in Tab. \[tab:cosmic ray photodissociation rates\]. This rate is dependent on the local physical conditions, and a set of base conditions is chosen which plausibly simulate the interior of a dark interstellar cloud:

-   The assumed abundances of and CO relative to $n_\mathrm{H}=n(\ce{H})+{2}n(\ce{H2})$ are $10^{-5}$ and $7\times10^{-5}$, respectively, and reflect typical dense cloud abundances [@aikawa2008].

-   A $\mathrm{{}^{14}N_2}\!:\!\mathrm{{}^{14}N{}^{15}N}$ ratio of 225 is chosen, appropriate for the solar elemental ratio of 450 [@marty2010].

-   All molecular species are assumed to have a thermal excitation of $T_\mathrm{ex}=20\,\mathrm{K}$ and be turbulently broadened with Doppler velocity $b=1\,\mathrm{km\,s^{-1}}$.

-   Dust grains are assumed to have a scattering cross section per H nucleus of $x_\mathrm{dust}\sigma^\text{abs}_\mathrm{dust} = 10^{-21}\,\mathrm{cm^2}$.

-   The high temperature limit, 3:1, is assumed for the ortho:para ratio of emitting H$_2$.

Further calculations listed in Tab. \[tab:cosmic ray photodissociation rates\] probe variations on this set of parameters.

For the base set of parameters considered in Tab. \[tab:cosmic ray photodissociation rates\], the photodissociation rate is $\mathrm{14\times10^{-16}\,s^{-1}}$. This is 5 orders of magnitude below the rate calculated for a standard interstellar radiation field in Sec. \[sec:pd rates\]. The cosmic-ray induced photodissociation rates calculated by @gredel1989 for a large number of other molecular species are generally larger than 