  We analyse $\textit{XMM-Newton}$ RGS spectra of Wolf-Rayet (WR) 140, an
archetype long-period eccentric WR+O colliding wind binary. We evaluate the
spectra of O and Fe emission lines and find that the plasmas emitting these
lines have the largest approaching velocities with the largest velocity
dispersions between phases 0.935 and 0.968 where the inferior conjunction of
the O star occurs. This behaviour is the same as that of the Ne line-emission
plasma presented in our previous paper. We perform diagnosis of electron number
density $n_{\rm e}$ using He-like triplet lines of O and Ne-like Fe-L lines.
The former results in a conservative upper limit of $n_{\rm e} \lesssim
10^{10}$-10$^{12}$ cm$^{-3}$ on the O line-emission site, while the latter can
not impose any constraint on the Fe line-emission site because of statistical
limitations. We calculate the line-of-sight velocity and its dispersion
separately along the shock cone. By comparing the observed and calculated
line-of-sight velocities, we update the distance of the Ne line-emission site
from the stagnation point. By assuming radiative cooling of the Ne
line-emission plasma using the observed temperature and the local stellar wind
density, we estimate the line-emission site extends along the shock cone by at
most $\pm$58 per cent (phase 0.816) of the distance from the stagnation point.
In this framework, excess of the observed velocity dispersion over the
calculated one is ascribed to turbulence in the hot-shocked plasma at earlier
orbital phases of 0.816, 0.912, and 0.935, with the largest velocity dispersion
of 340-630 km s$^{-1}$ at phase 0.912.
