The research on the response characteristic of nighttime 135.6 nm airglow emission intensity to Dst index based on the data of the Ionosphere PhotoMeter(IPM)on FY-3D Satellite
The Ionosphere PhotoMeter(IPM)is a far ultraviolet nadir-view photometer that flew aboard the second-generation,polar-orbiting Chinese meteorological satellite Feng-Yun 3D(FY-3D),which was launched on November 2th,2017.By observing far ultraviolet night-time OI 135.6 nm emissions,which are produced by the recombination of O+ions and electrons,The F2 layer peak electron density can be deduced.During daytime IPM was designed to measure the OI 135.6 nm and N2 Lyman-Birge-Hopfield(LBH)band emissions,which would be used to infer the O/N2 ration.Based on the night side dada of IPM,this paper studies the relative changes of nighttime 135.6 nm airglow emission intensity both mid and low latitudes during magnetic storms and quiet periods.Studies have shown that the nighttime 135.6 nm airglow emission is highly susceptible to disturbances due to magnetic storms.Even for very weak magnetic storms,the nighttime 135.6 nm airglow emission intensity will increase,and the time when the intensity increases corresponds well to the main phase and recovery phase of the magnetic storm.Through comparison with the TEC data provided by IGS(International GNSS Service),it is believed that the enhancement of 135.6 nm emission intensity during the magnetic storm is not caused by changes in the ionosphere.Studies of multiple magnetic storms with different intensities have shown that the increase in 135.6 nm intensity is inversely proportional to the Dst index,which means that the lower the Dst index,the greater the increase in 135.6 nm intensity during magnetic storms compared to magnetic calm,and the higher the latitude,the greater the increase in 135.6 nm emission intensity.
Dst index135.6 nm emission intensityPeak electron densityTEC
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