ENZO simulations using Adaptive Mesh Refinement
THE ADOPTION OF AN IMPLEMENTED MESH REFINMENT TECHNIQUE
PRODUCES MORE TURBULENCE IN ENZO CLUSTER SIMULATIONS
In Vazza et al.(2009) we show that
adopting an extra refinement criterion working
on velocity jumps
slightly changes the innermost thermal
structure of simulated galaxy clusters. In particular, we found
- innermost gas density is
reduced by 10% compared to cluster simulated with AMR;
- innermost gas temperature and
entropy are 10% larger;
- turbulent energy is 50-200%
higher (depending on radius).
SHOWS SPECTRAL SIGNATURES SIMILAR TO KOLMOGOROV TURBULENCE
We measured structure
functions and power spectra over nearly two order of magnitude,
signatures of a turbulent
cascade, from ~ Mpc scales to ~10kpc scales.
instabilities injected by infalling clummps and crossing shocks are
likely the main sources of turbulent motions in the ICM.
THE INJECTION OF TURBULENCE
AND THERMAL ENERGY AT SHOCKS
DO CORRELATE IN TIME
With the exquisite spatial resolution up
to 2 virial radii from the center of our simulated clusters,
we were able to follow in detail the evolution
of merger and accretion shocks, and to correlated them
with the evolution of the power spectrum of turbulent energy, finding
that the bulk
of both energy release is related to the major merger event which forms
of cluster mass.
see Vazza et al.2009 A&A