The important role of H2O as a source of odd hydrogen on Mars should now be clear and Water photochemistry also regulates the escape of hydrogen. The water vapor concentrations observed in the Martian atmosphere are strongly dependent on the local temperature and therefore, on altitude, latitude, and time of day. Most atmospheric H2O is probably confined near the surface by vapor pressure limitations, where it is destroyed by photodissociation and by reaction with energetic O (1D) from ozone photolysis:
O (1D) + H2O ® OH + OH
The odd hydrogen produced by these processes is rapidly cycled through H, OH, and HO2. The odd hydrogen sinks are:
H + HO2 ® H2O + O
® H2 + O2
HO2 + HO2 ® H2O2
HO2 + OH ® H2O + O2
The hydrogen peroxide produced here may either freeze out in the polar regions or photodissociate to reform odd hydrogen. The spectroscopic observations from the probe to Mars suggest that the O2 abundance exceed the CO abundance on Mars; the O2 generated by water photochemistry is the only possible source of this additional oxygen. In a dry CO2 atmosphere O2 abundance to be one half that of CO.
Frost on the Martian Surface
Reaction cycles that generate hydrogen gas, however, raise the question of atmospheric escape from Mars. Molecular hydrogen is generated by reaction of H with HO2, both of which are products of H2O photodissociation in the lower atmosphere. Some H2 is removed by O (1D) + H2 ® OH + H near the ground, leading next to water vapor, and also, in the ionosphere, by
CO2+ + H2 ® COOH+ + H
COOH+ + e- ® CO2 + H
H2 + hv ® H + H
Photolysis of molecular hydrogen requires rare photons with l < 850 Ĺ, which penetrate poorly through carbon dioxide. Thus almost all H2 photolysis occurs at altitudes above about 80 km, close to the top of the atmosphere.
In a steady state, the outward flux of hydrogen must be balanced by the production of H2 from H2O. This production rate is hard to estimate because of poorly known rate constants and the unknown catalytic effects of the ground and atmospheric aerosols on several important reactions. The total amount of water vapor that would be destroyed on Mars if the present escape flux of H atoms were sustained over the lifetime of the planet is about one thousandth of the water in the oceans on Earth today. This small water loss will certainly not have noticeably depleted Martian water resources. The other product of water photolysis, O2, does present a problem. With the observed escape rate of H, photolysis will produce the observed O2 amount in just 105 years.
Similarly, the calculated oxygen atom escape rate is in remarkable agreement with the production rate of O from H2O photodissociation inferred from the present H escape rate. This balance is no coincidence, but is in fact expected from the buffering effect of molecular hydrogen. It these escape rates have remained constant over geologic time, comparison of the total water lost by this mechanism with the total CO2 present in the atmosphere can be made. The inferred H2O: CO2 ratio in the outgassing of Mars is about 45:1. Comparison of the water content of Earth’s oceans with the CO2 in sedimentary carbonates on Earth actually yields a similar ratio. However, there are a number of cosmochemical reasons for expecting the H2O: CO2 ratio on Mars to considerably exceed that on Earth. It so, there must exit H2O removal mechanisms much more potent than atmospheric escape.
The escape of H2, operating together with the mechanisms for removing O2 from the atmosphere, results in net loss of H2O. This loss rate is limited by the average H2O photolysis rate, 109 molecules cm-2 s –1. Solar wind sweeping may also be a contribution to escape from the Martian atmosphere. Ions are produced by photo-ionization and by charge exchange with solar wind protons near the planetary limb. These ions, which include O2+, CO2+, O+, N2+, NO+, and CO+, can be swept up by the electric field of the impinging solar wind. Significant escape rate of CO2 ( 5 ´ 105 molecules cm-2 s –1 ) and N2 ( 2 ´ 105 molecules cm-2 s –1 ) may result.