A comparison between N₂⁺4278-Å emission and electron flux in the auroral zone

Abstract

This study utilizes data from the (AE-D) satellite. It is noted that a number of visual airglow experiment (VAE) and the low similar studies have been previously undertaken energy electron experiment (LEE) on board the [cf. Gustafsson, 1970; Deehr et al., 1970, 1973; Atmosphere Explorer D satellite. The 4278-% N• Gustafsson et al., 1972; Gustafsson and Egeland, surfade brightness profile is measured as a func-1976]. In no case, however, have the authors tion of angle along the satellite track by using a method which corrects for reflection from the ground below. This intensity is compared with the incident electron energy flux between 0.2 and 25 keV and plotted as a function of mean and tota•l electron energy. The observed ratio of I4278/F E is 256+ 125 R/erg cm -2 s -1, which is slightly higher than the value of ~210 R/erg cm -2 s -1 predicted theoretically by Rees and Luckey [1974]. Excess 4278-A emission on the southern edge of the aurora is shown to be a result of high-energy (>10 keV) proton precipitation. A general increase in the scatter of the data toward low mean electron energies is a possible indication of the presence of parallel electric fields below the altitude of the satellite (150-800 km). erg cm -2 s -1 for energies of <10 keV. The purpose of this study is to measure this ratio in the nighttime auroral zone by using observations from the Atmosphere Explorer D 1Now at Particle and auroral observations from the Esro I/Aurorae satellite, J. Atmos. Terr. Phys., 35, 1979, 1973. Ioo Edgar, B. C., W. T. Miles, and A. E. S. Green, Energy deposition of protons in molecular nitrogen and applications to proton auroral phenomena, J. Geophys. Res., 78, 6596, 1973. Gustafsson, G. A., Auroral luminosity patterns over northern Scandinavia during a number of Esro 1A (Aurorae) passages, Phy s . Norv., 4, 113, 1970.

A case study of the aurora, high‐latitude ionosphere, and particle precipitation during near‐steady state conditions

“…(Reasonable in this context is meant to imply as good as any current equivalent determination [i.e., Kasting and Hays, 1977].) (Reasonable in this context is meant to imply as good as any current equivalent determination [i.e., Kasting and Hays, 1977].)…”

“…Kasting and Hays [1977] noted similar discrepancies when they utilized the Rees and Luckey predictions. Some of this difference may be due to uncorrected background radiation.…”

Particle precipitations during NEIAL events: simultaneous ground based observations at Svalbard

“…Previous statistical and modelling studies have given a conversion factor from the 427.8 nm intensity to the total electron energy flux, varying between 210-270 R/(mW m −2 ) (Deehr and Egeland, 1972;Rees et al,1976;Kasting and Hays, 1977;Strickland et al, 1989). In this study we have used a conversion factor of 233 R/(mW m −2 ) .…”

Auroral energy deposition rate, characteristic electron energy, and ionospheric parameters derived from Dynamics Explorer 1 images

“…The electron impact cross section as a function of entergy is a well-established parameter for the 3914A band emission, and the energy flux of the electron precipitation may be inferred directly from the measured column emission rate [Rees and Luckey, 1974;Kasting and Hays, 1977;Rees and Robie, 1986] 4hi ( In spite of the uncertainties associated with the 5577A and the 6300• auroral radiations the "red to blue ratio" I(6300)/I(3914) and the "red to green ratio" I(6300)/I(5577) have been and are still being used to infer characteristic energies of precipitating auroral electron fluxes. The electron impact cross section as a function of entergy is a well-established parameter for the 3914A band emission, and the energy flux of the electron precipitation may be inferred directly from the measured column emission rate [Rees and Luckey, 1974;Kasting and Hays, 1977;Rees and Robie, 1986] 4hi ( In spite of the uncertainties associated with the 5577A and the 6300• auroral radiations the "red to blue ratio" I(6300)/I(3914) and the "red to green ratio" I(6300)/I(5577) have been and are still being used to infer characteristic energies of precipitating auroral electron fluxes.…”