Spatial relationship between CMEs and prominence eruptions during SC 24 and SC 25

During their propagation, coronal mass ejections (CMEs) and prominences sometimes display a nonradial motion. During the years after the solar minimum, the CME central position angle tended to be offset closer to the equator compared to that of the associated prominence eruptions (PE). No such effect was observed during solar maximum. The purpose of this paper is to investigate the latitudinal offsets of CMEs with respect to their source regions. We study 256 events from SC 24 and SC 25, listed in the Coordinate Data Analysis Workshop Data Center. We analyzed the CMES radial offset from the associated PEs by comparing their latitudes in the plane of the sky. This work is an extension of the previous work by Gopalswamy et al., but with an independent data set. We have confirmed the systematic equatorward offset of CME from the solar source region for the rising phase of Solar Cycle 25. Our analysis of the relation between CME linear speed and PE-CME latitudinal offset indicated that the velocities of the deflected CMEs are mainly in the range of 200 and 800 km s$^{−1}$. In this study, we compared the nonradial offsets for the rising and decay phases of SC 24 and our analysis has shown that during the decay phase more events deflected toward the pole can be observed. The observed variation is attributed to the presence of a substantial number of low-latitude coronal holes during the decay phase and to the influence from nearby active regions

Eruptions from coronal hole bright points : observations and non-potential modeling

Funding: DHM would like to thank the Science and Technology Facilities Council (UK) through the consolidated grant ST/N000609/1 and the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 647214).Context. We report on the third part of a series of studies on eruptions associated with small-scale loop complexes named coronal bright points (CBPs). Aims. A single case study of a CBP in an equatorial coronal hole with an exceptionally large size is investigated to extend our understanding of the formation of mini-filaments (MFs), their destabilisation and the origin of the eruption triggering the formation of jet-like features recorded in the extreme-ultraviolet (EUV) and X-ray emission. We aim to explore the nature of the so called micro-flares in CBPs associated with jets in coronal holes and mini coronal mass ejections in the quiet Sun. Methods. Co-observations from the Atmospheric Imaging Assembly (AIA) and Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO), and GONG Halpha images are used together with a Non-Linear Force Free Field (NLFFF) relaxation approach, where the latter is based on a time series of HMI line-of-sight magnetograms. Results. A mini-filament (MF) that formed beneath the CBP arcade around 3–4 h before the eruption is seen in the Halpha and EUV AIA images to lift up and erupt triggering the formation of an X-ray jet. No significant photospheric magnetic flux concentration displacement (convergence) is observed and neither is magnetic flux cancellation between the two main magnetic polarities forming the CBP in the time period leading to the MF liftoff. The CBP micro-flare is associated with three flare kernels that formed shortly after the MF liftoff. No observational signature is found for reconnection beneath the erupting MF. The applied NLFFF modeling successfully reproduces both the CBP loop complex as well as the magnetic flux rope that hosts the MF. Conclusions. The applied NLFFF modellng is able to clearly show that an initial potential field can be evolved into a non-potential magnetic field configuration that contains free magnetic energy in the region that observationally hosts the eruption. The comparison of the magnetic field structure shows that the magnetic NLFFF model contains many of the features that can explain the dfferent observational signatures found in the evolution and eruption of the CBP. In future it may eventually indicate the location of destabilisation that results in the eruptions of flux ropes.Publisher PDFPeer reviewe

Анализа на глобалните трговски текови за временскиот период 2008-2018 година

Предмет на анализа во овој труд е учеството на поважните групи на производи во структурата на глобалната трговија за временскиот период 2008-2018 година. Резултатите од анализата на глобално ниво укажуваат на намалување на вредноста на извозот на горива и производи од рударство за временскиот период 2008-2018 година, додека зголемување на вредноста на извозот на земјоделски производи и индустриски добра. Анализирано по групи на земји, како најзначаен извозник на поважните групи на производи се јавува Европската унија. Клучни зборови: глобална трговија, земјоделски производи, индустриски добра, ЕУ

АНАЛИЗА НА ГЛОБАЛНИТЕ ТРГОВСКИ ТЕКОВИ ЗА ВРЕМЕНСКИОТ ПЕРИОД 2008-2018 ГОДИНА

Предмет на анализа во овој труд е учеството на поважните групи на производи во структурата на глобалната трговија за временскиот период 2008-2018 година. Резултатите од анализата на глобално ниво укажуваат на намалување на вредноста на извозот на горива и производи од рударство за временскиот период 2008-2018 година, додека зголемување на вредноста на извозот на земјоделски производи и индустриски добра. Анализирано по групи на земји, како најзначаен извозник на поважните групи на производи се јавува Европската унија. &nbsp

A Statistical Analysis of Deflection of Coronal Mass Ejections in the Field of View of LASCO Coronagraphs

Coronal mass ejections (CMEs) can generate the most severe geomagnetic disturbances. One of the most critical factors affecting a CME’s geoeffectiveness is its trajectory. It is crucial to determine whether and when CME will hit Earth. It is commonly assumed that CMEs experience a deflection of propagation in the corona and in interplanetary space. In this study, we analyze more than 14,000 CMEs listed in the Coordinate Data Analysis Workshop (CDAW) catalog during 1996–2022 to estimate their deflection in the Large and Spectrometric Coronagraph field of view (LFOV). In our statistical analysis, the deflection was determined using the CME height–time measurements listed in the CDAW catalog. We have shown that, in the solar corona, CME deflection is a common phenomenon, heavily influenced by solar activity cycles as well as phases of these cycles. We have demonstrated that during periods of solar activity minima the deflection of CMEs is mostly toward the equator, and during periods of maxima it is mostly toward the poles. This general trend of deflection is further modified by the specific structure of the magnetic field generated during successive cycles of solar activity (e.g., the asymmetry between the hemispheres). A systematic increase in deflection with time was also recognized. We have also found that the deflection increases linearly with the distance from the Sun in the LFOV (the line slope is 0.5)

Eruptions from coronal hole bright points:observations and non-potential modeling

Context. We report on the third part of a series of studies on eruptions associated with small-scale loop complexes named coronal bright points (CBPs).Aims. A single case study of a CBP in an equatorial coronal hole with an exceptionally large size is investigated to extend our understanding of the formation of mini-filaments (MFs), their destabilisation and the origin of the eruption triggering the formation of jet-like features recorded in the extreme-ultraviolet (EUV) and X-ray emission. We aim to explore the nature of the so called micro-flares in CBPs associated with jets in coronal holes and mini coronal mass ejections in the quiet Sun.Methods. Co-observations from the Atmospheric Imaging Assembly (AIA) and Helioseismic Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO), and GONG Halpha images are used together with a Non-Linear Force Free Field (NLFFF) relaxation approach, where the latter is based on a time series of HMI line-of-sight magnetograms.Results. A mini-filament (MF) that formed beneath the CBP arcade around 3–4 h before the eruption is seen in the Halpha and EUV AIA images to lift up and erupt triggering the formation of an X-ray jet. No significant photospheric magnetic flux concentration displacement (convergence) is observed and neither is magnetic flux cancellation between the two main magnetic polarities forming the CBP in the time period leading to the MF liftoff. The CBP micro-flare is associated with three flare kernels that formed shortly after the MF liftoff. No observational signature is found for reconnection beneath the erupting MF. The applied NLFFF modeling successfully reproduces both the CBP loop complex as well as the magnetic flux rope that hosts the MF.Conclusions. The applied NLFFF modellng is able to clearly show that an initial potential field can be evolved into a non-potential magnetic field configuration that contains free magnetic energy in the region that observationally hosts the eruption. The comparison of the magnetic field structure shows that the magnetic NLFFF model contains many of the features that can explain the dfferent observational signatures found in the evolution and eruption of the CBP. In future it may eventually indicate the location of destabilisation that results in the eruptions of flux ropes