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.

Global distribution o fauroral luminosity inferredfrom the auroral precipitation model The brightness of auroral emissions associated with the energy flux of 1 erg-cm 'V1 versus of precipitating electron energy is shown in Fig. 1. The isotropy pitch-angle and Maxwell energy flux distributions of electrons were assumed to calculate these relations. An albedo for isotropic incident flux was calculated according to results by Sergienko and Ivanov [1993]. Concentrations of N2, 0 2, 0 (3P) components and temperature profile at the altitudes from 90 to 200 km were taken from Morrill and Benesch [1996]. 391.4 nm 557.7 nm 669.0 nm LBH(L) F ig.2 These relations and characteristics of precipitating electrons inferred from АРМ are used to get the global patterns of auroral luminosity under different magnetic activity conditions. As an example, Fig. 2 demonstrates the global distribution of four auroral emissions for the low (top panel, AL= -200 nT, Dst= -5 nT) and disturbed (bottom panel, AL= -1000 nT, Dst= -100 nT) magnetic activity. 1200 MLT is at the top of each panel and 0600MLT on the right side. The vertical color scale indicates the luminosity brightness in kiloRelights (kR). Maxima intensity on the colour scales in Fig. 2 are 8, 12, 1.6, 1.6 kR from 391.4 nm to LBH, respectively. POLAR АРМ 12 F ig.3 The function / (equation 2), which represents the contribution of LBH bands in the interval 160-180 nm, is similar to the resultant LBH(L) filter utilized in POLAR spacecraft ultraviolet imager (UVI) [Torr et al, 1995\. The POLAR UV image obtained on Jan. 10, 1997 at 0300:38 UT and corresponding АРМ pattern constructed for the same magnetic activity level (AL= -224 nT; Dst=8 nT) are shown in Fig 3. The brightness of UV luminosity in units of POLAR imager (photon-cm^-s'1) is indicated by vertical black-white and color scales in the right-hand side of patterns. The maximum of brightness on these scales is 30 photon-cm'V1. The comparison of two patterns gives an evidence of similarity both in disposition and distribution of oval luminosity. However, the dayside diffuse luminosity equatorward of the oval is noticeable only in the АРМ pattern. It could be because of the low sensitivity of POLAR UVI. Torr et al. [1995] reported that only 250 R (~8 photon-cm'V1) are measured by UVI with a signal to noise ratio of 5. That is why the luminosity in the -0830-1230 MLT sector of the auroral oval is very poorly expressed. The same are observed in a number others events compared by us under low and moderate magnetic activity. 970110 050038 UT 109