Proton aurora observed from the ground

Galand, M.; Chakrabarti, Supriya

doi:10.1016/j.jastp.2005.04.013

Cited by 27 publications

(16 citation statements)

References 71 publications

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“…While in the N 2 -dominated terrestrial atmosphere, such a signature is easily detectable (e.g. Galand and Chakrabarti 2006), it is not the case in an H 2 -dominated atmosphere. Suprathermal particles induce strong H emissions with photons undergoing frequency shift.…”

Section: Energetic Ionsmentioning

confidence: 99%

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

et al. 2014

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Section: Energetic Ionsmentioning

confidence: 99%

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

et al. 2014

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“…Galand (1996) showed that the energy losses associated with chargeexchange reactions and elastic collisions could be assumed to be continuous, which validated the entire approach. A wealth of different experimental and theoretical studies have been carried out lately (Jasperse, 1997;Lorentzen, 2000;Lummerzheim and Galand, 2001;Solomon, 2001;Chakrabarti et al, 2001;Basu et al, 2001;Fang et al, 2004;Hubert et al, 2004;Galand and Chakrabarti, 2006). None of the previous studies have solved simultaneously the electron and proton kinetic transports and the fluid equations.…”

Section: The Proton Transport Modellingmentioning

confidence: 99%

TRANS4: a new coupled electron/proton transport code – comparison to observations above Svalbard using ESR, DMSP and optical measurements

Simon¹,

Lilensten²,

Moen

et al. 2007

Ann. Geophys.

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Abstract. We present for the first time a numerical kinetic/fluid code for the ionosphere coupling proton and electron effects. It solves the fluid transport equations up to the eighth moment, and the kinetic equations for suprathermal particles. Its new feature is that for the latter, both electrons and protons are taken into account, while the preceding codes (TRANSCAR) only considered electrons. Thus it is now possible to compute in a single run the electron and ion densities due to proton precipitation. This code is successfully applied to a multi-instrumental data set recorded on 22 January 2004. We make use of measurements from the following set of instruments: the Defence Meteorological Satellite Program (DMSP) F-13 measures the precipitating particle fluxes, the EISCAT Svalbard Radar (ESR) measures the ionospheric parameters, the thermospheric oxygen lines are measured by an all-sky camera and the H α line is given by an Ebert-Fastie spectrometer located at Ny-Ålesund. We show that the code computes the H α spectral line profile with an excellent agreement with observations, providing some complementary information on the physical state of the atmosphere. We also show the relative effects of protons and electrons as to the electron densities. Computed electron densities are finally compared to the direct ESR measurements.

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“…It also allows the identification of the types of precipitating particles-an equal mixture of oxygen and sulfur ions-and an estimation of their energies, which is consistent with a magnetospheric origin and acceleration processes up to a few MeV/amu. Despite the new cross sections made available the past years, there is still a true need for additional measurements or modelling due to lack of data or dataset with too restricted energy coverage, too large uncertainness or too low spectral resolution (e.g., Lindsay and Stebbings 2005;Galand and Chakrabarti 2006;Karwasz et al 2006). Finally, the applicability of measurements obtained under laboratory conditions to space environment should be borne in mind (Lindsay and Stebbings 2005).…”

Section: Auroramentioning

confidence: 99%