Solar flux variability and the lifetimes of cometary H2O and OH

Details Solar flux variability and the lifetimes of cometary H2O and OH Solar flux variability and the lifetimes of cometary H2O and OH

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994icar..107..164b&link_type=abstract

Icarus, vol. 107, p. 164

Physics

68

Solar Flux Density, Comet Nuclei, Hydroxyl Radicals, Photodissociation, Far Ultraviolet Radiation, Extreme Ultraviolet Radiation, Solar Activity, Spatial Distribution, Solar Wind

Scientific paper

A solar EUV/FUV flux model based on recent SUSIM solar observations is presented. It is shown that both the fluxes and variabilities of the model are more consistent with SME and SUSIM solar spectrum measurements than those of the SERF1 model. It is calculated that photodissociation accounts for about 80 percent of the H2O destruction rate, while photoionization and solar wind particle interactions each account for about 10 percent of the H2O destruction. The calculated H2O and OH lifetimes against direct photodissociation both vary by 30 percent with solar activity. The major destruction channel for OH is predissociation, while direct photodissociation and solar wind interactions account for roughly 30 and 10 percent of the destruction rate, respectively.

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