Numerical simulation of the current sheet above solar spots

Current sheet (CS) creation in a region with anX-type zero magnetic field line in plasma was simulated by numerically solving the 3D MHD equations for conditions which were close to the solar corona: the disturbance propagated from the photosphere boundary under which the magnetic field sources were situated. Some of values (B,,V) were set on the photosphere boundary, while others were determined from the conditions inside the region. Several Alfvén times after its creation, the CS motion practically ceased, and the plasma velocity changed its direction above the sheet, so that the plasma flow was directed into the CS from both sides.     

An MHD model for a heliospheric current sheet

A numerical solution of the full set of MHD equations shows the generation of a heliospheric current sheet during the thermal expansion of the corona. Calculations were performed for a compressible plasma taking into account dissipative terms and anisotropy of the thermal conductivity of the magnetized plasma. It is shown that the current sheet is not magnetically neutral. The sheet contains a normal component of the magnetic field, which plays a fundamental role during the formation of the sheet and in the stationary state. The sheet is stable against MHD perturbations, which are apparently carried away by the plasma flow. For the numerical scheme chosen, the minimum sheet thickness is determined by the length of the spatial integration step. The PERESVET code was used for the calculations.     

Solar flare model: Comparison of the results of numerical simulations and observations

The electrodynamic flare model is based on numerical 3D simulations with the real magnetic field of an active region. An energy of ∼10³² erg necessary for a solar flare is shown to accumulate in the magnetic field of a coronal current sheet. The thermal X-ray source in the corona results from plasma heating in the current sheet upon reconnection. The hard X-ray sources are located on the solar surface at the loop foot-points. They are produced by the precipitation of electron beams accelerated in field-aligned currents. Solar cosmic rays appear upon acceleration in the electric field along a singular magnetic X-type line. The generation mechanism of the delayed cosmic-ray component is also discussed.     

锂辉石:巨型花岗伟晶岩锂-铯-钽矿床中关键含锂矿物SCIEI北大核心CSCD

寻找传统化石燃料的替代能源已成为全球性议题。受动力电池消费的拉动,锂资源需求急剧上升,伟晶岩型锂矿勘查热度持续攀升。虽然众多伟晶岩型锂矿地质特征尚不清晰,已有证据表明锂辉石是大多数大型-巨型伟晶岩型锂矿床的主要含锂矿物。与许多近直立的伟晶岩脉群不同,世界范围内大多数太古代伟晶岩矿脉往往呈近水平或缓倾斜在角闪岩相围岩中产出,它们往往具有复杂的三维形态并发育明显的矿物和地球化学分带。这些太古代伟晶岩脉通常形成于挤压或压剪构造体制下同变质环境中,成岩期最小主应力(σ;)近竖直。因此,伟晶岩常常侵位于近水平的构造局部引张区而形成复杂的几何学形态。压性的构造环境为富锂熔体多次脉动式注入和富含挥发分熔体垂向结晶分异提供了充足的时间;锂辉石在中高温压条件下结晶成为缓倾富锂带中最为常见的含锂矿物。     

Magnetohydrodynamic Simulation of Preflare Situations in the Solar Corona with the Use of Parallel Computing

Geomagnetism and Aeronomy - The use of parallel computations on Nvidia Tesla GPUs allows the magnetohydrodynamic (MHD) simulation of preflare situations in the solar corona above an active region...     

Simulation of the solar wind interaction with non-magnetic celestial bodies

Laboratory experiments are described to simulate the solar wind flowing around nonmagnetic planets for three cases: non-conducting and ideally conducting planets, and a planet with a gaseous shell. A glass sphere was used as a model of a non-conducting planet (the Moon). Spatial distributions of plasma density and magnetic field strength that have been obtained agree with the data from measurements in space. However, the magnetic field does not increase before the rarefaction wave in the model experiment. A field increase was observed only for a conducting lunella: this argues in favour of the existence of a high conduction region on the Moon. A wax ball was used to model phenomena on the day-side of non-magnetic celestial bodies with a gaseoue shell (Venus, comets). Its surface easily evaporates in the plasma flow, and ionized evaporation products form an artificial ionosphere. The magnetic field frozen in the plasma flow is shown to be a determinative factor in the formation of a sharp ionospheric boundary. The supersonic plasma flow that interacts with the ionosphere gives rise to a stationary shock wave.     

Geological and geophysical characteristics of hotspots of the Amur region

This study presents models of inactive and currently active hotspots of the Amur region that were developed based on the results obtained from seismogravitational modeling and a large–scale aeromagnetic survey in combination with other geological and geophysical data. The study considers the mechanisms triggering the evolutionary changes in the deep structure of the hotspots and the Maya—Selemdzha plume, as well as some characteristics of related ore–bearing regions.     

Magnetohydrodynamic simulation of a solar flare: 2. Flare model and simulation using active-region magnetic maps

The results of a three-dimensional MHD simulation and data obtained using specialized spacecraft made it possible to construct an electrodynamic model of solar flares. A flare results from explosive magnetic reconnection in a current sheet above an active region, and electrons accelerated in field-aligned currents cause hard X rays on the solar surface. In this review, we considered works where the boundary and initial conditions on the photosphere were specified directly from the magnetic maps, obtained by SOHO MDI in the preflare state, in order to simulate the formation of a current sheet. A numerical solution of the complete set of MHD equations, performed using the new-generation PERESVET program, demonstrated the formation of several current sheets before a series of flares. A comparison of the observed relativistic proton spectra and the simulated proton acceleration along a magnetic field singular line made it possible to estimate the magnetic reconnection rate during a flare (∼10⁷ cm s⁻¹). Great flares (of the X class) originate after an increase in the active region magnetic flux up to 10²² Mx.     

Convection and field-aligned currents, related to polar cap arcs, during strongly northward IMF (11 January 1983)

Electric and magnetic fields and auroral emissions have been measured by the Intercosmos-Bulgaria-1300 satellite on 10–11 January 1983. The measured distributions of the plasma drift velocity show that viscous convection is diminished in the evening sector under IMF B_y < 0 and in the morning sector if IMF B_y > 0. A number of sun-aligned polar cap arcs were observed at the beginning of the period of strongly northward IMF and after a few hours a θ-aurora appeared. The intensity of ionized oxygen emission [O⁺(²P), 7320 Å] increased significantly reaching up to several kilo-Rayleighs in the polar cap arc. A complicated pattern of convection and field-aligned currents existed in the nightside polar cap which differed from the four-cell model of convection and NBZ field-aligned current system. This pattern was observed during 12 h and could be interpreted as six large scale field-aligned current sheets and three convective vortices inside the polar cap. Sun-aligned polar cap arcs may be located in regions both of sunward and anti-sunward convection. Structures of smaller spatial scale correspond to the boundaries of hot plasma regions related to polar cap arcs. Obviously these structures are due to S-shaped distributions of electric potential. Parallel electric fields in these S-structures provide electron acceleration up to 1 keV at the boundaries of polar cap arcs. The pairs of field-aligned currents correspond to those S-structures: a downward current at the external side of the boundary and an upward current at the internal side of it.     

Field-aligned current generation at plasma clouds or bodies with plasma shells moving in magnetic fields

Field-aligned currents (FAC) can be generated during a plasma jet or the motion of a body with a plasma shell in a transverse magnetic field. They can be investigated in an active space experiment. For the proper choice of diagnostics and for evaluation of expected results a laboratory simulation is carried out. The preliminary results show FAC generation in conditions correlated with conditions in space.