Properties of small-scale magnetic fields of coronal bright points in coronal holes

Some cases of occurrence and development of coronal bright points (CBPs) in an equatorial coronal hole (CH) are considered. The observations carried out with the telescope AIA instrument (Atmospheric Imaging Assembly) on the Solar Dynamics Observatory (SDO) board in the Fe XII, XXIV λ 193 Å line and HMI-magnetograms (Helio seismic and Magnetic Imager) in the λ 6173.3 Å spectral line were used. General conclusion for all the considered CBP born in CH is the evolution of the underlying small-scale bipolar magnetic structures. It is shown that small-scale magnetic fields of corresponding CBP have a larger area, which does not affect the size of CBP. In most cases, before emergence of the CBP in the solar corona, there is a jump of the magnetic field strength for the leading polarity. The disappearance of all CBPs is observed in the case of annihilation polarities. Such a result is obtained for photospheric and coronal layers of the solar atmosphere. (authors)