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Black hole (BH) accretion flows and jets are dynamic hot relativisticmagnetized plasma flows whose radiative opacity can significantly affect flowstructure and behavior. We describe a numerical scheme, tests, and anastrophysically relevant application using the M1 radiation closure within anew three-dimensional (3D) general relativistic (GR) radiation (R)magnetohydrodynamics (MHD) massively parallel code called HARMRAD. Our 3DGRRMHD simulation of super-Eddington accretion (about $20$ times Eddington)onto a rapidly rotating BH (dimensionless spin $j=0.9375$) shows sustainednon-axisymmemtric disk turbulence, a persistent electromagnetic jet driven bythe Blandford-Znajek effect, and a total radiative output consistently near theEddington rate. The total accretion efficiency is of order $20\%$, thelarge-scale electromagnetic jet efficiency is of order $10\%$, and the totalradiative efficiency that reaches large distances remains low at only order$1\%$. However, the radiation jet and the electromagnetic jet both emerge froma geometrically beamed polar region, with super-Eddington isotropic equivalentluminosities. Such simulations with HARMRAD can enlighten the role of BH spinvs.\ disks in launching jets, help determine the origin of spectral andtemporal states in x-ray binaries, help understand how tidal disruption events(TDEs) work, provide an accurate horizon-scale flow structure for M87 and otheractive galactic nuclei (AGN), and isolate whether AGN feedback is driven byradiation or by an electromagnetic, thermal, or kinetic wind/jet. For example,the low radiative efficiency and weak BH spin-down rate from our simulationsuggest that BH growth over cosmological times to billions of solar masses byredshifts of $z\sim 6-8$ is achievable even with rapidly rotating BHs and tensolar mass BH seeds.

monthly notices of the royal astronomical society

Three-Dimensional General Relativistic Radiation Magnetohydrodynamical  Simulation of Super-Eddington Accretion, using a new code HARMRAD with M1  Closure