Geomagnetic influences on thermospheric winds observed in the auroral zone

Abstract

A large body of observations of the wind field in the high-latitude thermosphere (140 to 350 km) is examined to characterize the winds and to determine their probably source. Theories and existing models of these winds are first reviewed. The morphologies of auroral particle precipitation, electric fields, and current systems are discussed to elucidate the effects of these factors upon the wind field. Existing models suggest that the effects of auroral electric fields and heating can be separated in a geomagnetic coordinate frame. It is shown, in this study, that the mean temporal dependence of the (geomagnetic) meridional component is similar to that predicted by tidal models except the magnitudes of the observed winds are smaller than predicted (observed peak speeds – 150 m sec⁻¹). Deviations (up to 200 m sec⁻¹) of the observed meridional winds from this mean behavior are probably caused by heating of the thermosphere by Joule dissipation in the auroral electrojets. Zonal winds are shown to be principally driven by collisions of the neutrals with ions drifting under the action of the auroral zone electric field. Zonal speeds from 200 to 400 m sec⁻¹ are typical. The observed zonal winds are correlated with the direction of the auroral electric fields as inferred from magnetometer records. The response time of the observed winds to changes in direction of the electric field (northward to southward) is found to be ≈ 1¹/₂ hours. Tidal winds are of secondary importance for the zonal component (peak speeds ≈ 150 m sec⁻¹). Electric fields and Joule dissipation in the high-latitude thermosphere are concluded to be responsible for the principal observed characteristics of auroral-zone thermospheric winds.