Thermospheric vertical winds in the auroral oval/polar cap region

Abstract. Thermospheric mean vertical winds from high-resolution Fabry-Perot Spectrometer observations of the λ630 nm emission (from ∼240 km altitude), over a four year interval 1997–2000, from Mawson (67.6 ◦ S, 62.9 ◦ E, Inv 70.5 ◦ S) and Davis (68.6 ◦ S, 78.0 ◦ E, Inv 74.6 ◦ S) are presented. Combining the four years of data shows Maw-son mean hourly vertical winds vary between −10 m s−1 and +4 m s−1, while Davis mean hourly vertical winds vary between −10 m s−1 and +10 m s−1. Mean hourly vertical winds from Mawson show little change with Kp, while at Davis the range of variation increases with increasing ge-omagnetic activity. Histograms of frequency distributions of such winds, and their variations with Kp and λ630 nm emission intensity, are presented and discussed. Variations in mean hourly thermospheric winds and λ630 nm emission in-tensities show at least three significant associations between mean vertical winds and the auroral oval. Mean vertical winds within the auroral oval are smaller than those outside the oval, particularly those in the polar cap. A downward wind associated with entry of the observing region into the auroral oval can be seen in both Mawson and Davis hourly mean vertical winds. Large vertical winds are seen poleward of the auroral oval/polar cap boundary, most significantly up-ward winds occur within ±2 hr of magnetic midnight. Un-der moderately quiet geomagnetic conditions Davis passes through the auroral oval into the polar cap in the evening, but at higher Kp it passes into the polar cap earlier and larger, and more sustained mean vertical winds are observed. Key words. Meteorology and atmospheric dynamics (ther-mospheric dynamics)