Author: Monika Moscibrodzka
Left panel (top and bottom): model image of a black hole generated by light ray-tracing through plasma falling onto the black hole. The plasma model is based on supercomputer simulations of general relativistic magnetohydrodynamics. Here the colors code the light intensity (red/brighter being more intense and blue/dimmer less intense). Right panel (top and bottom): the same image as in the left but here the image is blured with a brush strokes. The direction of each brush stroke is perpendicular to the local light polarization plane. What does this mean? This means that the brush strokes follow the magnetic field structure responsible for the visible emission. In sum: left panel shows intensity of light and right panel shows intensity of light and magnetic field lines producing it. Method used to create brush strokes is called Line Integral Convolution (Carbal & Leedom 1993). Codes used to generate these visualizations: ipole (Moscibrodzka & Gammie 2018) and ipole-lic (Moscibrodzka 2020). These visualisations are nicknamed "v. Strokes" because they resemble v. Gogh paitings style.
Author: Monika Moscibrodzka
Movie
Click on the slide above to see how accreting black hole looks like for an observer that is orbiting around the black hole being embedded in accretion disk. The observer orbit is shown in the left panel in the figure above. This movie is based on state-of-the-art general relativistic MHD simulations combined with relativistic radiative transfer model.
Model of a Jet in M87 Galaxy
A model of relativistic jet in M87 galaxy seen at a various viewing angles. Effects of relativistic abberation (beaming of light towards the direction of motion) can be clearly seen.