  Galaxy evolution can be dramatically affected by the environment, especially
by the dense environment of a galaxy cluster. Recent observational studies show
that massive galaxies undergoing strong ram pressure stripping (RPS) also show
an enhanced frequency of nuclear activity. Here, we investigate this topic
using a suite of wind-tunnel hydrodynamical simulations of an individual
massive $M_\text{star} = 10^{11} M_\odot$ disk galaxy with 39 pc resolution and
including star formation and stellar feedback. We find that RPS increases the
inflow of gas to the galaxy centre regardless of the wind impact angle. This
increase is driven by the mixing of interstellar and non-rotating intracluster
media at all wind angles, and by increased torque on the inner disk gas, mainly
from local pressure gradients when the ICM wind has an edge-on component. In
turn, the increase in pressure torques is driven by rising gradient of ram
pressure. We estimate the black hole (BH) accretion using Bondi-Hoyle and
torque models, and compare it with the mass flux in the central 140 pc region.
We find that the torque model estimates much less accretion onto the BH of a
RPS galaxy than the Bondi-Hoyle estimator. However, we argue that both models
are incomplete because the commonly used torque model does not account for
torques caused by the gas distribution or local pressure gradients and the
Bondi-Hoyle estimator depends on the the sound speed of the hot gas, which
includes the ICM in stripped galaxies, thus a new estimator would be required.
