Detection of Rapidly Varying H2 Emissions in Jupiter's Aurora from the Galileo Orbiter

Pryor, W. R.; Stewart, A. I. F.; Simmons, K. E.; Ajello, J. M.; Tobiska, W. Kent; Clarke, J. T.; Gladstone, G. R.

doi:10.1006/icar.2001.6604

Cited by 12 publications

(9 citation statements)

References 15 publications

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“…As yet, however, there is no time-dependent model that makes this link explicitly. Such a model would be extremely useful; many studies have shown that there are auroral variations over time scales that range from minutes to months and years (e.g., Baron et al 1991, Livengood et al 1992, Pryor et al 2001, without being able to identify clearly the mechanisms producing them. The purpose of this paper is to take an important first step along the route to a fully coupled jovian magnetospheric and atmospheric model, by calculating the ionisation produced by various fluxes of energetic particles and the resultant conductivity.…”

Section: Introductionmentioning

confidence: 99%

On the Dynamics of the Jovian Ionosphere and Thermosphere III. The Modelling of Auroral Conductivity

Millward¹

2002

Icarus

103

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Section: Introductionmentioning

confidence: 99%

On the Dynamics of the Jovian Ionosphere and Thermosphere III. The Modelling of Auroral Conductivity

Millward¹

2002

Icarus

103

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“…Waite et al (2001) and Pryor et al (2001) have highlighted its amazing variability at UV wavelengths, on time scales of a few tens of seconds, and the incredibly high peak intensity of the emission (tens of kilorayleighs), inconsistent with models of cusp precipitation on Earth. Gladstone et al (2002) report evidence of emission of this spot in X-ray lines of highly ionized O and S ions.…”

Section: Renee Prangementioning

confidence: 99%

“…A number of FUV spectroscopic studies, aimed at characterizing the energy of the impinging magnetospheric particles via its penetration depth into the hydrocarbon absorbing layer have been conducted using HST and the FUV spectrographs onboard Galileo and Cassini Pryor et al 2001;Gustin et al 2002). Most of the time, they combine spectroscopy and imaging so that the particular auroral feature under study can now be identified.…”

Section: Renee Prangementioning

confidence: 99%

Commission 16: Physical Study of Planets and Satellites: (Etude Physique Des Planetes Et Des Satellites)

Cruikshank¹,

Courtin²,

Belton³

et al. 2002

Trans. Int. Astron. Union

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“…Gérard et al, 1995;Ballester et al, 1998;Clarke et al, 1998;Prangé et al, 1998;Trauger et al, 1998;Vincent et al, 2000;Pallier and Prangé, 2001;Pryor et al, 2001;Waite et al, 2001;Grodent et al, 2003), visible (Vasavada et al, 1999) and infrared (e.g. Satoh et al, 1996;Lam et al, 1997a;Satoh and Connerney, 1999;Trafton et al, 1999) radiation has shown that emission from neutral and ionised species is an important way of tracing the location of energy inputs into the upper atmospheres (Figures 1-2).…”

Section: Introductionmentioning

confidence: 96%

Giant Planet Ionospheres and Thermospheres: The Importance of Ion-Neutral Coupling

2005

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Planetary upper atmospheres -coexisting thermospheres and ionospheres -form an important boundary between the planet itself and interplanetary space. The solar wind and radiation from the Sun may react with the upper atmosphere directly, as in the case of Venus. If the planet has a magnetic field, however, such interactions are mediated by the magnetosphere, as in the case of the Earth. All of the Solar System's giant planets have magnetic fields of various strengths, and interactions with their space environments are thus mediated by their respective magnetospheres. This article concentrates on the consequences of magnetosphere-atmosphere interactions for the physical conditions of the thermosphere and ionosphere. In particular, we wish to highlight important new considerations concerning the energy balance in the upper atmosphere of Jupiter and Saturn, and the role that coupling between the ionosphere and thermosphere may play in establishing and regulating energy flows and temperatures there. This article also compares the auroral activity of Earth, Jupiter, Saturn and Uranus. The Earth's behaviour is controlled, externally, by the solar wind. But Jupiter's is determined by the co-rotation or otherwise of the equatorial plasmasheet, which is internal to the planet's magnetosphere. Despite being rapid rotators, like Jupiter, Saturn and Uranus appear to have auroral emissions that are mainly under solar (wind) control. For Jupiter and Saturn, it is shown that Joule heating and "frictional" effects, due to ion-neutral coupling can produce large amounts of energy that may account for their high exospheric temperatures.

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Detection of Rapidly Varying H2 Emissions in Jupiter's Aurora from the Galileo Orbiter

Cited by 12 publications

References 15 publications

On the Dynamics of the Jovian Ionosphere and Thermosphere III. The Modelling of Auroral Conductivity

On the Dynamics of the Jovian Ionosphere and Thermosphere III. The Modelling of Auroral Conductivity

Commission 16: Physical Study of Planets and Satellites: (Etude Physique Des Planetes Et Des Satellites)

Giant Planet Ionospheres and Thermospheres: The Importance of Ion-Neutral Coupling

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