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.

I. V. Mingalev et al. with time were calculated until they become stationary. The steady-state distributions of the atmospheric parameters were obtained on condition that inputs to the model and boundary conditions correspond to 10.30 UT. The temperature distributions, corresponding to this moment, were taken from the NRLMSISE-00 empirical model [Picone et al., 2002]. It turns out that atmospheric temperatures, calculated with the I300 help of the NRLMSISE-00 empirical model for two distinct values of solar activity (F 10.7 =101 30 and 230), are very similar below ® approximately 100 km, while, | о above this altitude, they may be -1 rather different. From Fig. 1, one ‘30 can see that, at the altitude of 110 km, differences between [~— r '""I. ----------- ~~~\ ^*200 temperatures, obtained for two -90 considered 10.7-cm solar fluxes, can achieve a few tens of degrees at identical points of the globe. Thus, the application of the NRLMSISE-00 empirical model shows that the influence of level of solar activity on the global distribution of the atmospheric temperature ought to be absent at altitudes of the troposphere, stratosphere, and mesosphere, while this influence ought to be appreciable at altitudes of the lower thermosphere for the winter period in the northern hemisphere. -180 -150 -120 -90 -60 -30 0 30 60 90 120 150 180 Longitude F ig .l. The global distributions of the atmospheric temperature (K) at 110 km altitude, obtained from the NRLMSISE-00 empirical model for 16 January, UT=10.30 and calculated for two distinct values of solar activity: F 10.7 =101 (top panel) and Fюл-230 (bottom panel). Fig.2. The global distributions of the vector of the simulated horizontal component of the neutral wind velocity at the altitude . Ш 30 of 50 km, obtained for 16 January and calculated for two distinct 4 “ ШШШШЩМйи, Щ 15 values of solar activity: F 10.7 =101 (top panel) and F10.7=230 (bottom panel). The velocities are given in m/s. Distributions of the atmospheric parameters, calculated with the help of the mathematical model and obtained for 16 January, are partly shown in Figs. 2-4. The results of modeling illustrate both common characteristic features and distinctions caused by different values of solar activity. The calculated global distributions of the atmospheric parameters display the following Longitude 134