A simple approach to CO cooling in molecular clouds
  CO plays an important role in interstellar molecular clouds, both as a
coolant, and as a diagnostic molecule. However, a proper evaluation of the
cooling rate due to CO requires a determination of the populations of many
levels, the spontaneous and stimulated radiative de-excitation rates between
these levels, and the transfer of the emitted multi-line radiation;
additionally, this must be done for three isotopologues. It would be useful to
have a simple analytic formulation that avoided these complications; this could
then be used in situations where CO plays an important role as a coolant, but
the details of this role are not the main concern. We derive such a formulation
here, by first considering the two asymptotic forms that obtain in the limits
of (a) low volume-density and optical depth, and (b) high volume-density and
optical depth. These forms are then combined in such a way as to fit the
detailed numerical results from Goldsmith \& Langer (1978), which cover low
temperatures, and a range of physical conditions where the interplay of thermal
and sub-thermal excitation, optical-depth effects, and the contributions from
rare isotopologues, are all important. The fit is obtained using the
Metropolis-Hastings method, and reproduces the results of GL78 well. It is a
purely local and analytic function of state --- specifically a function of the
density, $\rho$, isothermal sound speed, $a$, CO abundance, $X_{_{\rm CO}}$,
and velocity divergence, $\nabla\cdot{\boldsymbol\upsilon}$. As an application,
we consider the cooling layer following a slow steady non-magnetic planar
J-shock. We show that, if the post-shock cooling is dominated by CO and its
isotopologues, the thickness of the post-shock cooling layer is very small and
approximately independent of the pre-shock velocity, $\upsilon_o$, or pre-shock
isothermal sound speed, $a_o$.
