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Information × Registration Number 0207U004738, 0103U000667 , R & D reports Title Research of Sun active phenomenons according to the data of Earth and space monitoring popup.stage_title Head Akimov Leonid Opanasovich, Registration Date 14-08-2007 Organization Kharkov national university named after V.N. Karazin popup.description2 The subject of study is the Sun. The research purpose is: - getting a new solar activity data; - study of solar X-ray flare activity feature and its periodicity during 23 cycle of solar activity as compared to cycles 21 and 22; - the investigation of solar bursts dynamics and morphology in the MgXII l 0.842 nm line; - study of the daily astroclimate during days of solar eclipses. The solar activity monitoring was carried out on the international network of Solar Survey programs and on the special programs also. Date on 64 solar flares and 59 eruptive events were obtained from 156 days of observations. Collected data were send to World Data Center-A (Boulder, Colorado, USA) and published in Solar Geophysical Data. Images of the Sun in Ha HI, K CaII, 1083 nm HeI spectral lines were presented via Internet on the "KHASSM" website. The conception of solar monitoring on the new automated spectroheliograph was worked up; the software for CCD camera was created. The new spectroheliograph was making in the Radio Electronics Institute Ukrainian Academy of Sciences with the help of UNTC grant. Daily X-ray solar flare indices XFI (energy) and Nx (number) were calculated for time interval from 1.01.75 to 31.12.05. The solar activity evolution was analyzed by X-ray flare indices at 21 - 23 solar cycles. The last cycle peculiarity was found out in comparison with previous ones. The statistically significant maxima of XFI and Nx indices power spectrum was found for differential rotation period and for periods, which connecting with inner planets rotations. Maximum peaks of amplitude are determined by rotation periods of Mercury and Venus we observed at the 21 and 23 cycles minimums. It was supposed that the changing electric charge of inner planets could affect the origin of flares. The dependence of solar soft X-ray flares number during the cycles 21 - 23 from orbital locations of Mercury, Venus and Earth are studied. Statistically significant asymmetry of the flares number distribution from planet heliographic longitudewas found. The proposed hypothesis about the electromagnetic mechanism of planet interaction with solar active region was discussed. Two differences between odd cycles (21, 23) and cycle 22 were found by behavior X-ray flare indexes XFI, Nx and relative Sunspot Numbers W: -there are a time lag (10-15 months) of the X-ray flare activity with respect to the sunspot activity in cycles 21, 23, which is not in cycle 22; -the statistically significant maximum for period ~ 150 -day is observed in the power spectra of XFI, Nx for solar cycles 21 and 23, but it is not detected for the cycle 22. The temporal variations of X-ray integral intensity of active regions and their fragments were analyzed from data obtained in Mg XII 0.842 nm line with spectroheliometer SPIRIT on board CORONAS-F satellite. The power spectra of X-ray emission showed statistically important features with periods of 12 - 30 min and 40 - 200 min. The power spectrum changed after new magnetic flux emergence in active region NOAA 9840. The statistically significant maximum in power spectrum AR 9825, 9830 9835 was found for 160 - min period. The peaks with periods near 5 min there are in power spectra of the fragments of active region only. Amplitude of these peaks was in maximum for power spectra temporal variations of intensity apex of arch loop one active region. There was AR NOAA 9825, in which many flares occurred. About 3800 slit ness spectra of solar chromosphere near D3 helium line were received on the diffraction spectrograph with CCD - camera during total solar eclipse of 2006 March 29 by expedition of NIIA KhNU. The resolution along height in solar chromosphere is about 20 km. The research of photometric behavior of CCD - camera was made. The variations of the mean-square trembling amplitude of solar limb were studied during of solar partial eclipses of 2003 May 31 and 2005 October 3. The lessening of the mean-square trembling amplitude was found even during small phase partial eclipse (0.24). The measurement of the mean-square trembling amplitude of solar limb were made on the Mountain Astronomical Station of MAO RAS by special expedition telescope during total solar eclipse of 2006 March 29. The lessening of the mean-square trembling amplitude from 0.85" (before eclipse beginning) to 0.65" (near second and third eclipse contacts) was found. The conclusion about significance of atmospheric convection by daily trembling of images was confirmed. Two MrS were made by these research topics. Two students participate in solar observations. Product Description popup.authors popup.nrat_date 2020-04-02 Close