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The aries auroral modelling campaign: characterization and modelling of an evening auroral arc observed from a rocket and a ground-based line of meridian scanners

Authors :
Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Science, University of Michigan, Ann Arbor, MI 48109, U.S.A.
Herzberg Institute of Astrophysics, National Research Council, Ottawa, Ontario, Canada K1A 0R6
Institute of Space and Atmospheric Sciences, University of Saskatchewan, Saskatoon, Saskatchewan, Canada S7N 0W0
Geophysical Institute, University of Alaska, Fairbanks, AK 99775-800, U.S.A.
D??partement de Physique, Universit?? de Montr??al, Montr??al, Qu??bec, Canada H3C 3JY
Jones, A. Vallance
Gattinger, R.L.
Creutzberg, F.
Harris, F.R.
McNamara, A.G.
Yau, A.W.
Llewellyn, E.J.
Lummerzheim, D.
Rees, M.H.
McDade, Ian C.
Margot, J.
Space Physics Research Laboratory, Department of Atmospheric, Oceanic and Space Science, University of Michigan, Ann Arbor, MI 48109, U.S.A.
Herzberg Institute of Astrophysics, National Research Council, Ottawa, Ontario, Canada K1A 0R6
Institute of Space and Atmospheric Sciences, University of Saskatchewan, Saskatoon, Saskatchewan, Canada S7N 0W0
Geophysical Institute, University of Alaska, Fairbanks, AK 99775-800, U.S.A.
D??partement de Physique, Universit?? de Montr??al, Montr??al, Qu??bec, Canada H3C 3JY
Jones, A. Vallance
Gattinger, R.L.
Creutzberg, F.
Harris, F.R.
McNamara, A.G.
Yau, A.W.
Llewellyn, E.J.
Lummerzheim, D.
Rees, M.H.
McDade, Ian C.
Margot, J.
Publication Year :
2006

Abstract

An auroral arc system excited by soft electrons was studied with a combination of in situ rocket measurements and optical tomographic techniques, using data from a photometer on a horizontal, spinning rocket and a line of three meridian scanning photometers. The ground-based scanner data at 4709, 5577, 8446 and 6300 A were successfully inverted to provide a set of volume emission rate distributions in the plane of the rocket trajectory, with a basic time resolution of 24 s. Volume emission rate profiles, derived from these distributions peaked at about 150 km for 5577 and 4709 A, while the 8446 A emission peaked at about 170 km with a more extended height distribution. The rocket photometer gave comparable volume emission rate distributions for the 3914 A emission as reported in a separate paper by McDade et al. (1991, Planet. Space Sci. 39, 895). Instruments on the rocket measured the primary electron flux during the flight and, in particular, the flux precipitating into the auroral arc overflown at apogee (McEwen et al., 1991; in preparation). The local electron density and temperature were measured by probes on the rocket (Margot and McNamara (1991; Can. J. Phys. 69, 950). The electron density measurements on the downleg were modelled using ion production rate data derived from the optical results. Model calculations of the emission height profile based on the measured electron flux agree with the observed profiles. The height distribution of the N2+ emission in the equatorward band, through which the rocket passed during the descent, was measured by both the rocket and the ground-based tomographic techniques and the results are in good agreement. Comparison of these profiles with model profiles indicates that the exciting primary spectrum may be represented by an accelerated Maxwellian or a Gaussian distribution centered at about 3 keV. This distribution is close to what would be obtained if the electron flux exciting the poleward form were accelerated by a 1-2

Details

Database :
OAIster
Notes :
En_US
Publication Type :
Electronic Resource
Accession number :
edsoai.ocn894059161
Document Type :
Electronic Resource