An analytic model combining turbulent and gravitational length scales reproduces the simulated relation between effective column density and local hydrogen density in molecular clouds.
Astrochemistry: Synthesis and Modelling
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We discuss models that astrochemists have developed to study the chemical composition of the interstellar medium. These models aim at computing the evolution of the chemical composition of a mixture of gas and dust under as- trophysical conditions. These conditions, as well as the geometry and the physical dynamics, have to be adapted to the objects being studied because different classes of objects have very different characteristics (temperatures, densities, UV radia- tion fields, geometry, history etc); e.g., proto-planetary disks do not have the same characteristics as protostellar envelopes. Chemical models are being improved continually thanks to comparisons with observations but also thanks to laboratory and theoretical work in which the individual processes are studied.
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An analytic formalism to describe the $N_{\rm eff}(\rm H)$-$n_{\rm H}$ relationship in molecular clouds
An analytic model combining turbulent and gravitational length scales reproduces the simulated relation between effective column density and local hydrogen density in molecular clouds.