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Figure 1:
Results for the shock heating test of a cold, relativistically inflowing gas against a wall using the explicit Eulerian techniques of Centrella and Wilson [73]. The plot shows the dependence of the relative errors of the density compression ratio versus the Lorentz factor ![]() ![]() ![]() |
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Figure 2:
Godunov’s scheme: local solutions of Riemann problems. At every interface, ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 3:
Schematic profiles of the velocity versus radius at three different times during core collapse: at the point of “last good homology”, at bounce and at the time when the shock wave has just detached from the inner core. |
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Figure 4:
Movie Animations of a relativistic adiabatic core collapse using HRSC schemes (snapshots of the radial profiles of various variables are shown at different times). The simulations are taken from [339]: Velocity evolution. See text for details of the initial model. Visualization by José V. Romero. |
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Figure 4:
Movie Animations of a relativistic adiabatic core collapse using HRSC schemes (snapshots of the radial profiles of various variables are shown at different times). The simulations are taken from [339]: Rest-mass density evolution. See text for details of the initial model. Visualization by José V. Romero. |
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Figure 4:
Movie Animations of a relativistic adiabatic core collapse using HRSC schemes (snapshots of the radial profiles of various variables are shown at different times). The simulations are taken from [339]: Gravitational mass evolution. See text for details of the initial model. Visualization by José V. Romero. |
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Figure 4:
Movie Animations of a relativistic adiabatic core collapse using HRSC schemes (snapshots of the radial profiles of various variables are shown at different times). The simulations are taken from [339]: Lapse (squared) evolution. See text for details of the initial model. Visualization by José V. Romero. |
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Figure 5:
Movie The time evolution of the entropy in a core collapse supernova explosion [190]. The movie shows the evolution within the innermost 3000 km of the star and up to 220 ms after core bounce. See text for explanation. Visualization by Konstantinos Kifonidis. |
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Figure 6:
Movie The time evolution of a relativistic core collapse simulation (model A2B4G1 of [96]). Left: Velocity field and isocontours of the density. Right: gravitational waveform (top) and central density evolution (bottom). Multiple bounce collapse (fizzler), type II signal. The camera follows the multiple bounces. Visualization by Harald Dimmelmeier. |
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Figure 7:
Top panel: time evolution of the normalized four lowest Fourier mode amplitudes for the three-dimensional relativistic core collapse model E20A of [305]. Lower panel: gravitational wave strains ![]() ![]() |
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Figure 8:
Movie An equatorial 2D slice from the Ott et al. [305] 3D simulation of their collapse model E20A that has a post-core-bounce ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 9:
Movie Gravitational radiation from the three-dimensional collapse of a neutron star to a rotating black hole [30]. The figure shows a snapshot in the evolution of the system once the black hole has been formed and the gravitational waves are being emitted in large amounts. See [30] for further details. Visualization made in AEI/ZIB. |
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Figure 10:
Runaway instability of an unstable thick disk: contour levels of the rest-mass density ![]() ![]() ![]() |
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Figure 11:
Development of the MRI in a constant–angular-momentum magnetized torus around a Kerr black hole with ![]() ![]() ![]() ![]() |
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Figure 12:
Jet formation: the twisting of magnetic field lines around a Kerr black hole (black sphere). The yellow surface is the ergosphere. The red tubes show the magnetic field lines that cross into the ergosphere. Figure taken from [197] (used with permission). |
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Figure 13:
Ultrarelativistic outflow from the remnant of the merger of a neutron-star–binary system. The figure shows the gamma-ray burst model B01 from [8] corresponding to a time ![]() ![]() ![]() ![]() ![]() |
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Figure 14:
Relativistic wind accretion onto a rapidly-rotating Kerr black hole ( ![]() ![]() ![]() ![]() ![]() |
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Figure 15:
Movie The time evolution of the accretion/collapse of a quadrupolar shell onto a Schwarzschild black hole. The left panel shows isodensity contours and the right panel the associated gravitational waveform. The shell, initially centered at ![]() |
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Figure 16:
Movie The time evolution of the bar-mode instability of one of the differentially rotating neutron-star models of [29]. The animation depicts the distribution of the rest-mass density. The exponential growth of the instability, which is followed by its saturation, the development of spiral arms, and the attenuation of the bar deformation, is all clearly visible in the movie. The last part of the dynamics is dominated by an almost axisymmetric configuration. Visualization developed at SISSA. Used with permission. |
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Figure 17:
Movie An animation of a headon collision simulation of two ![]() ![]() ![]() |
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Figure 18:
Isodensity contours in the equatorial plane for the merger of a ![]() ![]() ![]() |
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