2013 PRACE PROJECT ON CURIE (FRANCE)
                   


Publications & Press:

    -    Simulations of cosmic rays in large-scale structures: numerical and physical effects (Vazza, F., Gheller C., Brüggen,   2014MNRAS.439.2662V  MNRAS)
    -    Scaling relations in clusters of galaxies (Manuel Stubbe, Bachelor Thesis at Hamburg University 2013)
    -    Testing diffusive shock acceleration in galaxy clusters with cosmological simulations (F. Vazza, M. Bruggen, D. Eckert, C. Gheller,  A. Bonafede, M. Stubbe, to be submitted)

     - Filaments of the radio cosmic web: opportunities and challenges for SKA,
2015arXiv150100315V,  (F. Vazza, C. Ferrari, A. Bonafede, M. Brüggen, C. Gheller, R. Braun, S. Brown, to appear in AASKA15, Proceeding of Science 2015)    



final density slice (z=0, 300x300 Mpc^2)


GOALS:
Study of non-thermal processes in large-scale structures, covering a large cosmological volume and high resolution, with complex cosmic rays physics.
Once completed, this should be the largest non-thermal simulation of the Universe ever produced so far.
It will offer us a very complete view of resolution effects, "astrophysical" (i.e. cooling, AGN feedback etc) and "physical" (i.e. details
in particle acceleration) effects contributing to the final budget of cosmic rays within clusters.


CODE:

We use the public versions of
ENZO.1.5  & 2.1 (Collins et al. 2010) plus several developments by our group:

+ injection, advection, pressure feedback and reduced thermalization  from injected cosmic rays hadrons (with a gamma=4/3
equation of state), as in Vazza et al. 2012

+ energy feedback (when cooling is activated) from AGNs internal to clusters, with kinetic/thermal energy release (as in Vazza et al.2013

+ re-acceleration from shock waves

+ Coulomb & hadronic losses of CRs (and heating of the gas)

In this project, we do not make any use of AMR, but we only use a fixed mesh resolution.
PROPOSAL:
The proposal for PRACE (originally designed for the FERMI BlueGeneP of CINECA) is here.
WHERE:
All "big" runs are produced the Linux cluster CURIE.
A few runs are generated also at Juelich (JUROPA) using the same version of the code.
Some last runs are also beeing run at CSCS (Monte Rosa.and Piz-Daint)


ARCHIVE
We store most of the "clean" data in the repository hosted at Hamburg (/home/hslxrsrv3/). The goal is to store both full-Universe boxes (512^3,1024^3,2048^3) at a few interesting
redshifts, and time-resolved cluster snapshots for regions of 2Rvir around each cluster.
All data have been moved!

Cosmological model:

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 production
 

CUR1
CUR2 CUR3
VOLUME
300 Mpc (216 Mpc/h)
150 Mpc (108 Mpc/h) 75 Mpc (50 Mpc/h)
Ncells
2048^3
1024^3
512^3
1024^3
512^3
1024^3
512^3

resol.[kpc]
146 (115/h)
296 (230/h)
592(460/h)
146(115/h)
296(230/h)
75(58/h)
146(115/h)

physics

1RD(z=0)@
0RD(z=0)
c0RD(z=0)
1RD(z=0)
0RD(z=0)


0RD(z=0)
1RD(z=0)

0RD(z=0)
cRD(z=0)*
cSNRD(z=0)*
0RD(z=0)
1RD(z=0)

0RD(z=0)
cSNRD(z=0)*
c0RD(z=0)*










c1RD(z=0)^




c1RD(z=0)^


1RD(z=0)* c1RD(z=0)* coolRD(z=0)*


physical models (reionization in all cases):
- 0 = Cosmic rays (inj-reacc-advec-pressure), efficinecy of Kang & Jones 2007 (as in first two "scienzo" papers, FV et al.2012,13).
- c: cooling + AGN feedback (bipolar thermal)

- 1 = as in CR0, but with the Kang & Ryu (2013) lower efficiency
- SN = "supernovae" boost of thermal and CR energy at z=2.

*=the data are in JUROPA@Juelich
^=the data are in MonteRosa@CSCS

@=the data are in Daint@CSCS

Gallery of first results:

Fly through the 2048^3 run of 300 Mpc at z=0

(shown in clockwise order are DM, gas density, CR energy and gas energy)






Fly through the 2048^3 run of 300 Mpc at z=0

(shown is the projected gas density)




Distribution functions as a function of resolution/volume, for non-radiative runs (CUR1 and CUR3).



Average CR to gas pressure ratio as a function of assumed physics for Cosmic rays.




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