Response of earth's atmosphere to increases in solar flux and implications for loss of water from Venus

Details Response of earth's atmosphere to increases in solar flux and implications for loss of water from Venus Response of earth's atmosphere to increases in solar flux and implications for loss of water from Venus

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984icar...57..335k&link_type=abstract

Icarus (ISSN 0019-1035), vol. 57, March 1984, p. 335-355.

Computer Science

61

Atmospheric Moisture, Earth Atmosphere, Solar Flux, Solar Planetary Interactions, Venus Atmosphere, Convection, Long Wave Radiation, Solar Radiation, Venus Clouds, Planets, Earth, Venus, Atmosphere, Water, Models, Temperature, Vapor, Solar Flux, Troposphere, Saturation, Clouds, Surface, Hydrogen, Oxygen, Absorption, Comparisons, Humidity, Climate, Altitude, Hyrodynamics, Escape, Enrichment, Chemistry, Element Ratios, Liquids, Radiation, Calculations, Convection, Data, Mixing

Scientific paper

A one-dimensional radiative-convective model is used to compute temperature and water vapor profiles as functions of solar flux for an earthlike atmosphere. The troposphere is assumed to be fully saturated, with a moist adiabatic lapse rate, and changes in cloudiness are neglected. Predicted surface temperatures increase monotonically from -1 to 111 C as the solar flux is increased from 0.81 to 1.45 times its present value. The results imply that the surface temperature of a primitive water-rich Venus should have been at least 80-100 C and may have been much higher. Water vapor should have been a major atmospheric constituent at all altitudes, leading to the rapid hydrodynamic escape of hydrogen. The oxygen left behind by this process was presumably consumed by reactions with reduced minerals in the crust.

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