Physics of auroral phenomena : proceedings of the 35th Annual seminar, Apatity, 28 Februaru – 02 March, 2012 / [ed. board: A. G. Yahnin, A. A. Mochalov]. - Апатиты : Издательство Кольского научного центра РАН, 2012. - 187 с. : ил., табл.

0.1. Yagodkina, KG. Vorobjev the poleward boundary of the auroral oval as determined by an abrupt drop in the proton energy flux. The dayside proton boundaries coincide with the dayside electron boundaries. Here and hereinafter we conceded the average energy fluxes and the average energies rate over the AOP region which on the nightside includes area between b2i - b5i. The average energy and the number flux of protons between the precipitation boundaries in all magnetic local time sectors were calculated. The regression equations used for study of the behavior the proton precipitation for different level of magnetic activity. In Fig. 1 the average proton energy fluxes and the energies integrated over each MLTs in the DAZ and AOP regions are plotted as a function of the magnetic activity expressed by the AL - index. DAZ AOP 200 400 600 800 1000 1200 AL,nT 200 400 600 800 1000 1200 AL, nT Fig. 1 ........................... 09-12 ..................................... 12-15 ................ ..............15-18 06-09 1--1--'--1-----1-----1 600 800 1000 1200 AL, nT The energy fluxes and energies in the nightside MLTs (00-03, 03-06, 18-21, 21-24) are marked by the solid lines, in the dayside MLTs (06-09, 09-12, 12-15, 15-18) those are marked by the dashed lines. DAZ region: In the afternoon sectors (12-15, 15-18, 18-21 MLTs) the proton precipitating fluxes grow with increasing activity and have the maximum in the 15-18 MLT. In the prenoon sectors (06-09, 09-12 MLTs) the fluxes do not change with the increasing activity, and in the pre-midnight and post-midnight sectors (21-24, 00-03, 03-06 MLTs) the values of the fluxes vary weakly with increase of activity. The maximum energies have the same tendency in the afternoon MLTs but in the other sectors the average proton energies either decrease or do not vary according to the magnetic activity. AOP region: The maximum proton fluxes and energies occur in the nightside MLTs. The energies and the fluxes in the dayside sectors vary weakly. Proton Fluxes Proton Energies ♦ DAZ 12-15MLT 1200 800 - « AOP 12-15MLT 09-12MLT 200 400 600 800 1000 1200 AL, nT Fig.2 Fig. 2 demonstrates the ratio of the proton fluxes to the electron fluxes Fi/Fe ( a,b ) and the proton energy to the electron energies Ei/Ee (c,d) depending on the magnetic activity over eight MLTs. The inspection of the Fi/Fe shows that in the DAZ the intensity of proton precipitation gains with the increasing activity in the afternoon 12-15 and 15-18 MLTs. A significant portion of protons takes place in the 15-18 MLT. In this sector during quiet condition (AL-50-150 nT) the electron precipitating fluxes exceeds proton precipitation. However the proton precipitation exceeds the electron one ~ in 3.5 times when AL= - 1000 nT. In all other sectors the ratio of the fluxes 124