Densities and vibrational distribution of H<sub>3</sub><sup>+</sup> in the Jovian auroral ionosphere

Kim, Y. H.; Fox, Jane L.; Porter, H. S.

doi:10.1029/92je00454

Cited by 67 publications

(59 citation statements)

References 63 publications

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“…The overall distribution of vibrational populations shown in Fig. 8 is similar to that of the model presented by Kim et al (1992), which includes only vibrational states. A small difference is visible, because Kim et al (1992) included V-V energy transfer from H 2 (v > 0) to H + 3 .…”

Section: Resultssupporting

confidence: 61%

“…8 is similar to that of the model presented by Kim et al (1992), which includes only vibrational states. A small difference is visible, because Kim et al (1992) included V-V energy transfer from H 2 (v > 0) to H + 3 . In the models presented here, we ignore interactions of H + 3 rovibrational levels with other constituents such as H atoms, and vibration energy transfer reactions with H 2 (v≥ 1).…”

Section: Resultssupporting

confidence: 51%

“…A model for the relative populations of the vibrational levels showed significant depopulations of v 2 = 1 and 2 by fast radiative relaxation (Kim et al 1992). Stallard et al (2002) developed a simple three level model to account for the observed intensity ratios of lines in the fundamental band to those in the hot band.…”

Section: Introductionmentioning

confidence: 99%

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NON-LTE EFFECTS ON THE H₃⁺ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

Kim¹

2012

Journal of The Korean Astronomical Society

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We investigate non-LTE effects on the H + 3 level populations to help the analysis of the observed 2 and 3.5 micron H + 3 emissions from the Jovian ionosphere. We begin by constructing a simple threelevel model, in order to compute the intensity ratio of the R(3,4) line in the hot band to the Q(1,0) line in the fundamental band, which have been observed in the Jovian auroral regions. We find that non-LTE effects produce only small changes in the intensity ratios for ambient H 2 densities less than or equal to 5×10 11 cm −3 . We then construct two comprehensive models by including all the collisional and radiative transitions between pairs of more than a thousand known H + 3 rovibrational levels with energies less than 10000 cm −1 . By employing these models, we find that the intensity ratios of the lines in the hot and fundamental bands are affected greatly by non-LTE effects, but the details depend sensitively on the number of collisional and radiative transitions included in the models. Non-LTE effects on the rovibrational population become evident at about the same ambient H 2 densities in the comprehensive models as in the three-level model. However, the models show that rotational temperatures derived from the intensities of rotational lines in the ν 2 and 2ν 2 bands may differ significantly from the ambient temperatures in the non-LTE regime. We find that significant non-LTE effects appear near and above the H + 3 peak, and that the kinetic temperatures in the Jovian thermospheric temperatures derived from the observed line ratios in the 2 and 3.5 micron H + 3 emissions are highly model dependent.

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Section: Resultssupporting

confidence: 61%

Section: Resultssupporting

confidence: 51%

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NON-LTE EFFECTS ON THE H₃⁺ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

Kim¹

2012

Journal of The Korean Astronomical Society

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“…-An alternative method is to utilise transport models based on the explicit, direct solution of the Boltzmann equation, which can use a two-stream approach (up/down) (Waite 1981;Waite et al 1983;Achilleos et al 1998;Grodent et al 2001;) or multi-stream approach (more than two pitch angles considered) (Kim et al 1992;Perry et al 1999;Menager et al 2010;Galand et al 2011). The Boltzmann equation expresses the conservation of the number of particles in the phase space, as given by:…”

Section: Energetic Electronsmentioning

confidence: 99%

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

et al. 2014

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“…Previous attempts to model the Jovian dayside ionosphere have failed to reproduce the electron densities and altitude distributions measured by Galileo and Voyager ( Hinson et al 1997( Hinson et al , 1998McConnell et al 1982). Modeled peak electron densities are at least an order of magnitude greater in density and higher in altitude than the measured results Kim et al 1992;Perry et al 1999). Discrepancies result from the lack of self-consistent, rotational-level H 2 ionospheric chemistry models.…”

Section: Introductionmentioning

confidence: 65%

A Rotational‐Level Hydrogen Physical Chemistry Model for General Astrophysical Application

Hallett

Shemansky

Liu

2005

ApJ

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A physical chemistry model has been developed to predict the non-LTE state of hydrogen-dominated astrophysical objects under electron and photon forcing. The model is composed of five constituents, H 2 , H, H þ 3 , H þ 2 , and H + , and is unique in the application of physical chemistry at the rotational level. The range of behavior is explored for electron and solar deposition. Application of solar forcing includes a prediction of the steady state photoelectron energy distribution, calculated from the interaction of solar photons and photoelectrons with the fine structure. The model is applied to a wide range of physical conditions, including those appropriate to the outer-planet upper atmospheres, from the exobase to the hydrocarbon homopause. Steady state partitioning is found to vary by multiple orders of magnitude in response to variation of neutral diffusion, ambient electron density, and gas kinetic temperature. The model is particularly sensitive to neutral diffusion. The non-LTE H 2 X 1 AE þ g (v : J ) partitioning exhibited for the range of explored physical conditions and forcing is critical to the prediction of the states of the outer-planet ionospheres. The determination of rotational-level H 2 partitioning allows the prediction of discrete and continuum emission features running the entire spectral range for comparison to observations of astrophysical phenomena, including outer-planet aurora and dayglow, comet coma environments, and stellar atmospheres.

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Densities and vibrational distribution of H₃⁺ in the Jovian auroral ionosphere

Cited by 67 publications

References 63 publications

NON-LTE EFFECTS ON THE H₃⁺ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

NON-LTE EFFECTS ON THE H₃⁺ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

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

A Rotational‐Level Hydrogen Physical Chemistry Model for General Astrophysical Application

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Densities and vibrational distribution of H3+ in the Jovian auroral ionosphere

Cited by 67 publications

References 63 publications

NON-LTE EFFECTS ON THE H3+ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

NON-LTE EFFECTS ON THE H3+ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

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

A Rotational‐Level Hydrogen Physical Chemistry Model for General Astrophysical Application

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Product

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Densities and vibrational distribution of H₃⁺ in the Jovian auroral ionosphere

NON-LTE EFFECTS ON THE H₃⁺ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE

NON-LTE EFFECTS ON THE H₃⁺ROVIBRATIONAL POPULATION IN THE JOVIAN IONOSPHERE