N. A. Kurazhkovskaya

Relation between Geomagnetic Field Intensity and Peculiarities of Its Variations with Inversion Frequency

The assumption that the variation of the ancient geomagnetic field (GF) is governed by processes in the Earth’s core is usually accepted without question. Numerical modeling of the evolution of αω -dynamo showed that change in the characteristics of the GF (paleointensity variations and inversion frequency) should correlate [1, 2]. However, the search for the correlation of paleointensity and inversion frequency has not been successful up to the present time owing to the lack of paleomagnetic data [3, 4]. Our reconstructions of paleointensity in the Jurassic and Cretaceous based on sedimentary rocks widened significantly the information dataset about this characteristic of the geomagnetic field. The summary of the author’s data on paleointensity obtained for the sedimentary rocks and world data based on thermomagnetized rocks provided a new basis for constructing the dynamics of the GF intensity and investigating the correlation between the characteristics of the magnetic field. Reconstruction of the fragments of GF intensity was based on the analysis of sedimentary rock collections gathered on the Russian Plate and adjacent territories [5, 6]. Previously, these collections were used for constructing the Middle Jurassic‐Cretaceous regional magnetostratigraphic scale [7]. The results of determinations of paleointensity based on thermomagnetized rocks were taken from the database (DB) at http://www. brk.adm.yar.ru/palmag/index.html. The information about inversions is mainly taken from [8]. The Albian‐ Coniacian interval is an exception. The frequency of the Albian‐Coniacian inversions was plotted from the more complete data in [7].

Geomagnetic (MIE) and storm sudden commencement (SSC) impulses in a high-latitude magnetosphere

Amplitude regularities, intermittence statistics, and conditions of generation of magnetic (mag- netic impulse event, MIE) and geomagnetic storm sudden commencement (SSC) impulses were compara- tively analyzed. Common and different properties of MIE and SSC impulses observed in a high-latitude mag- netosphere were detected. It was shown that MIE impulses are observed against a background of relatively stable interplanetary medium parameters and mostly when the IMF sector structure is negative. SSC impulses are observed against a background of sharply increasing solar wind and IMF parameters and when the IMF sector structure is positive. The amplitude dynamics, depending on the geomagnetic latitude of MIE and SSC impulses relative to the noon meridian, as well as in the daytime and nighttime MLT sectors, is sim- ilar. The dynamics of the intermittence indices (α), depending on the geomagnetic latitude of MIE and SSC impulses in the same MLT sectors, is antiphase. Independently of the IMF sector structure, the amplitudes of MIE and SSC impulses increase with increasing geomagnetic latitude, and the intermittence indices change in antiphase. It is assumed that the degree of plasma turbulence at the front boundary of magneto- sphere at moderate geomagnetic activity is relatively high and sufficient for the generation of MIE impulsive regimes. At the same time, SSC impulses originate at a lower turbulence level in the subsolar magnetospheric region but under the external action of solar wind inhomogeneities on the magnetosphere.

Intermittency in wave processes

The paper generalizes results of study of the intermittency pattern in some wave processes of the burst type in the high-latitude magnetosphere of the Earth. Based on the analysis of distributions of amplitudes and interpeak intervals, it is shown that generation regimes of magnetic impulse events, ipclpulsation burst series, and Pi3 pulsations possess the properties of intermittent processes and are associated with the development of plasma turbulence in their generation regions. The degree of turbulence of the high-latitude magnetosphere plasma is estimated at a qualitative level. Burst-type structures whose behavior corresponds to a typical intermittent process are discovered in variations of the ancient geomagnetic field.

Stochastic behavior of geomagnetic field in the Middle Jurassic-Paleogene

The distribution of the paleointensities and the lengths of geomagnetic polarity intervals (time intervals between the successive reversals of the Earth’s magnetic field) corresponding to the different geological epochs was studied. It was found that the stochastic series of paleointensities in most cases are best approximated by the power-law function. The exponents of the power-law distributions vary depending on the intervals of the geological time that accommodate the analyzed paleomagnetic data. The distributions of the lengths of polarity intervals are approximated by the exponential function. The exponents varied depending also on the intervals of the geological time. The analysis shows that the most significant changes in the behavior of paleointensity occurred in the Paleogene near the Paleocene-Eocene boundary. Based on the analysis of the paleomagnetic data, it is hypothesized that turbulence of the magnetoactive medium played an important role in the generation of the Earth’s magnetic field. The turbulence of the magnetoactive medium increased in the Cretaceous compared to the Jurassic and Paleogene.

Stratification of Horizons in Bottom Sediments of the Rybinsk Reservoir

Physical properties of cores taken from sediments in the channel zone of the Volga Stretch in the Rybinsk Reservoir are studied. The physical properties of the sediments are shown to be related to the evolution of geomorphological processes and the amount of organic matter in the sediment. Variations in the physical properties were used to recognize synchronous formation of sediment horizons corresponding to certain formation stages of the reservoir soil complex and anomalous environmental and climatic events. Three stages of channel sedimentation are established based on characteristic behavior of magnetic parameters and organic matter content. The magnetic parameters of sediments are shown to allow data reconstruction on some environmental and hydrological processes.

Paleointensity Behavior and Intervals Between Geomagnetic Reversals in the Last 167 Ma

The results of comparative analysis of the behavior of paleointensity and polarity (intervals between reversals) of the geomagnetic field for the last 167 Ma are presented. Similarities and differences in the behavior of these characteristics of the geomagnetic field are discussed. It is shown that bursts of paleointensity and long intervals between reversals occurred at high mean values of paleointensity in the Cretaceous and Paleogene. However, there are differences between the paleointensity behavior and the reversal regime: (1) the characteristic times of paleointensity variations are less than the characteristic times of the frequency of geomagnetic reversals, (2) the achievement of maximum values of paleointensity at the Cretaceous–Paleogene boundary and the termination of paleointensity bursts after the boundary of 45–40 Ma are not marked by explicit features in the geomagnetic polarity behavior.

Statistical Study of the Characteristics of Isolated Bursts of Midlatitude Pi 2 Geomagnetic Pulsations

The characteristics and interplanetary excitation conditions of isolated bursts of Pi2 geomagnetic pulsations observed during the development of magnetospheric substorms (substorm Pi2) and in its absence (nonsubstorm Pi2) on the night side of the Earth are comparatively analyzed. It is shown that, regardless of the local time and season, the amplitude of isolated Pi2 substorm bursts is always higher than that of the nonsubstorm ones, and the periods and duration of the wave packets of substorm Pi2 bursts are less than those of nonsubstorms. Diurnal and seasonal variations in the characteristics of the two groups of Pi2 bursts differ in the form and position of maxima and minima. It is found that the start of excitation of isolated Pi2 bursts, during substorms and in its absence, is controlled by the preferred direction of the interplanetary magnetic field (IMF) vector perpendicular to the Sun–Earth line (angle θxB = arccos(Bx/B) → 90°). It is assumed that isolated Pi2 bursts of both groups are triggered by reorientation of the IMF vector in the ecliptic plane and the plane perpendicular to it ~15 min before their onset. The most likely source of midlatitude isolated Pi2 bursts during substorm development and in its absence are bursty bulk flows (BBFs) in the plasma sheet of the magnetospheric tail, the regularities of which coincide in many respects with the observed features of Pi2 bursts.

Isolated bursts of irregular geomagnetic pulsations in the region of the dayside cusp

In this work, the results of comparative analysis of morphological regularities of right-polarized (R type) and left-polarized (L type) isolated bursts of ipcl pulsations (irregular pulsations continuous long period) with an anomalously large amplitude in the region of the daytime polar cusp, as well as conditions of their excitation, are presented. It has been found that R and L bursts are similar in the maximum amplitude level, wave packet duration, spectral composition, magnitude of ellipticity, diurnal variation shape, and other characteristics. At the same time, bursts of the R and L type are excited at different degrees of plasma turbulence in the generation region, at different IMF orientations in the plane of ecliptic, as well as in the plane perpendicular to it, and at different dynamics of the parameter β (characterizing the ratio of the thermal pressure to the magnetic pressure) and Alfvén Mach number Ma. It is supposed that the generation of isolated bursts of the R and L types can be related to the amplification of the plasma turbulence level due to the development of wind instability at the front boundary of the magnetosphere, and features of their polarization can be interpreted in the scope of the model of nonlinear propagation of Alfvén waves.

Long-period irregular pulsations under the conditions of a quiet magnetosphere

Simultaneous observations of high-latitude long-period irregular pulsations at frequencies of 2.0–6.0 mHz (ipcl) and magnetic field disturbances in the solar wind plasma at low geomagnetic activity (Kp ~ 0) have been studied. The 1-s data on the magnetic field registration at Godhavn (GDH) high-latitude observatory and the 1-min data on the solar wind plasma and IMF parameters for 2011–2013 were used in an analysis. Ipcl (irregular pulsations continuous, long), which were observed against a background of the IMF Bz reorientation from northward to southward, have been analyzed. In this case other solar wind plasma and IMF parameters, such as velocity V, density n, solar wind dynamic pressure P = ρV2 (ρ is plasma density), and strength magnitude B, were relatively stable. The effect of the IMF Bz variation rate on the ipcl spectral composition and intensity has been studied. It was established that the ipcl spectral density reaches its maximum (~10–20 min) after IMF Bz sign reversal in a predominant number of cases. It was detected that the ipcl average frequency (f) is linearly related to the IMF Bz variation rate (ΔBz/Δt). It was shown that the dependence of f on ΔBz/Δt is controlled by the α = arctan(By/Bx) angle value responsible for the MHD discontinuity type at the front boundary of magnetosphere. The results made it possible to assume that the formation of the observed ipcl spectrum, which is related to the IMF Bz reorientation, is caused by solar wind plasma turbulence, which promotes the development of current sheet instability and surface wave amplification at the magnetopause.