  Hydrogen loss to space is a key control on the evolution of the Martian
atmosphere and the desiccation of the red planet. Thermal escape is thought to
be the dominant loss process, but both forward modeling studies and remote
sensing observations have indicated the presence of a second,
higher-temperature "nonthermal" or "hot" hydrogen component, some fraction of
which also escapes. Exothermic reactions and charge/momentum exchange processes
produce hydrogen atoms with energy above the escape energy, but H loss via many
of these mechanisms has never been studied, and the relative importance of
thermal and nonthermal escape at Mars remains uncertain. Here we estimate
hydrogen escape fluxes via 47 mechanisms, using newly-developed escape
probability profiles. We find that HCO$^+$ dissociative recombination is the
most important of the mechanisms, accounting for 30-50% of the nonthermal
escape. The reaction CO$_2^+$ + H$_2$ is also important, producing roughly as
much escaping H as momentum exchange between hot O and H. Total nonthermal
escape from the mechanisms considered amounts to 39% (27%) of thermal escape,
for low (high) solar activity. Our escape probability profiles are applicable
to any thermospheric hot H production mechanism and can be used to explore
seasonal and longer-term variations, allowing for a deeper understanding of
desiccation drivers over various timescales. We highlight the most important
mechanisms and suggest that some may be important at Venus, where nonthermal
escape dominates and much of the literature centers on charge exchange
reactions, which do not result in significant escape in this study.
