The young sun and the atmosphere and photochemistry of the early earth

Details The young sun and the atmosphere and photochemistry of the early earth The young sun and the atmosphere and photochemistry of the early earth

Sep 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983natur.305..281c&link_type=abstract

Nature (ISSN 0028-0836), vol. 305, Sept. 22, 1983, p. 281-286.

Mathematics

Logic

50

Atmospheric Chemistry, Atmospheric Composition, Earth Atmosphere, Photochemical Reactions, Planetary Evolution, Solar System, Formaldehyde, Oxygen, Ozone, Solar Corona, Stellar Evolution, Ultraviolet Spectra

Scientific paper

The origin and evolution of the earth's early atmosphere depend crucially on the dissipation time of the primitive solar nebula (SN). Using different theories of turbulence, the dissipation time of an SN of 0.1 solar mass is estimated as 2.5-8.3 Myr. Because accretion times are usually much longer, it is concluded that most planetary accretion must have occurred in a gas-free environment. Using new IUE data, a wavelength-dependent UV flux is constructed for the young sun which is then used to study the photochemistry and concentrations of O, O2, O3, OH, H, HCO and formaldehyde H2CO in the earth's early prebiological atmosphere.

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