New electron energy transfer and cooling rates by excitation of O2

Павлов, А. В.

doi:10.1007/s00585-998-1007-8

Cited by 28 publications

(27 citation statements)

References 27 publications

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“…Electron cooling by electron impact excitation of carbon dioxide was identified [ Morrison and Greene , 1978] as an important energy transfer process in the Martian atmosphere, and probably important for Venus. Morrison and Greene [1978] calculated electron energy loss rates, elsewhere named electron energy transfer rates [ Pavlov , 1998], these being the rates of energy loss per unit electron and molecule density. These loss rates were calculated as a function of electron temperature and have been used as a parameter in modeling of the ionosphere of Venus [ Strangeway , 1996].…”

Section: Introductionmentioning

confidence: 99%

Carbon dioxide electron cooling rates in the atmospheres of Mars and Venus

Campbell¹,

Brunger²,

Rescigno³

2008

J. Geophys. Res.

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[1] The cooling of electrons in collisions with carbon dioxide in the atmospheres of Venus and Mars is investigated. Calculations are performed with both previously accepted electron energy transfer rates and with new ones determined using more recent theoretical and experimental cross sections for electron impact on CO 2 . Emulation of a previous model for Venus confirms the validity of the current model and shows that use of the updated cross sections leads to cooling rates that are lower by one third. Application of the same model to the atmosphere of Mars gives more than double the previous cooling rates at altitudes where the electron temperature is very low.

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Section: Introductionmentioning

confidence: 99%

Carbon dioxide electron cooling rates in the atmospheres of Mars and Venus

Campbell¹,

Brunger²,

Rescigno³

2008

J. Geophys. Res.

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“…Presently for most of these terms, we use the classical expressions, which are based on rather old estimations (Schunk & Nagy, ). Some of these terms have been updated (e.g., Smithtro & Solomon, , for heating rate and Pavlov, , ; Pavlov & Berrington, , for inelastic cooling), but we have not yet included all of them in the model; this could explain at least some of the differences.…”

Section: Discussionmentioning

confidence: 99%

IPIM Modeling of the Ionospheric F₂ Layer Depletion at High Latitudes During a High‐Speed Stream Event

et al. 2018

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Our aim is to understand the effect of high‐speed stream events on the high‐latitude ionosphere and more specifically the decrease of the foF2 frequency during the entire day following the impact. First, we have selected one summertime event, for which a large data set was available: Super Dual Auroral Radar Network (SuperDARN) and European Incoherent SCATter (EISCAT) radars, Tromsø and Sodankylä ionosondes, and the CHAllenging Minisatellite Payload (CHAMP) satellite. We modeled with the IPIM model (IRAP Plasmasphere Ionosphere Model) the dynamics of the ionosphere at Tromsø and Sodankylä using inputs derived from the data. The simulations nicely match the measurements made by the EISCAT radar and the ionosondes, and we showed that the decrease of foF2 is associated with a transition from F2 to F1 layer resulting from a decrease of neutral atomic oxygen concentration. Modeling showed that electrodynamics can explain short‐term behavior on the scale of a few hours, but long‐term behavior on the scale of a few days results from the perturbation induced in the atmosphere. Enhancement of convection is responsible for a sharp increase of the ion temperature by Joule heating, leading through chemistry to an immediate reduction of the F2 layer. Then, ion drag on neutrals is responsible for a rapid heating and expansion of the thermosphere. This expansion affects atomic oxygen through nonthermal upward flow, which results in a decrease of its concentration and amplifies the decrease of [O]/[N2] ratio. This thermospheric change explains long‐term extinction of the F2 layer.

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“…These are from Stubbe and Varnum [2], Newton et al [3] and Pavlov [1,7]. These are from Stubbe and Varnum [2], Newton et al [3] and Pavlov [1,7].…”

Section: Calculation Of Electron Energy Transfer Ratesmentioning

confidence: 97%

“…Pavolv [1,7] gives a formula for an electron energy transfer rate Q 0ν (per molecule) for the transition 0 → ν:…”

Section: Calculation Of Electron Energy Transfer Ratesmentioning

confidence: 99%

Understanding the Role of Electron-driven Processes in Atmospheric Behaviour

Brunger¹

2004

AIP Conference Proceedings

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Electron-impact excitation plays a major role in emission from aurora and a less significant but nonetheless crucial role in the dayglow and nightglow. For some molecules, such as N 2 , O 2 and NO, electron-impact excitation can be followed by radiative cascade through many different sets of energy levels, producing emission with a large number of lines. We review the application of our statistical equilibrium program to predict this rich spectrum of radiation, and we compare results we have obtained against available independent measurements. In addition, we also review the calculation of energy transfer rates from electrons to N 2 , O 2 and NO in the thermosphere. Energy transfer from electrons to neutral gases and ions is one of the dominant electron cooling processes in the ionosphere, and the role of vibrationally excited N 2 and O 2 in this is particularly significant. The importance of the energy dependence and magnitude of the electron-impact vibrational cross sections in the calculation of these rates is assessed.

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New electron energy transfer and cooling rates by excitation of O2

Cited by 28 publications

References 27 publications

Carbon dioxide electron cooling rates in the atmospheres of Mars and Venus

Carbon dioxide electron cooling rates in the atmospheres of Mars and Venus

IPIM Modeling of the Ionospheric F₂ Layer Depletion at High Latitudes During a High‐Speed Stream Event

Understanding the Role of Electron-driven Processes in Atmospheric Behaviour

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New electron energy transfer and cooling rates by excitation of O2

Cited by 28 publications

References 27 publications

Carbon dioxide electron cooling rates in the atmospheres of Mars and Venus

Carbon dioxide electron cooling rates in the atmospheres of Mars and Venus

IPIM Modeling of the Ionospheric F2 Layer Depletion at High Latitudes During a High‐Speed Stream Event

Understanding the Role of Electron-driven Processes in Atmospheric Behaviour

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Product

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IPIM Modeling of the Ionospheric F₂ Layer Depletion at High Latitudes During a High‐Speed Stream Event