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.

A.S. Kirillov et al. where А669Л~ 5.93xl0 4 s~‘ is Einstein probability for the transition [ Gilmore et al., 1992]. The solving of corresponding equations allows us to calculate also vibrational populations N v o f singlet states. Applying Einstein probabilities for radiative transitions we can calculate intensities of LBH bands (transitions a ’n g,v -> X12g+,v'). Here we take into account 21 bands of LBH system in the interval 160-180 nm: v'=v+3, v+4, v+5 for v=0-3 and v-v+2, v+3, v+4 for v=4-6. The function/ of the contribution of every band is as follow: ДА) = expf-(A-170)2/23], (2) where Ais the wavelength (in nm), 170 nm is the centre of the interval. The emissions of first negative group (1NG) of molecular nitrogen ion are related with radiative transitions: N2+(B2E u +, v ) -> N2+(X2Eg+,v’) + hv 1NG • (3) To calculate the intensity of 391.4 nm band of 1NG (v=v'=0) we apply the equation: I 391.4 = Q ' -А з 91.4/Аш, (4) where Q’ is the production rate of the B 2 I U+ state of N2+by auroral primary and secondary electrons [Gordiets and * Konovalov , 1991; Sergienko and Ivanov, 1993], qv =0.883 is the Franck-Condon factor for the transition XILg+,v=0-»B 2 Eu+,v=0, ^ 391 . 4 = 1 .14x10 7 s ”1 is the spontaneous transition probability for the transition B 2 Su+,v=0-> X Eg ,v'=0, ^ tot= l-60x10 s ' is the total spontaneous transition probability for the transitions В Zu ,v=0-> X 2g , v’>0 (Gilmore et al., 1992). The emission of green line 557.7 nm of atomic oxygen is related with the radiative transition: ' 0 ( 1 S) -» O('D) + hv 557 7 . (5) The main production mechanisms of O('S) in auroral upper atmosphere are (Sharp et al., 1979): ( a ) the energy transfer from metastable molecular nitrogen, ( b ) the electronic excitation by auroral primary and secondary electron impact, ( с ) processes of dissociative recombination of thermal ionospheric electrons with 0 2+ ions. Therefore, to calculate the intensity /5577 of 557.7 nm line of atomic oxygen we apply the equation: Л 57.7 ( v ) N ? [0 ] + Q ls + 0 .0 6 a N e[O +2 ] ( 6 ) 4 57.7 +A2912+k'0i[02\+k'0[0] where ASinj = 1.215 s _1 and A 291.2 = 0.076 s~' [Bates, 1992] are the spontaneous transition probabilities for the transitions 'S->'D and ’S-> 3 P, respectively, k 0 , k 0 are the rate coefficients for the quenching of O('S) in collisions with 0 2 and 0 ( 3 P), respectively, k \v ) are the rate coefficients for the processes (a) for v=0-6, Q\s is the rate of the process (b) [Gordiets and Konovalov, 1991; Sergienko and Ivanov, 1993], a is the rate coefficient of dissociative recombination (c) of ionospheric electrons (with concentration Ne) and molecular oxygen ions 0 2+, 0.06 is the quantum yield of O('S) in the process ( с ) [Petrignani et al, 2005]. The coe fficien ts^ , k \ are taken C/2 t/ according to (Bates, 1992), the coefficients k'(v) are taken according to [Kirillov andAladjev, 1998]. l,kR 391.4 557.7 669.0 LBHL 10 20 30 E,keV Fig. 1 108