The initial trajectories of eruptive solar prominences

Trajectories of eruptive prominences are compared with the shapes of coronal neutral surfaces calculated in a potential approximation using photospheric measurements. Space-based Solar Dymamics Observatory and STEREO observations carried out at different viewing angles enable a precise determination of a prominence’s position at successive times during its eruption. In the initial segments of their trajectories, eruptive prominences move along neutral surfaces (B_r = 0) of the potential coronal magnetic field. This can be used to predict the directions of subsequent coronal mass ejections and to estimate their geoefficiency.     

Composition and formation settings of the siliceous-volcanogenic complexes of the Nizhneussuriisk segment,Kiselevka-Manoma terrane,West Sikhote Alin

This paper reports new data on the mineralogical-petrographical composition, genetic types of sedimentary rocks, and geochemical features of the volcanic rocks of the Snarsky area of the Nizhneussuriisk segment of the Kiselevka-Manoma accretionary complex, which is developed on the right bank of the lower reaches of the Ussuri River. The Middle Jurassic-Aptian sedimentary rocks of the area are represented by pelagic radiolarian cherts, semipelagic siliceous-clayey deposits, subordinate shallow limestones, volcanomictic conglomerates, and turbidite sandstones. The basalts of the area are represented by alkaline basalts resembling within-plate ocean-island basalts and N-MORB-type tholeiitic basalts. Rock associations of two physicogeographical and geodynamic settings are distinguished: the pelagic setting with within-plate alkaline volcanic rocks and the hemipelagic one with volcanic edifices of spreading basalts.     

Coronal mass ejections and eruptive prominences: Mutual spatial arrangement

The mutual spatial arrangement of coronal mass ejections and eruptive prominences on the Sun is considered. These phenomena occur on different scales and are observed at different heights above the solar surface. In spite of the presumed causal connection between them, they are often widely separated in position angle at epochs of solar minimum. This means that the motion of a prominence in the corona is not strictly radial and has an appreciable component along the surface. This behavior can be explained in a model of a filament as a magnetic flux rope in equilibrium in the coronal magnetic field. The initial trajectory of the filament is determined by the structure of the global field.     

Spatial–Temporal CO2 Variations near St. Petersburg Based on Satellite and Ground-Based Measurements

Izvestiya, Atmospheric and Oceanic Physics - The results of studying spatial–temporal CO2 variations near St. Petersburg in 2014–2017 based on satellite measurements (OCO-2 satellite)...     

Application of Geoinformational Technologies and Aerospace Photography Materials for Monitoring the Land Irrigated by the Svetlyi Yar Irrigation System (Volgograd Oblast)

Izvestiya, Atmospheric and Oceanic Physics - The experience of constructing a geoinformational system (GIS) of the Svetlyi Yar irrigation system (Volgograd oblast) for monitoring the status of...     

Equatorial Plasma Bubbles: Variation of the Longitudinal Distribution with Altitude

Geomagnetism and Aeronomy - The equatorial plasma “bubbles” that form at the bottom-side of the F-layer are affected by zonal plasma drift when they rise to greater altitudes. Under the...     

Wind Preparation of the Generation of Equatorial Plasma “Bubbles”

Geomagnetism and Aeronomy - According to theoretical conclusions, zonal western thermospheric winds are the key influence on the generation of equatorial plasma “bubbles.” To verify...