Physics of auroral phenomena : proceedings of the 33rd Annual seminar, Apatity, 02 - 05 March, 2010 / [ed.: A.G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2011. - 206 с. : ил.

Long-term variations o f energetic electrons at low altitudes All the satellites carried onboard the same MEPED instruments that monitor the intensities of charged particle radiation at higher energies extending up to cosmic rays. Two identical electron telescopes are included in the instrument. One, termed the 0° electron detector, is mounted on the 3-axis stabilized NOAA spacecraft to view outward along the Earth-center-to-satellite vector. Whenever the satellite is poleward of a geographic latitude of about 35°, this detector monitors electrons in the atmospheric loss cone that will enter the Earth's atmosphere below the satellite. At lower geographic latitudes, this detector measures electrons that are geomagnetically trapped. The second electron telescope, called the 90° detector, is mounted to view in a direction approximately perpendicular to the 0° detector. At higher geographic latitude locations along the satellite orbit the 90° detector monitors electrons that are geomagnetically trapped since they will be reflected by the geomagnetic field at some point below the spacecraft The pair of electron telescopes provide 3 integral channels of electron data: Ee > 30 keV, Ee > 100 keV, and Ee > 300 keV. The proton mix in the channels out of the SAA is insignificant. excluded from the data set. On the figure 1 the comparison of detectors inter-calibration is shown. To compare the data of each channel were averaged by month, at L < 1.2 with SAA region excluded from the data set. The data from different satellites are in good agreement, indicating that the quality of inter-calibration of instruments on different satellites is high enough. The discrepancy shown is explained by the difference in heights of vehicles (up to 50 km), as well as the fact that satellites N15, N17, M02 work in the morning local time, and satellites N16, N18, N19 - in the evening. 1DOO »ooo 1 00 10 /* Лs I oo A A 'X F -.M '~‘ о о a I О 4 NortHemhemisphere A ■ о > op , 0 Southern hemisphere ^ SAA <*> £ <> с со 04 06X999 О! 0>062002 0*0*50; 3 02 0* 5004 03.06 2001 02 06 200* 01 06 2008 01 0« 2009 160 юо яо as 2 0 VSO *эоо •500 «ООО о*061»»* о; 0->.06.25>02 озобгогэ 0*0<J24>04 ©i0tt,200t —i- _i----- L_----- _ 02 06 2007 01062006 01062000 № — .—.’Л , ---------------------------- од ot> ivv« о) об.гооо О» 06 2.00? 05 О* 200 ? 2004 02062005 >2О* *007 01 0»>2006 01 06 200V v \ / V y .А Л л А ^ * Kp, month average 0 4 M „ „ 0* 0 * 2 0 0 0 03 06 2 0 0 1 О » 0 6 2 0 0 3 OS 04 7001 0 2 0 6 2 0 0 4 0 2 0 6 2 0 0 S 0 2 06 2 0 0 6 0 2 0 6 2 0 0 7 0 1 0 6 2 0 0 * 0 1 0 6 2 0 Fig. 2. The comparison of the electron flux and the magnetosphere parameters. Dst and Kp shows magnetospheric events. The CR average rate is shown on the bottom graph. 145