  This is the second paper of our series of works of studying the effects of
active galactic nuclei (AGN) feedback on the cosmological evolution of an
isolated elliptical galaxy by performing two-dimensional high-resolution
hydrodynamical numerical simulations. In these simulations, the inner boundary
is chosen so that the Bondi radius is resolved. Physical processes like star
formation, SNe Ia and II are taken into account. Compared to previous works,
the main improvements is that we adopt the most updated AGN physics, which is
described in detail in the first paper of this series (Yuan et al. 2018, Paper
I). These improvements include the discrimination of the two accretion modes of
the central AGN and the most updated descriptions of the wind and radiation in
the two modes. In Paper I, we consider the case that the specific angular
momentum of the gas in the galaxy is very low. In this paper, we consider the
case that the specific angular momentum of the gas is high. In the galactic
scale, we adopt the gravitational torques raised due to non-axisymmetric
structure in the galaxy as the mechanism of the transfer of angular momentum of
gas, as proposed in some recent works. Since our simulations are axisymmetric,
we make use of a parameterized prescription to mimic this mechanism. Same as
Paper I, we investigate the AGN light curve, typical AGN lifetime, growth of
the black hole mass, AGN duty-cycle, star formation, and the X-ray surface
brightness of the galaxy. Special attention is paid to the effects of specific
angular momentum of the galaxy on these properties. We find that some results
are qualitatively similar to those shown in Paper I, while some results such as
star formation and black hole growth do show a significant difference due to
the mass concentration in the galactic disk as a consequence of galactic
rotation.
