| We have observed Jupiter in the ultraviolet band of wavelengths from 850-1850 A using the Hopkins Ultraviolet Telescope, the Hubble Space Telescope, and a sounding rocket experiment. These measurements comprise moderate-resolution equatorial and north polar spectra and images that probe the stratosphere of Jupiter. We have determined that the abundances of acetylene, ethane and ethylene were 39 {dollar}pm{dollar} 3 ppb, 3 {dollar}pm{dollar} 1 ppm and {dollar}<{dollar}0.4 ppb respectively in 1990, and 28 {dollar}pm{dollar} 3 ppb, 3 {dollar}pm{dollar} 1 ppm and 0.4 {dollar}pm{dollar} 0.2 ppb in 1995. The integrated (1450-1850 A) contribution of the H{dollar}sb2{dollar} dayglow was 800 {dollar}pm{dollar} 400 Rayleighs in 1990 and {dollar}<{dollar}400 Rayleighs in 1995, which was a period spanning solar maximum and solar minimum. The polar data have shown the molecular hydrogen aurora to extend over {dollar}4.5pm0.5times10sp{lcub}-10{rcub}{dollar} sr with an average brightness of 106 {dollar}pm{dollar} 12 kR integrated over the band of wavelengths from 900 to 1650 A, excluding Ly{dollar}alpha{dollar}. We measure a 13% larger emitting area ({dollar}5.1pm0.5times10sp{lcub}-10{rcub}{dollar} sr) and significantly different morphology for the combined atomic and molecular hydrogen aurora (Ly{dollar}rmalpha + Hsb2{dollar}), although these differences could be due to time variability. Color ratios derived from the data indicate a total auroral energy deposition rate of 13 ergs s{dollar}rmsp{lcub}-1{rcub} cmsp{lcub}-2{rcub}{dollar} by 3-30 keV electrons.; The sounding rocket development program has involved parallel studies of CCD detectors and ultraviolet spectrographs. These studies have included characterization of front and back-illuminated UV-sensitive CCDs with average quantum efficiencies of 18% and 40%, respectively, and the development of an aberrationless LiF prism spectrograph for imaging of UV astronomical targets. |
