Statistical relationships between variations of the geomagnetic field, auroral electrojet, and geomagnetically induced currents

Using observations from the IMAGE magnetic observatories and the station for recording geomagnetically induced currents (GIC) in the electric transmission line in 2015, we examine relationships between geomagnetic field and GIC variations. The GIC intensity is highly correlated (R>0.7) with the field variability |dB/dt| and closely correlated with variations in the time derivatives of X and Y components. Daily variations in the mean geomagnetic field variability |dB/dt| and GIC intensity have a wide night maximum, associated with the electrojet, and a wide morning maximum, presumably caused by intense Pc5–Pi3 geomagnetic pulsations. We have constructed a regression linear model to estimate GIC from the time derivative of the geomagnetic field and AE index. Statistical distributions of the probability density of the AE index, geomagnetic field derivative, and GIC correspond to the log-normal law. The constructed distributions are used to evaluate the probabilities of extreme values of GIC and |dB/dt|

Geoinformation system for analyzing the dynamics of extreme geomagnetic disturbances from observations of ground stations

Основываясь на данных наблюдения магнитных обсерваторий и вариационных станций, публикуемых на портале SuperMAG, предлагается и верифицируется подход к построению специализированной веб-ГИС на базе микросервисной архитектуры, обеспечивающей аналитический контроль возмущенной составляющей вариаций геомагнитного поля. Реализованный в рамках данной системы метод пространственной интерполяции геомагнитных данных в совокупности с предложенной схемой их ранжировки и интерпретации, а также способом визуализации в виде изолиний позволяет отслеживать структуру, наблюдать динамику, выявлять вероятные регионы, длительность и временные интервалы возникновения экстремальных геомагнитных возмущений. The paper is concerned with an approach to developing a specialized web-GIS based on a microservice architecture that provides analytical control of the disturbed component of geomagnetic field variations, according to observation data from magnetic observatories and variational stations published on the SuperMAG portal . A method of spatial interpolation of geomagnetic data implemented in the proposed web-GIS, together with the proposed scheme for ranking and interpreting them, as well as a visualization method in the form of isolines, allows a user to track the structure, observe the dynamics, identify probable regions, duration and time intervals of the occurrence of extreme geomagnetic disturbances.Работа поддержана грантами РНФ 17-77-20034 и РФФИ № 20-07-00011-а, а также Министерством науки и высшего образования РФ в рамках выполнения работ по Государственному заданию ФГБОУ ВО УГАТУ # FEUE-2020-0007 по теме «Теоретические основы моделирования и семантического анализа процессов преобразования вихревых электромагнитных полей в инфокоммуникационных системах»

Role of dislocations in formation of ohmic contacts to heavily doped n-Si

We present experimental results concerning a high density of structural defects (in particular, dislocations) in the near-contact region of heavily doped n-silicon. They appear in the course of firing Au Pd Ti Pd -Si n ohmic contact at 450С for 10 min in a vacuum of ~10 Pa⁻⁴ . These defects lead to appearance of metal shunts that determine the current flow mechanism in these ohmic contacts. The calculated and experimental temperature dependences of contact resistivity, ρс(Т), are in good agreement. It is shown that ρс increases with temperature. This is characteristic of a model of ohmic contacts with a high dislocation density in the near-contact region of semiconducto

On a feature of temperature dependence of contact resistivity for ohmic contacts to n-Si with an n⁺ -n doping step

We present both theoretical and experimental temperature dependences of contact resistivity ρс(Т) for ohmic contacts to the silicon n⁺ -n-structures whose n⁺ -layer was formed using phosphorus diffusion or ion implantation. The ρс(Т) dependence was measured in the 125–375 K temperature range with the transmission line method, with allowance made for conduction in both the n⁺ -layer and n⁺ -n doping step

Statistical characteristics of the spatial distribution of Pc3-4 geomagnetic pulsations at high latitudes in the Antarctic regions

The diumal variations in the parameters of Pc3 (20–60 mHz) and Pc4 (10–19 mHz) pulsations at latitudes of the dayside cusp and polar cap have been studied using data of the magnetic stations of the trans-Antarctic meridional profile for the time interval from January to March 1997 (local summer) under weakly disturbed geomagnetic conditions (AE ≤ 250 nT). The technique for estimating pulsation parameters is based on the separation of the wave packets and noise. The diumal variations in the hourly average parameters of the wave packets in the Pc3 and Pc4 bands and noise in the Pc3-4 band (10–60 mHz)—the average number of wave packets, energy of wave packets and noise, and energy of a single wave packet—turned out to be different for the stations located deep in the polar cap (Φ ∼ 87°) and at the latitudes of the dayside polar cusp (Φ ∼ 70°) and auroral oval (Φ ∼ 66°). Several sources of pulsations caused by different channels of wave energy penetration into the magnetosphere through the dayside cusp, dayside magnetopause, and dawn flank of the magnetotail apparently exist at high latitudes

Seasonal and diurnal dependences of Pc3 and Pc4 geomagnetic pulsation power at very high latitudes

Introduction In our studies [Chugunova et al., 2002,03,04] we found the occurrence of ULF waves in the nominal Рс3-4 band in the polar cap. About 15% of this ULF activity is constituted by quasi-monochromatic waves. Though the mechanism of these waves in the region with open field lines has not been found yet [e.g., Pilipenko et al., 2004], inthis study we try to examine statistically the seasonal and yearly variations of signals and noise in the Рс3 and Рс4range. The data of observations in Antarctica have been used, where there is practically no industrial electromagnetic interference

Suppression of the dayside magnetopause surface modes

Magnetopause surface eigenmodes were suggested as a potential source of dayside high-latitude broadband pulsations in the Pc5-6 band (frequency about 1–2 mHz). However, the search for a ground signature of these modes has not provided encouraging results. The comparison of multi-instrument data from Svalbard with the latitudinal structure of Pc5-6 pulsations, recorded by magnetometers covering near-cusp latitudes, has shown that often the latitudinal maximum of pulsation power occurs about 2–3° deeper in the magnetosphere than the dayside open-closed field line boundary (OCB). The OCB proxy was determined from SuperDARN radar data as the equatorward boundary of enhanced width of a return radio signal. The OCB-ULF correspondence is further examined by comparing the latitudinal profile of the near-noon pulsation power with the equatorward edge of the auroral red emission from the meridian scanning photometer. In most analyzed events, the “epicenter” of Pc5-6 power is at 1–2° lower latitude than the optical OCB proxy. Therefore, the dayside Pc5-6 pulsations cannot be associated with the ground image of the magnetopause surface modes or with oscillations of the last field line. A lack of ground response to these modes beneath the ionospheric projection of OCB seems puzzling. As a possible explanation, we suggest that a high variability of the outer magnetosphere near the magnetopause region may suppress the excitation efficiency. To quantify this hypothesis, we consider a driven field line resonator terminated by conjugate ionospheres with stochastic fluctuations of its eigenfrequency. A solution of this problem predicts a substantial deterioration of resonant properties of MHD resonator even under a relatively low level of background fluctuations. This effect may explain why there is no ground response to magnetopause surface modes or oscillations of the last field line at the OCB latitude, but it can be seen at somewhat lower latitudes with more regular and stable magnetic and plasma structure