  The intracluster medium of a galaxy cluster often shows an extended
quasi-spiral structure, accentuated by tangential discontinuities known as cold
fronts (CFs). These discontinuities are thought to isolate between low-entropy,
high-metallicity gas inside (i.e., below) the CF that was lifted from the
center of the cluster by some radial factor $f_i$, and high-entropy,
low-metallicity gas outside the CF that was pushed inward by a factor $f_o$. We
find broad support for such a picture, by comparing the entropy and metallicity
discontinuities with the respective azimuthal averages, using newly deprojected
thermal profiles in clusters A2029, A2142, A2204 and Centaurus, supplemented by
deprojected CFs from the literature. In particular, the mean advection factors
$f_K$ and $f_Z$, inferred respectively from entropy and metallicity, strongly
correlate ($\mathcal{R}=0.7^{+0.2}_{-0.3}$) with each other, consistent with
large-scale advection. However, unlike sloshing simulations, in which the
inside/outside phases are an inflow/outflow settling back to equilibrium after
a violent perturbation, our results are more consistent with an outflow/inflow,
with the fast, Mach $\mathcal{M}_i\sim0.8$ gas inside the CF being a rapidly
heated or mixed outflow, probably originating from the cD galaxy, and gas
outside the CF being a $\mathcal{M}_o\sim0.03$, slowly-cooling inflow. In
particular, entropy indicates an outside advection factor $f_{Ko}\simeq
1.33\pm0.04$ that is approximately constant in all CFs, gauging the distance
traversed by inflowing gas within a cooling time. In contrast, $1.1\lesssim
f_{Ki}\lesssim 2.5$ and $1\lesssim f_Z\lesssim 17$ vary considerably among
clusters, and strongly correlate ($3.1\sigma\text{-}4.2\sigma$) with the virial
mass, $f_{Ki}\propto M_{200}^{0.14\pm0.07}$ and $f_Z\propto
M_{200}^{1.4\pm0.4}$, suggesting that each cluster sustains a quasi-steady
spiral flow.
