Modeling of global variations and ring shadowing in Saturn's ionosphere

Moore, Luke; Mendillo, M.; Müller‐Wodarg, I. C. F.; Murr, D.

doi:10.1016/j.icarus.2004.07.007

Cited by 83 publications

(179 citation statements)

References 46 publications

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“…While the overall magnitude of the density profiles is captured by ionospheric models (e.g. Moore et al 2004Moore et al , 2006Galand et al 2009), gravity waves need to be invoked to explain the highly-structure vertical profiles at Jupiter and Saturn (Barrow and Matcheva 2011;Matcheva and Barrow 2012;Barrow and Matcheva 2013). At low latitudes above the homopause, a surge in water inflow may also contribute to the presence of 'bite-outs' in the profiles observed at Saturn (Moore and Mendillo 2007).…”

Section: Ionospheric Response To Auroral Forcingmentioning

confidence: 99%

“…Kim and Fox 1991;Moses and Bass 2000). Ionospheric models have been developed for the outer planets, as reviewed by with more recent models proposed for Jupiter (Achilleos et al 1998;Perry et al 1999;Grodent et al 2001;Millward et al 2002;Tao et al 2010;Barrow and Matcheva 2011) and Saturn (Moses and Bass 2000;Moore et al 2004Moore et al , 2006Moore et al , 2008Moore et al , 2010Galand et al 2009Galand et al , 2011Barrow and Matcheva 2013).…”

Section: Ionospheric Modelsmentioning

confidence: 99%

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Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra

Branduardi‐Raymont

Galand

Hess

et al. 2015

The Magnetodiscs and Aurorae of Giant Planets

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Section: Ionospheric Response To Auroral Forcingmentioning

confidence: 99%

Section: Ionospheric Modelsmentioning

confidence: 99%

Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra

Branduardi‐Raymont

Galand

Hess

et al. 2015

The Magnetodiscs and Aurorae of Giant Planets

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“…It is then important to know in detail the rate constants of the collisions in which H 3 + participates. Models to estimate the concentration of the cation, as well as its vibrational structure and isotopic substituents, are used to follow the dynamics of the system as a function of solar fluence [7]. In addition, the rates of isotopic exchange processes are important in low-pressure plasmas of H 2 -D 2 mixtures [8].…”

Section: Hmentioning

confidence: 99%

Simulation of the infrared predissociation spectra of H5+

et al. 2012

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A quantum study of the bound states and infrared predissociation spectra of H 5 + is done using a recently proposed global and accurate potential-energy surface [Aguado et al., J. Chem. Phys. 133, 024306 (2010)]. The bound states are calculated for seven degrees of freedom using an iterative Lanczos method, yielding a dissociation energy in very good agreement with the available experimental data. The predissociation states are described by a wave-packet treatment considering a shared-proton model, in which the three-dimensional motion of the central atom is described using non-Jacobi bond coordinates. The justification of this model is that the change in the electric dipole moment is larger as a function of the motion of the central atom, responsible for the proton transfer in the H 3 + + H 2 → H 2 + H 3 + reaction. The electric dipole moment is calculated at the level of coupled-cluster theory with single and double excitations and fitted in nine dimensions to an analytical function. With it, the infrared predissociation spectrum is simulated, yielding a reasonable agreement with recent measurements.

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“…2 This figure shows the spectrum of emitted radiation, FðkÞ, the temperature-pressure profile in the atmosphere, (T gas , p gas ) and the degree of ionisation, f e , as a function of pressure for planet Earth, for Saturn and for two brown dwarfs. The Saturn thermodynamical data from Moses et al (2000), Moore et al (2004) (solid line) and Galand et al (2009) (dashed line) were used to derive the degree of ionisation [courtesy: Alejandro Luque]. Saturn's disk-integrated spectrum is based on the latest profiles of atmospheric temperature and gaseous composition derived from retrieval analysis of Cassini Composite Infrared Spectrometer spectra (Irwin et al 2008;Fletcher et al 2012;courtesy: Leigh Fletcher).…”

Section: Introductionmentioning

confidence: 99%

Atmospheric Electrification in Dusty, Reactive Gases in the Solar System and Beyond

et al. 2016

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Detailed observations of the solar system planets reveal a wide variety of local atmospheric conditions. Astronomical observations have revealed a variety of extrasolar planets none of which resembles any of the solar system planets in full. Instead, the most massive amongst the extrasolar planets, the gas giants, appear very similar to the class of (young) brown dwarfs which are amongst the oldest objects in the Universe. Despite this diversity, solar system planets, extrasolar planets and brown dwarfs have broadly similar global temperatures between 300 and 2500 K. In consequence, clouds of different chemical species form in their atmospheres. While the details of these clouds differ, the fundamental physical processes are the same. Further to this, all these objects were observed to produce radio and X-ray emissions. While both kinds of radiation are well studied on Earth and to a lesser extent on the solar system planets, the occurrence of emissions that potentially originate from accelerated electrons on brown dwarfs, extrasolar planets and protoplanetary disks is not well understood yet. This paper offers an interdisciplinary view on electrification processes and their feedback on their hosting environment in meteorology, volcanology, planetology and research on extrasolar planets and planet formation.

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Modeling of global variations and ring shadowing in Saturn's ionosphere

Cited by 83 publications

References 46 publications

Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra

Auroral Processes at the Giant Planets: Energy Deposition, Emission Mechanisms, Morphology and Spectra

Simulation of the infrared predissociation spectra of H5+

Atmospheric Electrification in Dusty, Reactive Gases in the Solar System and Beyond

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