Investigation of the evolution of coronal bright points and magnetic field topology

Our investigation has been carried using the instruments onboard the Solar Dynamics Observatory (SDO) providing a high resolution of images (AIA photographs and HMI magnetograms). We have investigated the structure and magnetic evolution of several coronal bright points and small scale N-S polarity magnetic fluxes closely associated with them. We also compare the evolution of the magnetic polarities of elementary isolated sources of positive and negative fluxes (magnetic bipoles) and coronal bright points. Tiny (“elementary”) coronal bright points have been detected. A standard coronal bright point is shown to be a group of “elementary” coronal bright points that flare up sequentially. Our investigation shows that a change in the magnetic fluxes of opposite polarities is observed before the flare of a coronal bright point. We show that not all cases of the formation of coronal bright points are described by the magnetic reconnection model. This result has not been considered previously and has not been pointed out by other authors.     

Latitudinal-Temporal Analysis of Long-Periodic Variations of Coronal Bright Points

Geomagnetism and Aeronomy - The latitudinal-temporal changes in wavelet spectra for the number of coronal bright points (CBPs) in solar-activity (SA) cycles 23 and 24 are analyzed with the Morlet...     

Calculation of the Main Parameters of a Magnetic Flux Tube within the Model of Cylindrically Symmetric Equilibria of Two-Component Plasma

Geomagnetism and Aeronomy - The paper presents an analytical model of a magnetic tube, which is described as a cylindrically symmetric equilibrium state of two-component plasma. The plasma flow is...     

What SDO tells us about structure and evolution of coronal bright points

Using magnetograms and coronal images from two instruments on board the Solar Dynamics Observatory (SDO), we study structure and evolution of a limited number of coronal bright points (CBPs). Our results show that the relation between CBPs and their magnetic footpoints is not simple. In some cases, CBP may appear as a bright portion of a larger loop (with clearly identifiable footpoints), and in some cases, an isolated CBP may develop between magnetic poles, which might not be the closest ones to each other or which might not be involved in the magnetic flux cancellation. We suggest that the magnetic connectivity responsible for formation of isolated coronal bright points is governed by the orientation of the large‐scale magnetic field. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Physicochemical and Energy Impact on the Process of Leaching of a Eudialyte Concentrate

Doklady Earth Sciences - The results of an experimental study of alkaline decomposition of eudialyte concentrate when exposed to physicochemical and energy impacts prior to the subsequent acid...