Other
Scientific paper
May 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...186.3303l&link_type=abstract
American Astronomical Society, 186th AAS Meeting, #33.03; Bulletin of the American Astronomical Society, Vol. 27, p.857
Other
1
Scientific paper
The ultraviolet spectra of the molecules H2 and HD by solar fluorescence and photoelectron excitation are calculated and compared with the Jovian equatorial dayglow spectrum obtained by the Hopkins Ultraviolet Telescope at 3 Angstroms resolution near the maximicrons of solar cycle 22. The Jovian dayglow is accounted for in both the brightness and the spectral shape by solar fluorescence and photoelectron excitation, and no additional energy source is required. It is characterized by an H2 rotational-vibrational temperature of 540 K and an H2 column density of 7 times 10(19) cm(-2) . The dayglow spectrum is in agreement with the presence of cascade contribution to the Lyman band emission from the high-lying E,F(1) Sigma_ {g}(+) states. The incorrectly perceived absence of appreciable cascade effects from comparison of the dayglow spectrum with the room-temperature laboratory spectrum of H2 is caused by the fact that the spectrum of H2 is sensitive to the temperature and the Jovian atmosphere is hotter. The observed weakness of the dayglow emission at short wavelengths is mainly caused by self-absorption by H2. The dayglow spectrum suggests minimal absorption by hydrocarbon on Jupiter. Wavelength coincidences of solar emission lines and absorption lines of H2 and HD occur, resulting in strong fluorescence of H2 and HD. The strong coincidence of the solar Lyman-beta line at 1025.72 Angstroms and the P(1) line of the (6,0) Lyman band of H2 at 1025.93 Angstroms together with other line coincidences produce unique line spectra which are identified in the dayglow spectrum. The fluorescence due to absorption of the solar O VI line at 1031.91 Angstroms by the vibrationally excited H2 via the Q(3) line of the (1,1) Werner band at 1031.86 Angstroms is a sensitive measure of the atmospheric temperature. Despite strong coincidence of the solar O VI line at 1031.91 Angstroms and the R(0) line of the (6,0) Lyman band of HD at 1031.91 Angstroms, the molecule HD remains to be detected due to the weakness of the HD signature and the dominance of the H2 emission.
Dalgarno Alexander
Liu Wende
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