Ray Traced Cosmos++ Movies
We are in the process of performing time-dependent radiative transfer on data from global, 3D, general relativistic MHD simulations of a tilted black hole accretion flow from the code Cosmos++. Using Geokerr, we compute photon orbits in a Kerr spacetime for a grid of rays, and solve the radiative transfer equation for desired emission and absorption coefficients in the region where the rays intersect the accretion flow. This creates a coordinate-independent observed image of the black hole. Repeating the procedure at many at many simulation time steps produces movies.
This analysis has been carried out in full for two models thus far: optically thin line emission, with the emissivity proportional to the fluid mass density, and a model with emissivity proportional to rho*T.
Movies of optically thin line emission at two observer inclinations. The panel size is 50x40M for i=60 degrees and 50x50M for i=0.
[60 degrees] [0 degrees (face on)]
Here are the equivalent movies of the untilted simulation.
[60 degrees] [0 degrees (face on)]
Movies of the rho*T emissivity at two observer inclinations. The panel size is the same as before.
[60 degrees] [0 degrees (face on)]
Here are the equivalent movies of the untilted simulation.
[60 degrees] [0 degrees (face on)]
Next, we consider optically thin synchrotron emission for galactic center black hole parameters at four frequencies and two observer inclinations. The panel size is now 30M.
| 3 GHz | [60 degrees] | [0 degrees] | 30 GHz | [60 degrees] | [0 degrees] |
| 300 GHz | [60 degrees] | [0 degrees] |
| 3000 GHz | [60 degrees] | [0 degrees] |
Finally, some of this preliminary work was presented as a poster (ppt pdf) at the 213th AAS Meeting in Long Beach.