Loss of water from Venus. I - Hydrodynamic escape of hydrogen

Details Loss of water from Venus. I - Hydrodynamic escape of hydrogen Loss of water from Venus. I - Hydrodynamic escape of hydrogen

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983icar...53..479k&link_type=abstract

Icarus (ISSN 0019-1035), vol. 53, March 1983, p. 479-508.

Astronomy and Astrophysics

Astronomy

93

Astronomical Models, Atmospheric Moisture, Hydrodynamic Equations, Hydrogen, Photochemical Reactions, Venus Atmosphere, Deuterium, Escape Velocity, Planetary Temperature, Planetology, Radiant Heating, Solar Radiation, Ultraviolet Radiation, Water Vapor, Venus, Water, Hydrodynamics, Escape, Hydrogen, Photochemistry, Models, Atmosphere, Flux, Calculations, Mixing, Concentration, Solar Radiation, Ultraviolet, Wavelengths, Heating, Deuterium

Scientific paper

A one-dimensional photochemical-dynamic model is used to study hydrodynamic loss of hydrogen from a primitive, water-rich atmosphere on Venus. The escape flux is calculated as a function of the H2O mixing ratio at the atmospheric cold trap. The cold trap mixing ratio is then related in an approximate fashion to the H2O concentration in the lower atmosphere. Hydrodynamic escape should have been the dominant loss process for hydroogen when the H2O mass mixing ratio in the lower atmosphere exceeded approximately 0.1. The escape rate would have depended upon the magnitude of the solar ultraviolet flux and the atmospheric EUV heating efficiency and, to a lesser extent, on the O2 content of the atmosphere. The time required for Venus to have lost the bulk of a terrestrial ocean of water is on the order of a billion years. Deuterium would have been swept away along with hydrogen if the escape rate was high enough, but some D/H enrichment should have occurred as the escape rate slowed down.

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