Press Release by CSCS 'Supercomputer
"feels" magnetic fields in the cosmo'
- "On the amplification of magnetic fields in cosmic filaments and galaxy clusters" (Vazza, Brüggen, Gheller & Wang 2014, MNRAS) 2014MNRAS.445.3706V
- "Ultra-High Energy Cosmic Rays and the study of Cosmic Magnetism" (Stefan Hackstein, Bachelor Thesis at Hamburg University 2014)
- "Numerical cosmology on the GPU with Enzo and Ramses" (Gheller, Wang, Vazza & Teyssier 2014), 2014arXiv1412.0934G
- News at Hamburg Observatory
- "Forecasts for the detection of the magnetised cosmic web from cosmological simulations" (Vazza, Ferrari, Brüggen, Bonafede, Gheller & Wang, submitted)
through the 2400^3 run (50 Mpc cubic) at z=0. Yellow
colors=magnetic fields; red/pink= gas temperature
We study the amplification of cosmic magnetic fields during structure formation, and derive the typical magnetic field strengths in galaxy clusters and
filaments. We also investigate the role of other astrophysical sources of magnetisation (galaxies and AGN) towards a self-consisten modelling of
cosmic magnetism in large-scale structures.
We use the public versions of ENZO. 2.1 (Collins et al. 2010) plus porting on the GPU using Cuda by Wang et al. (2010), plus
several developments by our group:
+ energy feedback (when cooling is activated) from AGNs internal to clusters, with kinetic/thermal energy release (as in Vazza et al.2013)
+ seeding from galaxies by injecting magnetic loops with a 1% energy in magnetic fields.
In this project, we make use both of large unigrid runs (1200^3-2400^3) and of AMR runs with nested initial conditions.
The successful proposal for CHRONOS is here.
All big runs were run at CSCS using Piz-Daint.
A few runs are generated also at Juelich (JUROPA) using the CPU version of the code.
We store most of the "clean" data in the repository hosted at Hamburg (/home/hslxrsrv3/).
LCDM with OmegaToT=1, Omega_Lambda=0.728, Omega_Matter=0.272, Omega_baryons=0.0455, h=0.702, sigma8=0.8
|Here a list of the runs evolved
so far down to z=0, and of the one under
|Gallery of first
Evolution of magnetic fields in a cosmic filament
Evolution of magnetic fields in a galaxy cluster
Average scaling between magnetic field and gas density for our 1200^3 run of a 25 cubic Mpc, with and without
additional magnetisation from galaxies.
Power spectra of velocity and magnetic fields as a function of resolution, for the ICM and the WHIM of a simulated filament.