Electron impact emission cross sections needed in modeling UV observations of the upper atmospheres of the planets

Joseph Ajello; Isik Kanik; Geoffrey K. James; Donald E. Shemansky

doi:10.1117/12.140844

22 January 1993 Electron impact emission cross sections needed in modeling UV observations of the upper atmospheres of the planets

Joseph Ajello, Isik Kanik, Geoffrey K. James, Donald E. Shemansky

Author Affiliations +

Proceedings Volume 1764, Ultraviolet Technology IV; (1993) https://doi.org/10.1117/12.140844
Event: San Diego '92, 1992, San Diego, CA, United States

Abstract

In recognition of the need for accurate collision cross-sections suitable for modeling spectroscopic observations of the planetary systems and calibrate flight instruments, NASA-JPL has determined the laboratory emission cross-sections of H, H2, N2, SO2, etc. Resonance excitation, predissociation, and non-Franck-Condon band intensity systems are determined by configuration interaction and must be taken into account in analyses of spacecraft observations. Attention is given to the application of the cross-sectional data obtained to both electron energy loss codes and models of Voyager, IUE, Galileo, and HST observations of the solar system.

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Joseph Ajello, Isik Kanik, Geoffrey K. James, and Donald E. Shemansky "Electron impact emission cross sections needed in modeling UV observations of the upper atmospheres of the planets", Proc. SPIE 1764, Ultraviolet Technology IV, (22 January 1993); https://doi.org/10.1117/12.140844

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