Thermospheric O I 844.6‐nm emission in twilight

Abstract

The thermospheric O I 844.6‐nm column emission rate was measured over Toronto, a midlatitude station, in the autumn of 1991 using an imaging Fabry‐Perot spectrometer. Twilight decay curves were measured on four clear evenings when the solar zenith angle was between 95° and 104°, giving corresponding column emission rates between 874 R and 130 R at 20° elevation angle in the azimuth of the Sun. The expected decay curves were calculated from the field line interhemisperic plasma model assuming only photoelectron impact excitation as the production mechanism with a cross section appropriate to an optically thin atmosphere. The agreement was good when the solar and geomagnetic activity levels were low to moderate, but the emission rate was overestimated during high activity periods. The comparison indicates that the photoelectron impact mechanism with a thin‐atmosphere cross section is sufficient to explain the twilight decay of the thermospheric O I 844.6‐nm emission.