Cosmological Simulations & Projects
 
Here is a detailed list of the most important projects
we are running using some of the largest computing
facilities around. Our tool of choice is the ENZO grid code.
  1. THE EVOLUTION OF COSMIC MAGNETISM
    We prouduce with ENZO some of the largest Magneto-Hydrodynamical (MHD) simulations to-date in order to study how cosmic magnetic fields evolve across cosmic epochs and get to the values measured nowadays. GPU-accelerated computations allows us to explore a big range of parameters.
  2. THE QUEST FOR THE RADIO COSMIC WEB
    We study the best strategies to detected the warm-hot intergalatic medium (WHIM) in the filamentary mass component of the cosmic web with the existing (e.g. LOFAR) or future (SKA) big radio telescopes.
  3. TURBULENCE IN THE INTRACLUSTER MEDIUM
    We use adapative mesh refinement to study turbulence in galaxy clusters at very high resolution, by probing its spatial and spectral feature. We study how turbulent motions are distributed across scales and modes (solenoidal vs compressive) and how turbulence can influence many observables.
  4. COMPLEXITY & INFORMATION IN THE COSMOS
    We produced first and original exploration of the flux of information across cosmic structures. The complexity inherent to the formation of cosmic structure can be quantified with numerical simulations, which also highlight how different processes bring complexity into the Universe.
  5. COSMIC RAYS IN LARGE-SCALE STRUCTURES
    With an original implementation of cosmic ray physics in ENZO we can study the injection of cosmic rays by shocks waves during the formation of cosmic structure, and limit the acceleration of cosmic ray protons and electrons as a function of plasma parameters.
  6. MASSIVE & REFINED CLUSTERS
    We produced a sample of >1e15Msol galaxy clusters with AMR in order to study shocks, turbulence, clumping and accretions with unprecedented high resolution.
  7. COSMOLOGY CODES COMPARISON
    We compared ENZO, GADGET and TVD on the same set of cosmological initial conditions, and measure their differences and similarity on gas an shocks statistics.
More

see Vazza et al. 2014 MNRAS

Gheller et al. 2015     Hackstein et al. 2016

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see Vazza et al. 2015 PoS

Vazza et al. 2015 A&A

Bonafede et al. 2015 PoS

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see Vazza et al. 2012 MNRAS

Vazza et al. 2013 MNRAS

Vazza et al. 2014 MNRAS

Gheller et al. 2015 MNRAS

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see Vazza et al. 2017 MNRAS;  Wittor, FV & Bruggen 2017

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Vazza et al. 2013 MNRAS

see Vazza et al. 2010 NewA

Vazza et al. 2011 A&A

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see Vazza et al. 2010 NewA