), its thermal conductivity (Jubelgas et al. 2004), and also non-thermal pressure components like cosmic rays (Pfrommer et al. 2006; Ensslin et al. 2006; Jubelgas et al. 2006) or intracluster magnetic fields (Dolag et al. 2002).”