Movie 1 – xObs-yObs Intensity Movie from TObs=2000M-2400M

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 b_μb^μ (where u_g is the gas internal energy).

Movie 2 – Black Hole/Accretion Disk from Rotating Vantage Points

These images show intensity maps of emissivity j ~ b_μb^μ 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.

Movie 3 – Jet intensity Movie Viewed from 30°

This movie is shown with the jet axis from a large inclination angle from the (parallel) lines of sight to emphasize the jet. The jet emissivity is j ~ D^2.5b_μb^μ  , where D is the Doppler factor,  at observer angle 30° and observer times T_Obs=1600M-2500M. Regions above 0.005 the maximum intensity are white.

Movie 4 – Intensity Map for j ~ D^2.5b_μb^μ Viewed 15° from Jet Axis

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

Intensity map movies for j ~ D^2.5b_μb^μ  with 30° viewing angle. 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~(b_μ b^μ)^.75 from (θ_Obs ,ϕ_Obs) = (15°,0°) (top), the energy density per unit mass cut  u_g/ρ >0.1 is made to exclude points outside the contour shown in the bottom movie. I use t_Step=56M = 21 days 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 r_G(M_M87)/c) using emissivity prescription j=(b_μb^μ) ^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 43 GHz VLA observations) is indicative of a magnetic Kelvin-Helmholtz instability.

Movie 8 – Current Density Model Jet

In this model, a synchrotron emissivity

j~P_g b^(1+p)/2 ν^(p-1)/2

is used where the pressure P_g due to gas radiating at the observed frequency is related to dissipation by setting

P_g ~ (D_x B_y -D_y B_x )²_z ,

where the z-component of the curl of the magnetic field is the current density along the jet axis. The movie is viewed from (θ_Obs ,ϕ_Obs) = (15°,0°).

Movie 9 – Alpha Model Jet

Movie 10 – Shear Model Jet