Case D: Magnetized and Neutrinos (Simplified)
Here we look at the time evolution of the rest-mass density and magnetic fields. The binaries consist of identical irrotational neutron stars, each of rest-mass $M_{0}$ = 1.51 $M_{\odot}$, with total ADM mass M = 2.7 $M_{\odot}$. The rest-mass density is normalized to its initial central value. Time is measured in $M = 1.32 \times 10^{-2} \rm ms$. The neutron stars spiral inwards, forming a hypermassive neutron star (HMNS) and a disk of matter that orbits it. Shortly after merger, we insert neutrino transfer using a simplified M1 closure scheme that only evolves one neutrino species ($\bar{\nu}_e$) and considers only charged-current interactions. Eventually the HMNS undergoes delayed collapse, and a BH is formed. We can see the magnetic field lines (white lines) become collimated above and below the BH, and that matter is ejected at mildly relativistic speeds (green arrows). The field lines above the poles form a helical funnel which drives and confines the matter in the jet. The BH remnant has a final spin of $a_{BH}/M_{BH} \approx 0.69$.
 Fig. 1-1: Density and Magnetic Fields |
 Fig. 1-2: Density and Magnetic Fields |
 Fig. 1-3: Density and Magnetic Fields |
 Fig. 1-4: Density and Magnetic Fields |
 Fig. 1-5: Density and Magnetic Fields |
 Fig. 1-6: Density and Magnetic Fields |
