HR: 1340h
AN: SH14A-1699    [Abstracts]
TI: High-latitudinal Activity in Solar Cycle 23
AU: * Benevolenskaya, E E
AF: Elena Benevolenskaya, W.W. Hansen Experimental Physics Laboratory, 491 South Service Road, Stanford, CA 94305, United States
AB: Cycle 23 is going to be finished. What is the new we know about the nature of the solar cyclicity on the base of the modern observations in space and on the ground? How deep is our knowledge about the high-(mid)- latitudinal activity on the Sun? And, it is the next question. Is our undestanding of the solar activity enough to predict the next cycle and the behavior of the solar activity in the future. All these questions come from the past and are still an important. The Solar and Heliospheric Observatory provides us an important data of coronal and magnetic activity since 1996 (the beginning of the cycle 23). Due to these data we can look at the EUV corona on the solar disk and compare it with the magnetic energy release, directly. We can observe the changing of the magnetic pattern during the solar cycle from small-scale magnetic elements ('knots', or facular) to large-scale (prominances, sunspots) both at the photosphere and the corona. The results of investigations of the current cycle made by different authors show the complicated picture of the solar cycle while the main features like Hale's and Joe's laws, 'butterfly' distibutions, polar magnetic field reversals are kept. Here, I represent the results of the investigation of the high-latitudinal activity and its relation to the mid-latitude of the photoshere and the corona for the current cycle 23 using the SOHO/MDI, SOHO/EIT and WSO solar data. The observational dynamic behavior of the solar magnetic features is discussed with the relation to the dynamo theories.
DE: 2162 Solar cycle variations (7536)
DE: 7509 Corona
DE: 7524 Magnetic fields
DE: 7549 Ultraviolet emissions
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting