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Titre du document / Document title

Galileo orbiter ultraviolet observations of Jupiter aurora

Auteur(s) / Author(s)

AJELLO J. (1) ; SHEMANSKY D. (2) ; PRYOR W. (3) ; TOBISKA K. (4) ; HORD C. (3) ; STEPHENS S. (4) ; STEWART I. (3) ; CLARKE J. (5) ; SIMMONS K. (3) ; MCCLINTOCK W. (3) ; BARTH C. (3) ; GEBBEN J. (3) ; MILLER D. (3) ; SANDEL B. (6) ;

Affiliation(s) du ou des auteurs / Author(s) Affiliation(s)

(1) Jet Propulsion Laboratory, Califomia Institute of Technology, Pasadena, ETATS-UNIS
(2) Department of Aerospace Engineering, University of Southern, California, Los Angeles, ETATS-UNIS
(3) Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, ETATS-UNIS
(4) Federal Data Corporation, Jet Propulsion Laboratory, Pasadena, California, ETATS-UNIS
(5) Space Physics Research Laboratory, University of Michigan, Ann Arbor, ETATS-UNIS
(6) Lunar and Planetary Laboratory, University of Arizona, Tucson, ETATS-UNIS

Résumé / Abstract

In 1996 during the first four orbits of the satellite tour the Galileo ultraviolet spectrometer (UVS) (11304320 A) and extreme ultraviolet spectrometer (EUVS) (540-1280 A) performed near-simultaneous observations of the Jupiter aurora in both the north and south polar regions. These observations are modeled to provide the absolute surface brightness of the aurora from the H2 Rydberg Systems (B, B', B, C, D, D' → X band systems). The spectral distribution and brightness of the EUV aurora are sensitive to H2 abundance, H2 temperature, and CH4 abundance. Analysis of the emission spectra indicates that the EUV aurora (800-1200 A) are produced over a range of altitudes corresponding to slant column abundances of H2 from 1016 to 1020 cm-2 or greater. The UVS spectra of the far ultraviolet (FUV) from 1130 to 1700 A are optically thin in H2, but highly sensitive to the CH4 column abundance and to the secondary electron energy distribution. The slant column abundance of CH4 absorbers found from models of the FUV spectra varied in the range 0 - 10 x 1016 cm-2, indicating the presence of both high altitude aurora, at or above the homopause, and deep aurora. The FUV spectra show C2H2 absorption bands near 1520 A. The surface brightness of the aurora from the H2 Rydberg Systems ranged from 100 to 600 kR and of H Lyman α was 60 to 130 kR for a 2000 km wide oval. The total power input to the atmosphere from particle deposition is estimated to be ∼ 1 X 1014 W.

Revue / Journal Title

Journal of geophysical research    ISSN  0148-0227 

Source / Source

Congrès
Conference on Magnetospheres of the Outer Planets, Boulder, Colorado , ETATS-UNIS (17/03/1997)
1998, vol. 103, no E9 (438 p.)  (1 p.1/4), pp. 20125-20148

Langue / Language

Anglais

Editeur / Publisher

American Geophysical Union, Washington, DC, ETATS-UNIS  (1949-2012) (Revue)

Mots-clés anglais / English Keywords

Data analysis

;

Modelling

;

Brightness distribution

;

Surface brightness

;

Hydrogen Molecules

;

Methane

;

Column density

;

Acetylene

;

Absorption band

;

Polar region

;

Jupiter planet

;

Planetary magnetospheres

;

Aurorae

;

Galileo space probes

;

Extreme ultraviolet spectra

;

Emission spectra

;

Mots-clés français / French Keywords

Analyse donnée

;

Modélisation

;

Distribution brillance

;

Brillance surface

;

Hydrogène Molécule

;

Méthane

;

Densité colonne

;

Acétylène

;

Bande absorption

;

Zone polaire

;

Planète Jupiter

;

Magnétosphère planétaire

;

Aurore

;

Sonde spatiale Galileo

;

Spectre UV extrême

;

Spectre émission

;

Mots-clés espagnols / Spanish Keywords

Distribución brillantez

;

Brillantez superficie

;

Densidad columna

;

Banda absorción

;

Zona polar

;

Localisation / Location

INIST-CNRS, Cote INIST : 3144, 35400007054605.0230

Nº notice refdoc (ud4) : 1582876



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