In certain scenarios, the accreted angular momentum of plasma onto a black
hole could be low; however, how the accretion dynamics depend on the angular
momentum content of the plasma is still not fully understood. We present
three-dimensional, general relativistic magnetohydrodynamic simulations of low
angular momentum accretion flows around rapidly spinning black holes (with spin
$a = +0.9$). The initial condition is a Fishbone-Moncrief (FM) torus threaded
by a large amount of poloidal magnetic flux, where the angular velocity is a
fraction $f$ of the standard value. For $f = 0$, the accretion flow becomes
magnetically arrested and launches relativistic jets but only for a very short
duration. After that, free-falling plasma breaks through the magnetic barrier,
loading the jet with mass and destroying the jet-disk structure. Meanwhile,
magnetic flux is lost via giant, asymmetrical magnetic bubbles that float away
from the black hole. The accretion then exits the magnetically arrested state.
For $f = 0.1$, the dimensionless magnetic flux threading the black hole
oscillates quasi-periodically. The jet-disk structure shows concurrent revival
and destruction while the gas outflow efficiency at the event horizon changes
accordingly. For $f \geq 0.3$, we find that the dynamical behavior of the
system starts to approach that of a standard accreting FM torus. Our results
thus suggest that the accreted angular momentum is an important parameter that
governs the maintenance of a magnetically arrested flow and launching of
relativistic jets around black holes.

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