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MOVIE GALLERY

The movies are from hydrodynamic and MHD simulations using either the FLASH or PLUTO code on a variety of supercomputers, including the IBM Sp5, Sp6, and the Linux clusters CLX and BCX hosted at CINECA (Italy), the Linux clusters hosted at the HPC facility SCAN of INAF-OAPA (Italy), and the Grid Infrastructure of Consorzio COMETA (Italy). More details regarding the science can be found by following the links given with each item.

Crushing of interstellar gas clouds in supernova remnants.
I. The role of thermal conduction and radiative losses
(Orlando et al. 2005, A&A 444, 505)

3-D visualizations of the mass density evolution during the shock-cloud interaction. The movies show the density distributions, in log scale.
More details

NUMERICAL CODE: FLASH

movie 1, movie 2, movie 3

Crushing of interstellar gas clouds in supernova remnants.
II. X-ray emission
(Orlando et al. 2006, A&A 457, 545)

Evolution of the X-ray emission originating from the shock-cloud interaction as derived from models with (model RCm50c10) or without (model HYm50c10) thermal conduction and radiative losses.
More details

NUMERICAL CODE: FLASH

movie 1, movie 2, movie 3

The importance of magnetic-field-oriented thermal conduction in the interaction of SNR shocks with interstellar clouds
(Orlando et al. 2008, ApJ 678, 274)

2.5D MHD simulations of a shock impacting on an isolated gas cloud, including anisotropic thermal conduction and radiative cooling. The movies show the evolution of mass density distribution in log scale for simulations with different initial magnetic field orientation.
More details

NUMERICAL CODE: FLASH

movie 1, movie 2, movie 3

Three-dimensional modeling of the asymmetric blast wave from the 2006 outburst of RS Ophiuchi: Early X-ray emission
(Orlando et al. 2009, A&A 493, 1049)

3D hydrodynamic simulations of the blast wave from the 2006 outburst, propagating through the inhomogeneous CSM. The movies show the evolution of 3D spatial distribution of mass density, in log scale, and the corresponding evolution of X-ray emission.
More details

NUMERICAL CODE: FLASH

movie 1, movie 2, movie 3

X-ray emitting MHD accretion shocks in classical T Tauri stars. Case for moderate to high plasma-beta values
(Orlando et al. 2010, A&A 510, A71)

2D axisymmetric MHD simulations of an accretion stream impacting onto the chromosphere of a CTTS. The movies show the mass density (left) and temperature (right) in simulations with different plasma beta
More details

NUMERICAL CODE: PLUTO

movie 1, movie 2, movie 3

3-D Modeling of X-ray Mixed Morphology Supernova Remnants with Enhanced Metallic Abundances
(Orlando et al. 2009, Il Nuovo Cimento C 32, 45)

3-D MHD simulations of the blast wave of a SN explosion, taking into account the thermal conduction and the radiative cooling, and following the evolution of the CSM-ejecta mixing.
More details

NUMERICAL CODE: FLASH

movie 1, movie 2

The early blast wave of the 2010 explosion of U Scorpii
(Drake & Orlando 2010, ApJ 720, L195)

3D hydrodynamic simulations of the early blast wave of the 2010 explosion of U Scorpii. The movie shows the first five minutes of evolution of 3D spatial distribution of mass density, in log scale. The ejecta material is marked in brown.
More details

NUMERICAL CODE: FLASH

movie

Mass accretion to young stars triggered by flaring activity in circumstellar disks
(Orlando S. et al. 2011, MNRAS 415, 3380)

3D MHD simulation describing a flare occurring close to the circumstellar disk of a classical T Tauri star. The model includes the effects of gravity, radiative cooling, magnetic-field-oriented thermal conduction, disk viscosity.
More details

NUMERICAL CODE: PLUTO

movie