  The conventional accretion disk lore is that magnetized turbulence is the
principal angular momentum transport process that drives accretion. However,
when dynamically important large-scale magnetic fields thread an accretion
disk, they can produce mass and angular momentum outflows, known as winds, that
also drive accretion. Yet, the relative importance of turbulent and wind-driven
angular momentum transport is still poorly understood. To probe this question,
we analyze a long-duration ($1.2 \times 10^5 r_{\rm g}/c$) simulation of a
rapidly rotating ($a=0.9$) black hole feeding from a thick ($H/r\sim0.3$),
adiabatic, magnetically arrested disk (MAD), whose dynamically important
magnetic field regulates mass inflow and drives both uncollimated and
collimated outflows (i.e., winds and jets, respectively). By carefully
disentangling the various angular momentum transport processes within the
system, we demonstrate the novel result that disk winds and disk turbulence
both extract roughly equal amounts of angular momentum from the disk. We find
cumulative angular momentum and mass accretion outflow rates of $\dot{L}\propto
r^{0.9}$ and $\dot{M}\propto r^{0.4}$, respectively. This result suggests that
understanding both turbulent and laminar stresses is key to understanding the
evolution of systems where geometrically thick MADs can occur, such as the hard
state of X-ray binaries, low-luminosity active galactic nuclei, some tidal
disruption events, and possibly gamma-ray bursts.
