  The helioglow is a fluorescence of interstellar atoms inside the heliosphere,
where they are excited by the solar EUV. Because the mean free path between
collisions for the interstellar gas is comparable to the size of the
heliosphere, the distribution function of this gas inside the heliosphere
strongly varies in space and with time and is non-Maxwellian. Coupling between
realistically modeled solar factors and the distribution function of
interstellar neutral gas is accounted for in a helioglow model that we have
developed. WawHelioGlow is presented in the accompanying Paper I. Here, we
present the evolution of the gas density, solar illumination, helioglow source
function, and other relevant parameters building up the helioglow signal for
selected lines of sight observed at 1 au. We compare these elements for various
phases of the solar cycle and we present the sensitivity of the results to
heliolatitudinal anisotropy of the solar EUV output. We assume a realistic
latitudinal anisotropy of the solar wind flux using results from analysis of
interplanetary scintillations. We compare the simulated helioglow with with
selected maps observed by the SOHO/SWAN instrument. We demonstrate that
WawHelioGlow is able to reproduce fundamental features of the sky distribution
of the helioglow. For some phases of the solar cycle, the model with an
anisotropy of the solar EUV output better reproduces the observations, while
for other phases no EUV anisotropy is needed. In all simulated cases, the solar
wind anisotropy following insight from interplanetary scintillation
measurements is present.
