The far ultraviolet (1200-1900 Å) spectrum of Jupiter obtained with a rocket-borne multichannel spectrometer

Giles, John W.; Moos, H. W.; McKinney, Wayne R.

doi:10.1029/ja081i034p05797

Cited by 30 publications

(7 citation statements)

References 43 publications

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“…Further observations, with inconclusive evidence for auroras on Jupiter, were undertaken by Rottman et al [1973], Clary and Hunter [1975], Giles et al [1976], and Holman and Hunter [1977]. Atreya et al [1977] presented evidence for the existence of auroral hot spots at the feet of the Io flux tube (IFT) using the Copernicus satellite spectrometer data.…”

Section: Jupitermentioning

confidence: 99%

Auroral emissions of the giant planets

Bhardwaj¹,

Gladstone²

2000

Reviews of Geophysics

153

128

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Abstract. Auroras are (generally) high-latitude atmospheric emissions that result from the precipitation of energetic charged particles from a planet's magnetosphere. Auroral emissions from the giant planets have been observed from ground-based observatories, Earthorbiting satellites (e.g., International Ultraviolet Explorer (IUE), Hubble Space Telescope (HST), and R6entgensatellit (ROSAT)), flyby spacecraft (e.g., Voyager 1 and 2), and orbiting spacecraft platforms (e.g., Galileo) at X-ray, ultraviolet (UV), visible, infrared (IR), and radio wavelengths. UV, visible, and IR auroras are atmospheric emissions, produced or initiated when ambient atmospheric species are excited through collisions with the precipitating particles, while radio and X-ray auroras are beam emissions, produced by the precipitating species themselves. The emissions at different wavelengths provide unique and complementary information, accessible to remote sensing, about the key physical processes operating in the atmospheric and magnetospheric regions where they originate. This paper reviews the development of our current understanding of auroral emissions from Jupiter, Saturn, Uranus, and Neptune, as revealed through multispectral observations and supplemented by plasma measurements.

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Section: Jupitermentioning

confidence: 99%

Auroral emissions of the giant planets

Bhardwaj¹,

Gladstone²

2000

Reviews of Geophysics

153

128

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“…Auroral activity near Jupiter's north pole has been observed in the FUV by means of rocket experiments, the Voyager ultraviolet spectrometer, and Earth-orbiting telescopes such as the International Ultraviolet Explorer (IUE) satellite [Broadfoot et al, 1981;Durrance et al, 1982;Giles et al, 1976;Rottman et al, 1973;Skinner, 1984;Skinner et al, 1984;Waite et al, 1988]. The IUE is particularly valuable, as its stable orbital position allows consecutive observations sequenced over several hours in order to resolve short time scale variability, while its extraordinary durability has permitted the construction of a data collection spanning more than a decade.…”

Section: Introductionmentioning

confidence: 99%

Long‐term study of longitudinal dependence in primary particle precipitation in the north Jovian aurora

Livengood¹,

Strobel²,

Moos³

1990

J. Geophys. Res.

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An analysis of wavelength‐dependent absorption in 229 FUV spectra (1150–1950 Å) of the Jovian north polar emissions obtained with the International Ultraviolet Explorer over the period 1978–1989 shows that the hydrocarbon optical depth in front of the auroral emission has a consistent dependence on the Jovian magnetic longitude. This variation is interpreted in two distinct ways: (1) the Jovian upper atmosphere is longitudinally homogeneous, and the variation in optical depth is due to a variation in penetration, and thus energy, of the primary particles; or (2) the energy of the primaries is longitudinally homogeneous, and it is aeronomic properties which change, most likely as a result of auroral heating. For case 1, the estimates of energy per particle for each of four particles which have been proposed as auroral primaries vary by a factor of ∼1.5–3.2 as a function of magnetic longitude, depending on the identity of the particles considered; the atmospheric model‐dependent energies are of the order of 14 keV for electrons, 0.4 MeV for protons, 0.4 MeV/nucleon for oxygen, and 0.3 MeV/nucleon for sulfur ions in a simple model polar atmosphere which we propose. Energy estimates for oxygen and sulfur ions fall well within limits established by Voyager measurements of the population of energetic O and S ions in the magnetosphere. For case 2, changes in atmospheric properties are modeled as a variation in the eddy diffusion coefficient K in the polar model, which covers the range from ∼3×106 to 2×107 cm² s−1, consistent with expected effects of localized auroral heating. Both interpretations imply a remarkable degree of stability in the coupling of the magnetosphere and atmosphere during the period of the observations, which covers a complete solar cycle and includes the Voyager encounters with Jupiter.

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“…The first indications of H^ Lyman band emission in the 'Jovian atmosphere were recorded in the sounding rocket spectra of Rottman et al [1973] and Giles et al [1976]. However, the first positive identification of Jovian auroral processes was provided by the Voyager ultraviolet spectrometers [Broadfoot e t al., 1979;Sandel et al, 1979] and the International Ultraviolet…”

Section: Introductionmentioning

confidence: 99%

The Jovian aurora: Electron or ion precipitation?

Waite¹,

Clarke²,

Cravens³

et al. 1988

J. Geophys. Res.

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High signal‐to‐noise spectra of the Jovian aurora at UV wavelengths obtained using the International Ultraviolet Explorer Observatory (including the brightest Jovian aurora observed to date) are used to study the existence of sulfur and oxygen emissions which would be associated with the precipitation of energetic heavy ions in the upper Jovian atmosphere. Model calculations of heavy ion precipitation and corresponding estimates of the associated sulfur and oxygen UV emissions carried out in the preceding companion paper of Horanyi et al. suggest emission values for 1304‐Å O I emission that are at least 50 times larger than the upper limit values set by the IUE observations reported here. On the other hand a possible emission feature of S II at 1256 Å is comparable to the theoretically predicted emission intensity. Earlier X ray observations and in situ plasma observations have indicated the existence of energetic heavy ion precipitation in the Jovian auroral zone. Based on the IUE observations reported here, we suggest a scenario where heavy ion auroral energy deposition is concentrated at altitudes below the homopause (i.e., >300 keV/nucleon) and electrons with energies of 10 to 30 keV are responsible for the bulk of the observable UV and EUV emissions since they deposit their energy above the methane‐absorbing layer defined by the homopause.

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The far ultraviolet (1200-1900 Å) spectrum of Jupiter obtained with a rocket-borne multichannel spectrometer

Cited by 30 publications

References 43 publications

Auroral emissions of the giant planets

Auroral emissions of the giant planets

Long‐term study of longitudinal dependence in primary particle precipitation in the north Jovian aurora

The Jovian aurora: Electron or ion precipitation?

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