Evolution of Coronal Bright Points in different regions of Solar Atmosphere

Sattarov Isroil, isattar@astrin.uz, Astronomical Institute AS of Uzbekistan
Karachik Nina, Tashkent state pedagogical university
Sherdanov Chori, Astronomical institute AS of Uzbekistan
Minenko Ekaterina, Astronomical Institute AS of Uzbekistan
Tillaboev Azlarkhon, Tashkent state pedagogical university

Abstract
Coronal bright points (CBP), point like bright features in solar corona, are observed over entire solar disc - in quiet and active regions, in coronal holes, etc., and present during all cycle – from solar minimum to solar maximum. As bright features in solar corona, CBP must be connected to solar magnetic fields. Previous studies of CBP and small scale magnetic fields (magnetic elements, ME) didn’t answer to the question on connection of CBP and ME. Moreover, a latitudinal distribution of CBP differs from the one of ME. It is known that the magnetic fields of quiet and active regions are different. We study evolution of CBP in different regions of solar corona: in quiet and active region, and coronal holes. In this report the evolution of CBP in different regions of solar corona is presented. The mechanism of flaring of CBP is discussed.