  We study the X-ray cluster gas density distribution in hydrostatic
equilibrium using the universal temperature profile obtained from recent
simulations involving only gravitational processes. If this temperature profile
is an indicator of the influence of gravitational processes alone on the
intracluster medium, then the comparison of various X-ray parameters expected
from this profile and the observed data would point towards any additional
physics that may be required. We compare the entropy at 0.1 R_{200} and
R_{500}, the scaled entropy profile, the gas fraction at 0.3 R_{200} and the
gas fraction profile with recent observations and discuss the implications of
this temperature profile in light of these data. We find that the entropy
imparted to the gas from gravitational processes alone is larger than
previously thought. The entropy at R_{500} for rich clusters is consistent with
data, whereas the entropy at 0.1R_{200} is still less than the observed values.
We also find that the gas fraction in the inner region of clusters, expected
from gravitational processes alone, is smaller than previously thought but
larger than the observed data. It does show a trend with the emission-weighted
temperature (<T>) as shown by data. We therefore find that the role of any
additional non-gravitational process influencing the physical state of ICM
would have to be revised in light of these findings.
