  During the formation of the large scale structure of the Universe, matter
accretes onto high density peaks. Accreting collisionless dark matter (DM)
forms caustics around them, while accreting collisional baryonic matter (BM)
forms accretion shocks. The properties of the accreting matter depend upon the
power spectrum of the initial perturbations on a given scale as well as the
background expansion in a given cosmological model. In this paper, we have
calculated the accretion of DM particles in one-dimensional spherical geometry
under various cosmological models including the Einstein-de Sitter universe,
the open universe with $\Omega_o<1$, and the flat universe with
$\Omega_{\Lambda}=1-\Omega_o$. A density parameter in the range $0.1\le
\Omega_o \le 1$ has been considered. The initial perturbation characterized by
a point mass at the origin has been considered. Since the accretion shock of BM
is expected to form close to the first caustic of DM, the properties of the
accreting BM are common with those of the DM. Hence, the accretion calculations
with DM particles have been used to find the position and velocity of the
accretion shock and the cluster mass inside it. The average temperature of BM
has been estimated by adopting simplifying assumptions. The velocity of the
accreting BM around clusters of a given temperature is smaller in a universe
with smaller $\Omega_o$, but only by up to $\sim24\%$ in the models with
$0.1\le \Omega_o \le 1$. Thus, it would be difficult to use that quantity to
discriminate among the cosmological models. However, the accretion velocity
around clusters of a given mass or a given radius depends more sensitively on
the cosmological models. It is smaller in a universe with smaller $\Omega_o$ by
up to $\sim41\%$ and $\sim65\%$, respectively. So, it can provide a better
