UV Spectroscopy by Electron Impact for Planetary Astronomy and Astrophysics



The objectives of UV emission spectroscopy by electron impact carried out over the past 20 years at the Jet Propulsion Laboratory (JPL) have been: 1) to measure electron impact emission cross sections (0-2keV) and fluorescence spectra (50-1200nm) for important atoms and molecules of planetary atmospheres, stellar atmospheres and the interstellar medium (ISM) for modeling remote sensing observations of EUVE, FUSE, HST, HUT, Galileo, Cassini and many other spacecraft, 2) to emphasize UV transitions of species of Jovian planetary systems, Herbig-Haro objects and comets: H, H2, N2, SO2, O, CO and O2, and 3) to develop collision strengths in analytical form for UV radiative processes for electron energy loss transport codes. A specialized review is given of our twenty year laboratory program to provide accurate UV emission cross sections for these species. The five sets of high spectral resolution apparatus that have been developed at JPL for this experimental program provided results to the astronomy community from the extreme ultraviolet beginning at 50 nm to the visible at 600 nm.


Line Profile Boron Carbide Hubble Space Telescope Emission Cross Section Dissociative Excitation 
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Copyright information

© Springer Science+Business Media New York 2002

Authors and Affiliations

  1. 1.Jet Propulsion LaboratoryCalifornia Institute of TechnologyUSA

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