Coronal hole spatial-temporal evolution is studied and comparison made with that of the solar global magnetic field in cycles 21 -23 (1976 -2012). The latitude-longitude distribution dynamics of coronal holes and the regularities in the global magnetic field associated with the solar polar field reversal are analyzed. Polar and non-polar coronal hole populations are considered. The investigation reveals some temporal and spatial regularities in coronal hole distributions that match well the global magnetic-field cycle evolution. The results show that the non-polar coronal hole longitudinal distribution follows all configuration changes in the global magnetic-field structure. Reorganizations of the global magnetic-field and coronal hole distributions occur simultaneously during a time interval of a few solar rotations. The cycle evolution of the non-polar coronal holes reflects the transition of the solar global magnetic field from the zonal structure to sectorial and vice versa. Two different type waves of nonpolar coronal holes are revealed from their latitudinal distribution. The first one is short poleward waves. They trace the poleward motion of the unipolar photospheric magnetic fields from approximately 35 • to the associated pole in each hemisphere and the redevelopment of a new-polarity polar CH. Although they start the poleward movement before the change of the polar magnetic field in the associated hemisphere, they reach the pole after the polar reversal. The other type of non-polar CH wave forms two sinusoidal branches associated with the positive-and negative-polarity magnetic fields. The complete period of the wave was equal to ≈268 CRs (22 years). These wave CHs arrive at high latitudes during declining phases when the new polarity polar CHs are already completely formed.

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An estimate of the dimension of the attractor of the dynamic system responsible for solar activity is obtained from the time series of carbon 14 experimental data (4300 BC to 1950 AD). According to this estimate the attractor is a fractal, in shape close to a 3-torus. The attractor's trajectories characterizing the evolution of the magnetic field exhibit irregular long-term behaviour.

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Abstract. The properties of the magnetic field in the coronal holes (CH) were considered during 1996-2002. The daily observations from the Kitt Peak observatory in the line HeI 10830Å were compiled. The measurement of the magnetic fields in the CH was carried out by comparing the data obtained from the Kitt Peak telescope and the magnetograms of SOHO/MDI. The dependence between the brightness of CH from intensity of the magnetic field and distributions of CH depending from the magnetic field and latitude were presented for minimum and maximum of the cycle. The latitude and the unipolarity degree of the magnetic field that influence on the brightness of the CH were examined. It was shown that the average magnetic field was 1-2G, the unipolarity degree of the magnetic field was 0.1-0.3 and brightness of the coronal holes increases with the average magnetic field. The latitude-time distributions of CH for different polarity were obtained.The coronal holes (CH) are an important factor characterizing the solar activity. It is known that CH are the source of the high-speed solar wind, which effectively influences on the magnetosphere of Earth. Today the observations in the line Hel 10830A are remained the most effective type of the optic observations for identifying CH (Harvey & Recely (2002)). The regular daily observations in this line have been taking place on the Kitt Peak observatory since 1974. The relatively low amplitude of the cycle 23 allows us to examine the formation of CH at the backdrop of the smaller sunspot activity. The daily observations of the magnetic fields on SOHO/MDI with the small noise level permit to determine the intensity and structure of the magnetic fields in the coronal holes.The formal automatic procedure was developed for the purpose of identifying the borders of the coronal holes by using the daily Kitt Peak observations in the line HeI 10830Å during 1996-2003. The coronal holes in HeI line are represented in intensity by the bright regions. It was found that the limited intensity is between 5-10 relative units. This allowed to define the magnetic properties of CH using the comparative analysis with magnitograms. The total number of the bright regions with the area more than 3x10 9 km 2 was 17000. The number of the bright structures with the area more than 3x10 10 km 2 that can be associated with the CH was 3300. The latitude-time dependence of the coronal holes with the area more than 3x10 10 km 2 show us two types of the coronal regions: the high latitudes and pre-equator. The distribution of bright elements with the smaller area in the line HeI 10830Å was discussed in paper Tlatov & Tavastsherna (2002). The large and small structures are identical as a whole, what proves the uniform nature of the formation mechanism of the helium regions. The distribution of the coronal holes in solar cycle activity shows, that CH exit outside the sunspot zone, where the large-scale magnetic fields with the only one predominant polarity exist. Probably the main role in the formation of CH has the s...