Auroral response of WINDII green line emission rate to precipitated electrons measured by DMSP/SSJ4

Physics

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2407 Auroral Ionosphere (2704), 2455 Particle Precipitation, 2704 Auroral Phenomena (2407)

Scientific paper

The auroral response during day and night to magnetospheric precipitating electrons is investigated using a statistical approach. The vertical profiles of daytime auroral emission rate are obtained from UARS/WINDII measurements by removing airglow components from the total green line emission rates of O(^1S) at 557.7 nm using an empirical Chapman function model for dayglow as functions of solar zenith angle and F10.7 cm developed by Zhang and Shepherd (2005), providing auroral peak altitudes and integrated emission rates. Precipitated particle input is observed with DMSP-F10 and -F12 SSJ4 from which total energy and average energy are obtained. In order to investigate solar flux effect, two years of data are examined; 1993 (high solar flux) and 1996 (low solar flux). Total electron energy flux increases with increasing solar zenith angle (SZA) from 40° to 160° so that the energy flux at nighttime is much greater than in the daytime. During the daytime (SZA ≤ 90°) auroral atmospheric response has a good correlation with electron energy input with auroral production rates of 1.2 and 3.0 kR erg-1cm2s for years 1993 and 1996, respectively, but above SZA = 90° the auroral emission rate is significantly reduced in comparison with the total electron energy, except near solar zenith angles around 120°, where the two are consistant. Higher average energy electrons are precipitated in the lower solar flux year with mean average energy 1.37 and 2.77 keV for years 1993 and 1996 at 50°N geomagnetic latitude. A consistant decrease in average electron energy is seen with increasing latitude, along with a corresponding increase in auroral altitude, which is found to be inversely proportional to the average electron energy.

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