Abstract
Based on observation data with a high spatial resolution, the multifractal properties of turbulent magnetized plasma in a nonperturbed solar atmosphere are revealed. It is shown that magnetic fluxes in elements of the magnetic field, as well as the size of elements, are distributed lognormally, which is indicative of multifractality. In coronal holes (CHs), the multifractality of magnetic fields is observed on scales of 10000-400 km; at the same time, it is observed on smaller scales as the resolution improves, and its degree increases. It is shown that two subsets of granules exist: the usual granules, with a characteristic size of 1000–1300 km and Gaussian size distribution, and mini-granules, which do not have a well-pronounced characteristic size and are mostly less than 600 km in diameter. The size distribution function of the mini-granules obeys lognormal law and their multifractal character is seen on small scales down to 50 km, which allows one to make a conclusion about the presence of multifractality of photospheric plasma flows in CHs and in a nonperturbed photosphere. A conclusion is made that multifractality takes place for small-scale magnetic fields of quiet regions, as well as for large-scale fields of active regions. This makes it possible to suppose that solar magnetic fields are generated by a common nonlinear dynamical process.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
