[3] Some authors consider the active regions to be the source of high-speed solar wind streams. Mustel [1980] supposed that active regions are the sources of quasi-stationary corpuscular streams. Active regions on the solar disk are preceded in certain cases by coronal holes with a relatively undisturbed area between them. This explains the origin of the idea of the so-called "cone of avoidance" [Mustel, 1980]. According to Kuklin and Plyusnina [1979] the sources of high-speed solar wind streams are located in the vicinity of the complexes of activity.
[4] According to the current data of optical and radio observations the solar corona has a fine structure at all observed scales. All the structural features of the corona and their changes within the solar cycle are manifested in variations in solar wind parameters. Analyzing the observations in the radio range made by the National Radio Astronomy Observatory's Very Large Array, Woo [1996] showed that fine structure followed down to the photosphere is observed in the regions of location of coronal holes. Since the coronal hole regions are sources of high-speed geoefficient solar wind streams, to explain the mechanism of formation and acceleration of the solar wind, one needs an exact picture of the processes occurring in all layers of the solar atmosphere. The SOHO data [Insley et al., 1995] show that there are active processes at the boundaries of the chromospheric net in the zones of coronal holes location. McKenzie et al. [1995] were the first to assume that high-speed streams of the solar wind are generated directly in the chromospheric network in the vicinity of the basis of coronal holes and that possibly high-frequency waves are generated in the process of a small-scale reconnection. Bocchialini and Vial [1996] detected differences in the structure of the high-chromosphere and low-transition-region network between the regions of equatorial coronal hole location and quiet regions.
[5] The main goal of this work is to compare coronal holes in X ray and He I line. Compare their mutual location, photospheric magnetic fields peculiarities in arias corresponding to the coronal holes locations, and corresponding solar wind response and try to understand why similar X-ray coronal holes produce different solar wind evolution.
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