Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://uranus.sai.msu.ru/~ilusha/pubs/Livshits_n.pdf Äàòà èçìåíåíèÿ: Wed Jul 19 21:59:30 2006 Äàòà èíäåêñèðîâàíèÿ: Sat Apr 9 23:16:01 2016 Êîäèðîâêà: Windows-1251 Ïîèñêîâûå ñëîâà: ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ï ð ï ð ï ð ï ð ï ð ï ð ï ð ï ð ï ð ï

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. , ( ). . , . ÷horiz 1-2 . , -, , , .. . , , . , , , -, , . . , , . , , , .. - - . , , -. , . 1-2 . , , . 1.3 , . , , (. [12]), , , .

. , , , . ( , Ulyssys). , , , . , , , . . , - . , , . .. .. , .. -. ( 05-02-16090 04-02-16068).
1. S. V. Berdugina, D. Moss , D. D. Sokoloff, and I. G. Usoskin, Astron. and Astrophys. 445, 703 (2006). 2. J. T. Hoeksema and P. H. Scherrer, The Solar Magnetic Field - 1976 through 1985, WDCA Report UAG-94 (NGDC, Boulder, 1986). 3. J. T. Hoeksema, Solar magnetic fields - 1985 through 1990, Report CSSA-ASTRO-91-01 (1991). 4. V. N. Obridko and B. D. Shelting, Solar Phys. 1999, 184, 187. 5. . . , . . , . . 1999. 76, 942. 6. . . , . . 1999. 76, 385.
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7. . . , . . , . . , . . 1999. 76, 218. 8. P. Frick, S. L. Baliunas, D. Galyagin, et al., Astrophys. J. 483, 426. 9. .. , . . " "

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(-: , 2001) . 241. .. 10. , . . 40 (2006, ). 11. R. Howe, J. Christensen-Dalsgaard, F. Hill, et al., Science, 287, 2456 (2000). 12. . , . . , . , . . (2006, ).

VARIATION OF THE DIPOLE MAGNETIC MOMENT OF THE SUN DURING AN ACTIVITY CYCLE
I. M. Livshits, V. N. Obridko
Observations of large-scale solar magnetic fields (synoptic charts) and the Sun as a star (general magnetic field) have been used to determine the magnetic moment and direction of the dipole field for the last three solar cycles. Both the magnitude of the magnetic moment and its vertical and horizontal components proved to change regularly in the course of a solar cycle never vanishing completely. A wavelet analysis has shown that the amplitude of 27-day variations of the general magnetic field of the Sun (GMF) is closely related to the magnitude of the horizontal dipole. The sing reversal of of the global dipole consists in the change of the inclination angle of its axis. This process is not smooth but occurs in steps lasting for 1-2 years. Before the sing reversal, the dipole axis is precessing with respect to the solar rotation axis. Then, it moves in the meridional plane to reach very low latitudes, where it begins to shift significantly in longitude. These results are discussed in the context of helioseismic inferences of the existence of oscillations with a period of about 1.3 years and particularities of the dynamo processes in the case of inclined rotator.



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