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We investigate the increase of the DEM (differential emission measure)towards the chromosphere due to small and cool magnetic loops (height$\lesssim8$~Mm, $T\lesssim10^5$~K). In a previous paper we analysed theconditions of existence and stability of these loops through hydrodynamicsimulations, focusing on their dependence on the details of the optically thinradiative loss function used. In this paper, we extend those hydrodynamicsimulations to verify if this class of loops exists and it is stable when usingan optically thick radiative loss function. We study two cases: constantbackground heating and a heating depending on the density. The contribution tothe transition region EUV output of these loops is also calculated andpresented. We find that stable, quasi-static cool loops can be obtained byusing an optically thick radiative loss function and a background heatingdepending on the density. The DEMs of these loops, however, fail to reproducethe observed DEM for temperatures between $4.6<\log T<4.8$. We also show thetransient phase of a dynamic loop obtained by considering constant heating rateand find that its average DEM, interpreted as a set of evolving dynamic loops,reproduces quite well the observed DEM.

Modelling solar low-lying cool loops with optically thick radiative losses