%0 Generic %1 citeulike:13635870 %A Marinacci, Federico %A Vogelsberger, Mark %A Mocz, Philip %A Pakmor, Ruediger %D 2015 %K imported %T The large-scale properties of simulated cosmic magnetic fields %U http://arxiv.org/abs/1506.00005 %X We perform uniformly sampled large-scale cosmological simulations including magnetic fields with the moving mesh code AREPO. We run two sets of MHD simulations: one including adiabatic gas physics only; the other featuring the fiducial feedback model of the Illustris simulation. In the adiabatic case, the magnetic field amplification follows the \$B \rho^2/3\$ scaling derived from `flux-freezing' arguments, with the seed field strength providing an overall normalisation factor. At high baryon overdensities the amplification is enhanced by shear flows and turbulence. Feedback physics and the inclusion of radiative cooling change this picture dramatically. Gas collapses to much larger densities and the magnetic field is amplified strongly, reaching saturation and losing memory of the initial seed field. At lower densities a dependence on the seed field strength and orientation, which in principle can be used to constrain models of cosmological magnetogenesis, is still present. Inside the most massive haloes magnetic fields reach values of \$\sim 10-100\,G\$, in agreement with galaxy cluster observations. The topology of the field is tangled and gives rise to rotation measure signals in reasonable agreement with the observations. However, the rotation measure signal declines too rapidly towards larger radii compared to observational data.

@misc{citeulike:13635870, abstract = {We perform uniformly sampled large-scale cosmological simulations including magnetic fields with the moving mesh code AREPO. We run two sets of MHD simulations: one including adiabatic gas physics only; the other featuring the fiducial feedback model of the Illustris simulation. In the adiabatic case, the magnetic field amplification follows the \$B \propto \rho^{2/3}\$ scaling derived from `flux-freezing' arguments, with the seed field strength providing an overall normalisation factor. At high baryon overdensities the amplification is enhanced by shear flows and turbulence. Feedback physics and the inclusion of radiative cooling change this picture dramatically. Gas collapses to much larger densities and the magnetic field is amplified strongly, reaching saturation and losing memory of the initial seed field. At lower densities a dependence on the seed field strength and orientation, which in principle can be used to constrain models of cosmological magnetogenesis, is still present. Inside the most massive haloes magnetic fields reach values of \$\sim 10-100\,\mu G\$, in agreement with galaxy cluster observations. The topology of the field is tangled and gives rise to rotation measure signals in reasonable agreement with the observations. However, the rotation measure signal declines too rapidly towards larger radii compared to observational data.}, added-at = {2019-03-25T08:20:55.000+0100}, archiveprefix = {arXiv}, author = {Marinacci, Federico and Vogelsberger, Mark and Mocz, Philip and Pakmor, Ruediger}, biburl = {https://www.bibsonomy.org/bibtex/2f2d1a221b03ff0448080774090ab3a73/ericblackman}, citeulike-article-id = {13635870}, citeulike-linkout-0 = {http://arxiv.org/abs/1506.00005}, citeulike-linkout-1 = {http://arxiv.org/pdf/1506.00005}, day = 29, eprint = {1506.00005}, interhash = {9fadf8171f80bf563de1536a3fe91f67}, intrahash = {f2d1a221b03ff0448080774090ab3a73}, keywords = {imported}, month = may, posted-at = {2015-06-07 19:36:59}, priority = {2}, timestamp = {2019-03-25T08:20:55.000+0100}, title = {{The large-scale properties of simulated cosmic magnetic fields}}, url = {http://arxiv.org/abs/1506.00005}, year = 2015 }