This movie shows the simulation region projected onto an observer plane 80 gravitational radii (M) on a side (with axes in units of the simulation datablock spatial step xStep = yStep = 80M/256) looking directly along the jet axis. Emission from the accretion disk (seen rotating counterclockwise) dominates jet emission in this zero opacity case with optically thin synchrotron emissivity j~u_g bμbμ (where ug is the gas internal energy).
These images show intensity maps of emissivity j~bμbμ viewed along the jet axis then almost at a right inclination angle from the jet axis. In the latter image, horizon scale features are visible.
This movie is shown with the jet axis from a large inclination angle from the (parallel) lines of sight to emphasize the jet.
The images are shown here in rainbow and disk masked (by setting the middle fifth band of the simulated region in the direction away from the observer to zero) to accentuate coherent motion of high intensity regions of the jet outflow.
Movie 5 – Azimuthal Variation
These four panel image maps simultaneously show the jet from vantage points tilted 15° in the polar direction from the jet axis at varying azimuths 0° (top left), 90° (top right), 180° (bottom left) and 270° (bottom right).
Movies 6A and 6B – Energy Density Cuts
In the 11-frame movies of j~(bμ bμ).75 from (θObs ,ϕObs) = (15°,0°) (top), the energy density per unit mass cut ug/ρ >0.1 is made to exclude points outside the contour shown in the bottom movie. I use tStep=56M = 21days for M based on the gravitational radius of M87.
Movie 7 – Corkscrewing Jet
A movie derived from a model of observations of the M87 jet by the VLA with 21 days (= 56 rG(MM87)/c) using emissivity prescription j=(bμbμ) 3/4 and a geometric cut of simulation regions |z|<20M and 0.5|z|<x2+y2 to make jet substructure prominent. Note the helical magnetic field structure corkscrewing outward (as seen in some 43GHz VLA observations) is indicative of a magnetic Kelvin-Helmholtz instability.
Movie 8 – Current Density Model Jet
In this model, a synchrotron emissivity
j~Pg b(1+p)/2 ν(p-1)/2
is used where the pressure Pg due to gas radiating at the observed frequency is related to dissipation by setting
Pg ~ (Dx By -Dy Bx )2z ,
where the z-component of the curl of the magnetic field is the current density along the jet axis. The movie is viewed from (θObs ,ϕObs) = (15°,0°).