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Kelvin-Helmholtz instability developed in a slab, relativistic flow. Perucho et al., 2005.
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FRI jet evolved during 7 Myrs through a galactic pressure and density profile. The jet power is 1.e44 erg/s. A strong recollimation shock at 1.5 kpc from injection causes entrainment and jet deceleration through the growth of a non-linear KH pinching instability. Perucho & Martí, 2007.
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Axial cuts of the 3D box in the planes perpendicular (left) and
parallel (right) to the jet-star plane of rest-mass density (g/cm^3)
for an inital model of the interaction of a clumpy wind with a
relativistic outflow in a high-mass X-ray binary. Perucho & Bosch-Ramon, 2012.
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Axial cuts of the 3D box in the planes perpendicular (left) and
parallel (right) to the jet-star plane of rest-mass density (g/cm^3)
for one of the simulations at t=1640 seconds. The image shows the
strong interaction between the clumps and the jet. |
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Axial cuts of the
3D box in the planes perpendicular (left) and parallel (right) to the
jet-star plane of axial velocity (cm/s) for one of the simulations at
t=1640 seconds. The image shows the jet deceleration of the jet due to
entrainment of clumps.
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Transversal cuts
of rest-mass density (g/cm^3), axial velocity (cm/s) and Mach number
for one of the simulations at t=1900 s. The cut is done at 3.2 10^{12}
cm from the injection. The color scale of the Mach number has been
saturated at M=5 to show the transition of the flow to transsonic and
subsonic speeds.
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Axial cuts of the
3D box in the planes perpendicular (left) and parallel (right) to the
jet-star plane of rest-mass density (g/cm^3) for a simulation with
three clumps at t=970 seconds. The image shows the strong interaction
between single clumps and the jet.
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Maps of logarithms
of rest-mass density (left) and temperature (right) for a jet
simulation (jet power 1.e46 erg/s) at time 180 Myrs. The figure shows a
mirrored image around the two symmetry axis in the simulation. The
color scale (increasing from blue to red) ranges between densities
7e−32 g/cm^3 and 10e−27 g/cm^3, and temperatures 9.1e6 K and 1.65e9 K.
The main features of the jet are indicated in the figure. The evolution
of a supersonic jet generates a characteristic morphology: i)a
bow-shock that acts on the ambient medium, ii) a terminal or reverse
shock at the head of the jet where the jet flow is decelerated and iii)
the cocoon inflated by the shocked jet particles, typically hotter and
underdense compared with the ambient. The latter region is formed by a
mixture of shocked Intracluster medium and jet materials stirred via
instabilities arising at the contact discontinuity between both media.
Our calculations show it as the origin of the X-ray cavities after a
long term evolution. The whole system can be roughly described by the
simple analytical model (see Perucho, Quilis, Martí, 2011) , which
helps to understand the validity of our numerical results. The
simulations have been performed using the finite-volume code Ratpenat,
which solves the equations of relativistic hydrodynamics in
conservation form using high-resolution-shockcapturing methods. The
code also uses the equation of state of relativistic gas with two
populations of particles, leptons and baryons. The jets are injected in
a grid occupied by an ambient composed by fully ionized Hydrogen gas
(intracluster medium) with a King-like density profile in hydrostatic
equilibrium. The free parameters of the density profile were chosen to
fit 3C 31 X-ray data (Hardcastle et al. 2002) using two King-density
profiles representing the central elliptical galaxy and the cluster.
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Qualitative comparison of an X-ray map of the cluster MS 0735.6+7421
(left, credit: X-ray image: NASA/CXC/Ohio U./B.McNamara et al. 2005;
illustration: NASA/CXC/M.Weiss) and a synthetic X-ray luminosity map
extracted from the simulation shown above (right). Both images display
regions of similar sizes. Although this comparison must be taken with
caution, the main features of both images seem to match remarkably well.
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Movie of the interaction between a relativistic jet and a homogeneous cloud. Bosch-Ramon, Perucho, Barkov (2012).
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Movie of the interaction between a relativistic jet and an inhomogeneous cloud. Bosch-Ramon, Perucho, Barkov (2012).
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