Jovian auroral spectroscopy with FUSE: analysis of self-absorption and implications for electron precipitation

• Published in: Icarus (New York, N.Y. 1962) Vol. 171; no. 2; pp. 336 - 355
• Main Authors: Gustin, J., Feldman, P.D., Gérard, J.-C., Grodent, D., Vidal-Madjar, A., Ben Jaffel, L., Desert, J.-M., Moos, H.W., Sahnow, D.J., Weaver, H.A., Wolven, B.C., Ajello, J.M., Waite, J.H., Roueff, E., Abgrall, H.
• Format: Journal Article Web Resource
• Language: English
• Published: San Diego, CA Elsevier Inc 01.10.2004; Elsevier; Academic Press Inc Elsevier Science
• Subjects: Astronomy; Astrophysics; Aurora; Earth sciences & physical geography; Earth, ocean, space; Exact sciences and technology; Jupiter; Physical, chemical, mathematical & earth Sciences; Physics; Physique, chimie, mathématiques & sciences de la terre; Sciences de la terre & géographie physique; Solar system; Spectroscopy; Ultraviolet observations; Aurora; Spectroscopy; Jupiter; Ultraviolet observations; Self-absorption; Methane; Ground states; Rydberg states; Spectral window; Electron distribution; High temperature; Jupiter planet; Spectral analysis; Characteristic function; Transition energy; One dimensional model; Solar system; Ultraviolet observation
• ISSN: 0019-1035; 1090-2643; 1090-2643
• DOI: 10.1016/j.icarus.2004.06.005

High-resolution ( ∼ 0.22   Å ) spectra of the north jovian aurora were obtained in the 905–1180 Å window with the Far Ultraviolet Spectroscopic Explorer (FUSE) on October 28, 2000. The FUSE instrument resolves the rotational structure of the H 2 spectra and the spectral range allows the study of self-absorption. Below 1100 Å, transitions connecting to the v ″ ⩽ 2 levels of the H 2 ground state are partially or totally absorbed by the overlying H 2 molecules. The FUSE spectra provide information on the overlying H 2 column and on the vibrational distribution of H 2. Transitions from high-energy H 2 Rydberg states and treatment of self-absorption are considered in our synthetic spectral generator. We show comparisons between synthetic and observed spectra in the 920–970, 1030–1080, and 1090–1180 Å spectral windows. In a first approach ( single-layer model ), the synthetic spectra are generated in a thin emitting layer and the emerging photons are absorbed by a layer located above the source. It is found that the parameters of the single-layer model best fitting the three spectral windows are 850, 800, and 800 K respectively for the H 2 gas temperature and 1.3 × 10 18 , 1.5 × 10 20 , and 1.3 × 10 20   cm − 2 for the H 2 self-absorbing vertical column respectively. Comparison between the H 2 column and a 1-D atmospheric model indicates that the short-wavelength FUV auroral emission originates from just above the homopause. This is confirmed by the high H 2 rovibrational temperatures, close to those deduced from spectral analyses of H + 3 auroral emission. In a second approach, the synthetic spectral generator is coupled with a vertically distributed energy degradation model, where the only input is the energy distribution of incoming electrons ( multi-layer model ). The model that best fits globally the three FUSE spectra is a sum of Maxwellian functions, with characteristic energies ranging from 1 to 100 keV, giving rise to an emission peak located at 5 μbar, that is ∼ 100   km below the methane homopause. This multi-layer model is also applied to a re-analysis of the Hopkins Ultraviolet Telescope (HUT) auroral spectrum and accounts for the H 2 self-absorption as well as the methane absorption. It is found that no additional discrete soft electron precipitation is necessary to fit either the FUSE or the HUT observations.