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Дата изменения: Thu Oct 22 05:31:57 2009
Дата индексирования: Mon Oct 1 19:43:14 2012
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My research interests focus on Hydrodynamical and MHD numerical
simulations of the radio source feedback on the intra-cluster medium
(ICM) in galaxy clusters. Here are some movies of my simulations:
ABOVE: the effects of a relativistic jet on the random
structure of the magnetic fields in galaxy clusters. The animation shows a
zoom to the central region of a 3D cube. This is a slice
at X=0, where the axes show the distance and the colour scale,
the
logarithm of the intensities of the magnetic fields
in microGauss. The time is given in million years. The jet's cocoon
orders
and amplifies the magnetic fields in its vicinities
while the fields modify the propagation of the jet. Here is the paper.
ABOVE: A more complete 3DMHD implementation (with Flash3.1) of the experiment
described above but after the active phase of jets (two, back-to-back, in this case).
The upper left panel shows the logarithm of the denity.
The upper right panel shows the x velocity component in sound speed units.
The lower left panel shows the logarithm of the magnetic pressure.
The magnetic fields have a random topology and a Kolmogorov energy power spectrum index.
The intensity of the magnetic fields follows the plasma's radial pressure profile as well.
The lower right panel shows the divergence of the magnetic fields and the adaptive grid.
The units are arbitrary.
ABOVE: A similar experiment. A closer look to the jets' cocoon. The jets stop at t=0.015.
These are the XY, XZ and YZ planes intersecting at the origin.
The grid is uniform in this case, with 200x200x200 cells.
There is an error: in the histogram at section "RM maps", the green curve should not be shifted to the right.
ABOVE: 2D axisymmetric hydrodynamical simulations of the
metal advection from a cluster galaxy into the ICM, driven by
the jets of a radio-loud AGN. We implement the ICM with gravity
and a cooling flow, and a central giant galaxy with a metal
distribution, continuous metal formation and powerful intermittent
jets. We model the metals using tracer fluids. The axes show
the distances (in centimeters) and the colours, the logarithm
of the metals (in arbitrary units) implementing the metal
distribution of the central galaxy. The time is given in million
years. The 3 outbursts of the jets advect the metals from the
galaxy into the ICM and produce turbulence and mixing in it. THE
SCALE RANGE CHANGES IN TIME TO FOLLOW
THE EVOLUTION OF THE
FLOWS.
ABOVE: the late phase on the ICM metal advection evolution. The
jets' remnant bubbles transport the metals to distances >
1.5 Mpc
into the cluster. The axes, colour and time
units are the same as for the second animation. Here is the paper.
I used the Flash
code to do these simulations. The first and last movies were made with Visit,
and the other two with IDL and
its Flash library XFlash.