Magnetic field amplification in cold dark matter anisotropic collapse

Bruni, Marco; Maartens, Roy; Tsagas, Christos G.

doi:10.1046/j.1365-8711.2003.06095.x

Cited by 35 publications

(33 citation statements)

References 19 publications

(20 reference statements)

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“…Additional to any dynamo action, further support for strong magnetic field amplification during the process of structure formation comes from the application of the Zel'dovich approximation (Zel'dovich 1970) to follow the MHD equations during the gravitational collapse (Bruni et al 2003;King and Coles 2006). These papers demonstrate the existence of a super-adiabatic amplification due to the anisotropy of the collapse of the LSS within the cold dark matter paradigm.…”

Section: Approximative Simulationsmentioning

confidence: 99%

Non-Thermal Processes in Cosmological Simulations

2008

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Non-thermal components are key ingredients for understanding clusters of galaxies. In the hierarchical model of structure formation, shocks and large-scale turbulence are unavoidable in the cluster formation processes. Understanding the amplification and evolution of the magnetic field in galaxy clusters is necessary for modelling both the heat transport and the dissipative processes in the hot intra-cluster plasma. The acceleration, transport and interactions of non-thermal energetic particles are essential for modelling the observed emissions. Therefore, the inclusion of the non-thermal components will be mandatory for simulating accurately the global dynamical processes in clusters. In this review, we summarise the results obtained with the simulations of the formation of galaxy clusters which address the issues of shocks, magnetic field, cosmic ray particles and turbulence.

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Section: Approximative Simulationsmentioning

confidence: 99%

Non-Thermal Processes in Cosmological Simulations

2008

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“…This increases the strength of the magnetic field, which remains frozen-in with the baryons, beyond the adiabatic limit (Bruni, Maartens & Tsagas 2003;Dolag, Bartelmann & Leach 1999). The enhanced B-field could then backreact and have a stronger effect on the evolution of density perturbations.…”

Section: The Magnetic Effectsmentioning

confidence: 99%

Magnetized cosmological perturbations in the post-recombination era

Vasileiou

Tsagas

2015

Mon. Not. R. Astron. Soc.

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We study inhomogeneous magnetised cosmologies through the post-recombination era in the framework of Newtonian gravity and the ideal-magnetohydrodynamic limit. The nonlinear kinematic and dynamic equations are derived and linearised around the Newtonian counterpart of the Einstein-de Sitter universe. This allows for a direct comparison with the earlier relativistic treatments of the issue. Focusing on the evolution of linear density perturbations, we provide new analytic solutions which include the effects of the magnetic pressure as well as those of the field's tension. We confirm that the pressure of field inhibits the growth of density distortions and can induce a purely magnetic Jeans length. On scales larger than the aforementioned characteristic length the inhomogeneities grow, though slower than in non-magnetised universes. Wavelengths smaller than the magnetic Jeans length typically oscillate with decreasing amplitude. We also identify a narrow range of scales, just below the Jeans length, where the perturbations exhibit a slower power-law decay. In all cases, the effect of the field is proportional to its strength and increases as we move to progressively smaller lengths.

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“…Further support for strong MF amplification during the process of structure formation comes from the application of the Zel'dovich approximation to follow the MHD equations during the gravitational collapse (Bruni, Maartens & Tsagas 2003;King & Coles 2005). Such works showed superadiabatic amplification due to the anisotropy of the collapse of the LSS within the cold dark matter paradigm.…”

Section: Cosmological Mhd Simulationsmentioning

confidence: 99%

Simulating large‐scale structure formation with magnetic fields

Dolag¹

2006

Astron Nachr

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Abstract. In the past, different works based on numerical simulations have been presented to explain magnetic fields (MFs) in the large scale structure and within galaxy clusters. In this review, I will summarize the main findings obtained by different authors and -even if many details are still unclear -I will try to construct a consistent picture of our interpretation of largescale magnetic fields based on numerical effort. I will also sketch how this is related to our understanding of radio emission and summarize some arguments where our theoretical understanding has to be improved to match the observations.

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Magnetic field amplification in cold dark matter anisotropic collapse

Cited by 35 publications

References 19 publications

Non-Thermal Processes in Cosmological Simulations

Non-Thermal Processes in Cosmological Simulations

Magnetized cosmological perturbations in the post-recombination era

Simulating large‐scale structure formation with magnetic fields

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