Analytic models of electron impact excitation cross sections

Green, A.E.S.; Stolarski, R. S.

doi:10.1016/0021-9169(72)90030-x

Cited by 109 publications

(38 citation statements)

References 32 publications

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“…The cross sections of the b′ and 1 Π u were obtained from Zipf and McLaughlin []. The sum of the Rydberg states was derived by normalizing the values from Green and Stolarski [] to the total dissociation cross sections of Zipf and McLaughlin when they are added to the cross sections of the b′ and 1 Π u states.…”

Section: Methodsmentioning

confidence: 99%

An empirical approach to modeling ion production rates in Titan's ionosphere II: Ion production rates on the nightside

et al. 2015

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Ionization of neutrals by precipitating electrons and ions is the main source of Titan's nightside ionosphere. This paper has two goals: (1) characterization of the role of electron impact ionization on the nightside ionosphere for different magnetospheric conditions and (2) presentation of empirical ion production rates determined using densities measured by the Cassini Ion and Neutral Mass Spectrometer on the nightside. The ionosphere between 1000 and 1400 km is emphasized. We adopt electron fluxes measured by the Cassini Plasma Spectrometer-Electron Spectrometer and the Magnetospheric Imaging Instrument as classified by Rymer et al. (2009). The current paper follows an earlier paper (Paper I), in which we investigated sources of Titan's dayside ionosphere and demonstrated that the photoionization process is well understood. The current paper (Paper II) demonstrates that modeled and empirical ionization rates on the nightside are in agreement with an electron precipitation source above 1100 km. Ion production rate profiles appropriate for different Saturnian magnetospheric conditions, as outlined by Rymer et al., are constructed for various magnetic field topologies. Empirical production rate profiles are generated for deep nightside flybys of Titan. The results also suggest that at lower altitudes (below 1100 km) another source, such as ion precipitation, is probably needed.

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Section: Methodsmentioning

confidence: 99%

An empirical approach to modeling ion production rates in Titan's ionosphere II: Ion production rates on the nightside

et al. 2015

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“…All cross sections for CO (excitation and ionization) were approximated by semiempirical formulas [ Sawada et al , 1972b]. Cross sections for all processes of electron impact on O and N 2 were taken from Green and Stolarski [1972], Jackman et al [1977], and the recent compilation by Itikawa [2006].…”

Section: Model Input Parametersmentioning

confidence: 99%

Monte Carlo model of electron transport for the calculation of Mars dayglow emissions

Shematovich¹,

Bisikalo²,

Gérard³

et al. 2008

J. Geophys. Res.

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[1] A model of the photoelectron collision-induced component of the Mars dayglow using recent cross sections and solar flux is described. The calculation of the photoelectron source of excitation is based on a stochastic solution of the Boltzmann equation using the direct simulation Monte Carlo method. The neutral atmosphere is taken from outputs of a global circulation model, and recent inelastic collision cross sections are adopted. The calculated vertical profiles of the CO Cameron bands and CO 2 + doublet emissions integrated along the line of sight compare well with the Spectroscopy for the Investigation of the Characteristics of the Atmosphere of Mars (SPICAM) limb profiles observed with the SPICAM spectrograph on board Mars Express made at Ls = 166°during the summer season at northern midlatitudes. The comparison shows agreement to within the uncertainties of the excitation cross sections. Seasonal changes in the brightness and the altitude of the emission peaks are predicted with intensity variations in the range 15-20%.

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“…where the values 2.0 and 1.9 are determined based on the relative magnitude of the total cross sections, where the ionization and excitation cross section for 02 and N2 evaluated by GREEN and STOLARSKI (1972) are adopted. Assuming the phase functions of elastic collision for the three species are identical and using the newly defined atmospheric depth T, we can apply Eq.…”

Section: Validity O F the Discrete Ordinate Methodsmentioning

confidence: 99%

“…1. The total cross sections for excitation and ionization are taken from GREEN and STOLARSKI (1972). The phase function for the elastic and inelastic collisions is another important parameter for the degrading process of fast electrons.…”

Section: Formulationmentioning

confidence: 99%

Behaviour of low energy electrons precipitating in the upper atmosphere - an approach with the discrete ordinate method.

Takahashi

1975

J. geomagn. geoelec

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Analytic models of electron impact excitation cross sections

Abstract: Journal of Atmospheric and Terrestrial Physics 34 (1972) 1703-1717. doi:10.1016/0021-9169(72)90030-XReceived by publisher: 1972-04-25Harvest Date: 2016-01-04 12:19:59DOI: 10.1016/0021-9169(72)90030-XPage Range: 1703-171

Cited by 109 publications

References 32 publications

An empirical approach to modeling ion production rates in Titan's ionosphere II: Ion production rates on the nightside

An empirical approach to modeling ion production rates in Titan's ionosphere II: Ion production rates on the nightside

Monte Carlo model of electron transport for the calculation of Mars dayglow emissions

Behaviour of low energy electrons precipitating in the upper atmosphere - an approach with the discrete ordinate method.

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