Movies for Figure 4 in "She's Got Her Mother's Hair: End-to-End Collapsar Simulations Unveil the Origin of Black Holes' Magnetic Field, (#AAS56924)"

<p>There are 10 videos: Six 2D vertical maps of the logarithmic mass density and four 3D renderings of the disk density (red) and jet magnetization (blue). In the 2D maps, the black contours outline the magnetic field lines, where solid and dashed lines delineate positive and negative magnetic polarity, respectively.</p> <p>The filenames correspond to the model names in the paper:</p> <p>Model a9&Phi;hD includes a rapidly spinning black hole with a high magnetic flux reservoir and large angular momentum to form a disk.</p> <p>Model a9&Phi;hI includes a rapidly spinning black hole with a high magnetic flux reservoir and small angular momentum that does not form a disk.</p> <p>Model a1&Phi;hD includes a slowly spinning black hole with a high magnetic flux reservoir and large angular momentum to form a disk.</p> <p>Model a9&Phi;lD includes a rapidly spinning black hole with a low magnetic flux reservoir and large angular momentum to form a disk.</p> <p>Model a5&Phi;lD includes a moderately spinning black hole with a low magnetic flux reservoir and large angular momentum to form a disk.</p> <p>Model a1&Phi;lD includes a slowly spinning black hole with a low magnetic flux reservoir and large angular momentum to form a disk.</p> <p>BHs with higher spins and magnetic fluxes retain the remnant poloidal field of the PNS to maintain steady jet launching. When the BH spin and the initial flux on the BH are low, or an accretion disk is absent (model a9&Phi;hI), the BH cannot sustain a large-scale field. As a result, magnetic loops of opposite polarity are accreted onto the BH, causing the BH magnetic flux to reconnect and reduce the flux on the BH, resulting in the depletion of jets.</p>