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Дата индексирования: Mon Oct 1 19:43:14 2012
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Martín Huarte-Espinosa

Research Student
Room 919 Rutherford Building
Cavendish Laboratory
JJ Thomson Avenue
Cambridge CB3 0HE
Telephone: (+44) (0)1223 339991
Fax: (+44) (0)1223 354599
mh475@mrao.cam.ac.uk
Here is my CV
Here is a list of my publications
My recent talks
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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.
Here is the poster that I presented at "Physics of galactic nuclei."
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.
Thanks for reading.
Last update: 25 June '09.