Magnetosphere Ionosphere Research Articles

Entangled dynamos and Joule heating in the Earth's ionosphere

Abstract. The Earth's neutral atmosphere is the driver of the well-known solar quiet (Sq) and other magnetic variations observed for more than 100 years. Yet the understanding of how the neutral wind can accomplish a dynamo effect has been incomplete. A new viable model is presented where a dynamo effect is obtained only in the case of winds perpendicular to the magnetic field B that do not map along B. Winds where u×B is constant have no effect. We identify Sq as being driven by wind differences at magnetically conjugate points and not by a neutral wind per se. The view of two different but entangled dynamos is favoured, with some conceptual analogy to quantum mechanical states. Because of the large preponderance of the neutral gas mass over the ionized component in the Earth's ionosphere, the dominant effect of the plasma adjusting to the winds is Joule heating. The amount of global Joule heating power from Sq is estimated, with uncertainties, to be much lower than Joule heating from ionosphere–magnetosphere coupling at high latitudes in periods of strong geomagnetic activity. However, on average both contributions could be relatively comparable. The global contribution of heating by ionizing solar radiation in the same height range should be 2–3 orders of magnitude larger.

Magnetospheric Multiscale Observations of the Off-equatorial Dipolarization Front Dynamics in the Terrestrial Magnetotail

Abstract We report the Magnetospheric Multiscale observations of dynamics at an off-equatorial dipolarization front (DF) in the Terrestrial Magnetotail. Three different plasma waves, namely electromagnetic ion cyclotron (EMIC) waves, lower hybrid drift waves, and electrostatic solitary waves (ESWs), associated with different electron pitch angle distributions were detected at different subregions of a single DF. It is interesting to note that the EMIC wave was linearly polarized, associating with a parallel current as a result of the antiparallel drift of electrons in the energy range of about 0.3–2 keV. These suggest that the wave was most likely to be locally generated. This generation could be explained by the current-driven kink-like instability due to the electron drift. The current-driven instabilities may dissipate the energy of the field-aligned current at the DF and thus play important roles in the magnetosphere–ionosphere coupling. On the other hand, the detected ESWs are interpreted as multidimensional electromagnetic electron holes (EHs) which are manifestations of several distinguishing features in electric and magnetic field perturbation. The EHs with a strong positive central potential suggested the likelihood of nonlinear behavior.

Statistical Analysis of Infrasonic Parameters Generated by the Chelyabinsk Meteoroid

The passage of the Chelyabinsk meteoroid generated a wide variety of physical effects in all subsystems in the Earth–atmosphere–ionosphere–magnetosphere system. Earlier studies have been conducted in order to examine the Chelyabinsk meteoroid’s effects in the atmosphere, ionosphere, and the geomagnetic field. Particular attention has been given to the features of the infrasound signal generated by the Chelyabinsk meteoroid. At the same time, the results of the statistical analysis of infrasonic parameters are absent in the literature. The purpose of this paper is to construct scatter diagrams for basic infrasonic parameters of the signal propagating globally (such as signal-to-noise ratios, time lags, celerity, time durations, amplitudes, and periods per cycle) depending on either the distance between the infrasound source and the sensor or the source back-azimuth as well as to fit respective regression lines. The data have been retrieved from 15 infrasound stations of the International Monitoring System (IMS) set up by the Comprehensive Nuclear-Test-Ban Treaty Organization (CTBTO). On individual occasions, these data have been complemented by the data acquired by the infrasound stations located at the Eurasian geophysical observatories. Scatter diagrams have been constructed for basic parameters of the infrasonic signal propagating globally. The estimated regression lines superimposed on the scatter diagrams of these parameters versus distance or back-azimuth are shown. Estimates of the infrasound signal celerity (approximately 280 m/s) and tropospheric and stratospheric wind speed (approximately 30 m/s) averaged over all propagation paths have been determined. The advantages and disadvantages of the proposed regression lines are discussed.

Feedback and Ballooning Instabilities in the Magnetosphere‐Ionosphere Coupling

AbstractA unified model for the feedback and ballooning instabilities in the magnetosphere‐ionosphere (M‐I) coupling is developed by means of the reduced magnetohydrodynamic and two‐fluid equations, involving the local current closure and the ionospheric conductivity change in a scale of auroral fine structures, self‐consistently. In a low pressure gradient case, the Alfvén harmonics are destabilized through the feedback mechanism, while the ballooning instability appears if the magnetospheric pressure gradient exceeds a critical value. Transition of the dominant instability between the feedback and ballooning modes is brought by change of the normalized pressure gradient or the convection electric field in the magnetosphere. The obtained results imply a variety of appearance of auroral arcs and beads in the M‐I coupling system.

Dynamical Complexity of the 2015 St. Patrick's Day Magnetic Storm at Swarm Altitudes Using Entropy Measures.

The continuously expanding toolbox of nonlinear time series analysis techniques has recently highlighted the importance of dynamical complexity to understand the behavior of the complex solar wind–magnetosphere–ionosphere–thermosphere coupling system and its components. Here, we apply new such approaches, mainly a series of entropy methods to the time series of the Earth’s magnetic field measured by the Swarm constellation. We show successful applications of methods, originated from information theory, to quantitatively study complexity in the dynamical response of the topside ionosphere, at Swarm altitudes, focusing on the most intense magnetic storm of solar cycle 24, that is, the St. Patrick’s Day storm, which occurred in March 2015. These entropy measures are utilized for the first time to analyze data from a low-Earth orbit (LEO) satellite mission flying in the topside ionosphere. These approaches may hold great potential for improved space weather nowcasts and forecasts.

Implications for Magnetosphere‐Ionosphere Coupling From Jupiter's System IV Quasi‐Period

AbstractThe Io plasma torus exhibits a fundamental rotational periodicity distinct from the rotation of the magnetic field that is easily observed in physical components such as ultraviolet emission or ionic mixing ratios, yet this distinct periodicity has no widely accepted explanation. To seek the origins of this additional periodicity, called System IV, a two‐dimensional (radial and azimuthal) physical chemistry model (Copper et al., 2016), is used to investigate the torus response to a prescribed System III hot electron modulation following Steffl et al. (2008) and an additional hot electron modulation that we relate to various transport and mass loading parameters. The model thus self‐consistently generates a radially independent periodicity consistent with that of System IV. We argue that the origin of this periodicity is the interplay between chemical and transport time scales working to prevent an azimuthal shearing of the hot electron modulation due to the physical subcorotation profile. We also examine recent observations (Tsuchiya et al., 2019,) that volcanic eruptions return the System IV periodicity toward rigid corotation with System III, counter to previous magnetosphere‐ionosphere(MI) coupling models that examined mass loading (Pontius & Hill, 1982, ). Instead, the return to corotation implies improved MI coupling, possibly due to a transport‐related increase in hot electrons following the eruption. Thus, we argue that the System IV periodicity is a diagnostic of MI coupling efficiency at Jupiter and the ultimate result of energy dissipation associated with Alfvénic coupling to the planet.

Coupling between the Magnetospheric Dipolarization Front and the Earth’s Ionosphere by Ultralow-frequency Waves

Abstract Magnetosphere–ionosphere coupling is representative of a class of astrophysical problems involving the interaction between very different plasma regimes that are connected by magnetic fields. It is a major issue of the planet’s (e.g., Earth, Jupiter, Saturn) system how the magnetospheric plasma is coupled to the planet’s ionosphere/atmosphere. Due to their roles on energy transport and conversion in the terrestrial magnetosphere, dipolarization fronts (DFs) in the magnetotail have been intensively studied. While the energy may also be transported toward the ionosphere during the magnetosphere–ionosphere coupling, the coupling processes during DF events remain unclear. Using high-quality MMS and Swarm measurements, we present new conjugated observations of ultralow-frequency waves associated with the DF in the magnetotail and multiscale field-aligned currents (FACs) in the ionosphere. The tail large-amplitude low-frequency magnetic disturbances and associated FACs were found connected with a pair of ionospheric FACs near the magnetic footprints of MMS. The earthward field-aligned Poynting flux of low-frequency waves reveals the energy transport from the DF toward the ionosphere. Meanwhile, small-scale and highly temporal ionospheric FACs suggest that the magnetotail shear Alfvén waves may evolve into kinetic Alfvén waves during the coupling processes. This finding implies that a very localized dynamic process (e.g., DFs in the terrestrial magnetotail) in the magnetosphere could couple the ionosphere with Alfvén waves.

Magnetohydrodynamic modelling of star–planet interaction and associated auroral radio emission

ABSTRACT We present calculations of auroral radio powers of magnetized hot Jupiters orbiting Sun-like stars, computed using global magnetohydrodynamic (MHD) modelling of the magnetospheric and ionospheric convection arising from the interaction between the magnetosphere and the stellar wind. Exoplanetary auroral radio powers are traditionally estimated using empirical or analytically derived relations, such as the radiometric Bode’s law (RBL), which relates radio power to the magnetic or kinetic energy dissipated in the stellar wind–planet interaction. Such methods risk an oversimplification of the magnetospheric electrodynamics giving rise to radio emission. As the next step towards a self-consistent picture, we model the stellar wind–magnetosphere–ionosphere coupling currents using a 3D MHD model. We compute electron-cyclotron maser instability-driven emission from the calculated ionospheric field-aligned current density. We show that the auroral radio power is highly sensitive to interplanetary magnetic field (IMF) strength, and that the emission is saturated for plausible hot Jupiter Pedersen conductances, indicating that radio power may be largely independent of ionospheric conductance. We estimate peak radio powers of 1014 W from a planet exposed to an IMF strength of 103 nT, implying flux densities at a distance of 15 pc from Earth potentially detectable with current and future radio telescopes. We also find a relation between radio power and planetary orbital distance that is broadly consistent with results from previous analytic models of magnetosphere–ionosphere coupling at hot Jupiters, and indicates that the RBL likely overestimates the radio powers by up to two orders of magnitude in the hot Jupiter regime.

AMPERE polar cap boundaries

Abstract. The high-latitude atmosphere is a dynamic region with processes that respond to forcing from the Sun, magnetosphere, neutral atmosphere, and ionosphere. Historically, the dominance of magnetosphere–ionosphere interactions has motivated upper atmospheric studies to use magnetic coordinates when examining magnetosphere–ionosphere–thermosphere coupling processes. However, there are significant differences between the dominant interactions within the polar cap, auroral oval, and equatorward of the auroral oval. Organising data relative to these boundaries has been shown to improve climatological and statistical studies, but the process of doing so is complicated by the shifting nature of the auroral oval and the difficulty in measuring its poleward and equatorward boundaries. This study presents a new set of open–closed magnetic field line boundaries (OCBs) obtained from Active Magnetosphere and Planetary Electrodynamics Response Experiment (AMPERE) magnetic perturbation data. AMPERE observations of field-aligned currents (FACs) are used to determine the location of the boundary between the Region 1 (R1) and Region 2 (R2) FAC systems. This current boundary is thought to typically lie a few degrees equatorward of the OCB, making it a good candidate for obtaining OCB locations. The AMPERE R1–R2 boundaries are compared to the Defense Meteorological Satellite Program Special Sensor J (DMSP SSJ) electron energy flux boundaries to test this hypothesis and determine the best estimate of the systematic offset between the R1–R2 boundary and the OCB as a function of magnetic local time. These calibrated boundaries, as well as OCBs obtained from the Imager for Magnetopause-to-Aurora Global Exploration (IMAGE) observations, are validated using simultaneous observations of the convection reversal boundary measured by DMSP. The validation shows that the OCBs from IMAGE and AMPERE may be used together in statistical studies, providing the basis of a long-term data set that can be used to separate observations originating inside and outside of the polar cap.

Interhemispheric Asymmetries in the Ground Magnetic Response to Interplanetary Shocks: The Role of Shock Impact Angle

AbstractInterplanetary (IP) shocks drive magnetosphere‐ionosphere (MI) current systems that in turn are associated with ground magnetic perturbations. Recent work has shown that IP shock impact angle plays a significant role in controlling the subsequent geomagnetic activity and magnetic perturbations; for example, highly inclined shocks drive asymmetric MI responses due to interhemispherical asymmetric magnetospheric compressions, while almost head‐on shocks drive more symmetric MI responses. However, there are few observations confirming that inclined shocks drive such asymmetries in the high‐latitude ground magnetic response. We use data from a chain of Antarctic magnetometers, combined with magnetically conjugate stations on the west coast of Greenland, to test these model predictions (Oliveira & Raeder, 2015, https://doi.org/10.1002/2015JA021147; Oliveira, 2017, https://doi.org/10.1007/s13538-016-0472-x). We calculate the time derivative of the magnetic field ( ) in each hemisphere separately. Next, we examine the ratio of Northern to Southern Hemisphere intensities and the time differences between the maximum immediately following the impact of IP shocks. We order these results according to shock impact angles obtained from a recently published database with over 500 events and discuss how shock impact angles affect north‐south hemisphere asymmetries in the ground magnetic response. We find that the hemisphere the shock strikes first usually has (1) the first response in and (2) the most intense response in . Additionally, we show that highly inclined shocks can generate high‐latitude ground magnetic responses that differ significantly from predictions based on models that assume symmetric driving conditions.

European Space Agency SMILEand Czech participation

AbstractSMILE (Solar wind Magnetosphere Ionosphere Link Explorer) is a space mission which aims to measure Earth's global system responses to solar wind and geomagnetic variations with innovative instrumentation, for example, wide–field X‐ray telescope of Lobster–Eye type, on board. It is a collaborative project of the European Space Agency and the Chinese Academy of Sciences. The SMILE international consortium involves the Czech Technical University in Prague and the Czech teams are expected to contribute to the project, mainly to the science and software related to the X–ray telescope. The aim of this short paper is to provide an outline of SMILE and in particular of the Czech participation to this mission, with emphasis on observation of celestial X‐ray sources as SMILE secondary science.

Modeled IMF By Effects on the Polar Ionosphere and Thermosphere Coupling

AbstractThere is still an inadequate understanding of how the interplanetary magnetic field (IMF) east‐west component (By) affects thermospheric composition, and other ionospheric and thermospheric fields in a systematic way. Utilizing the state‐of‐art first‐principles Coupled Magnetosphere Ionosphere Thermosphere (CMIT) modeling and TIMED/Global Ultraviolet Imager (GUVI)‐observed ΣO/N2 covering an entire solar cycle (year 2002–2016), as well as a neutral parcel trajectory tracing technique, we emphasize that not only the direction of By, but also its strength relative to the IMF north‐south component (Bz) that has important effects on high latitude convection, Joule heating, electron density, neutral winds, and neutral composition patterns in the upper thermosphere. The Northern Hemisphere convection pattern becomes more twisted for positive By cases than negative cases: the dusk cell becomes more rounded compared with the dawn cell. Consequently, equatorward neutral winds are stronger during postmidnight hours in negative By cases than in positive By cases, creating a favorable condition for neutral composition disturbances (characterized by low ΣO/N2) to expand to lower latitudes. This may lead to a more elongated ΣO/N2 depletion area along the morning‐premidnight direction for negative By conditions compared with the positive By conditions. Backward neutral parcel trajectories indicate that a lower ΣO/N2 parcel in negative By cases comes from lower altitudes, as compared with that for positive By cases, leading to larger enhancements of N2 in the former case.

Measuring Information Coupling between the Solar Wind and the Magnetosphere–Ionosphere System

The interaction between the solar wind and the Earth’s magnetosphere–ionosphere system is very complex, being essentially the result of the interplay between an external driver, the solar wind, and internal processes to the magnetosphere–ionosphere system. In this framework, modelling the Earth’s magnetosphere–ionosphere response to the changes of the solar wind conditions requires a correct identification of the causality relations between the different parameters/quantities used to monitor this coupling. Nowadays, in the framework of complex dynamical systems, both linear statistical tools and Granger causality models drastically fail to detect causal relationships between time series. Conversely, information theory-based concepts can provide powerful model-free statistical quantities capable of disentangling the complex nature of the causal relationships. In this work, we discuss how to deal with the problem of measuring causal information in the solar wind–magnetosphere–ionosphere system. We show that a time delay of about 30–60 min is found between solar wind and magnetospheric and ionospheric overall dynamics as monitored by geomagnetic indices, with a great information transfer observed between the z component of the interplanetary magnetic field and geomagnetic indices, while a lower transfer is found when other solar wind parameters are considered. This suggests that the best candidate for modelling the geomagnetic response to solar wind changes is the interplanetary magnetic field component . A discussion of the relevance of our results in the framework of Space Weather is also provided.

ULF waves observed in solar wind and on the ground at high, mid, and low latitudes

We analyze fluctuations of the magnetic field in the solar wind registered by the ACE satellite in the L1 Lagrangian point and the ULF waves observed with ground magnetometers at high, middle, and low latitudes during 84 intense substorm events. Our goal is to establish possible connections between ULF oscillations observed simultaneously in the different parts of the solar wind–magnetosphere–ionosphere system during substorms. Our analysis reveals that there is a good correlation between oscillations with frequencies less than 1 mHz observed in the solar wind and in three different latitudes during strong substorms. In particular, we show that: (1) the dominant frequencies of the waves observed on the ground at high, middle, and low latitudes are approximately the same; (2) the waves with frequencies of 0.45–0.55mHz, and 0.75–0.80mHz are the most often seen in high, middle, and low latitudes and in the solar wind. Therefore, we conclude that there is a strong coupling between the Earth’s magnetosphere–ionosphere system and the solar wind in the frequency range below 1mHz mediated by the disturbances in the magnetic field.

The semiannual variation of transpolar arc incidence and its relationship to the Russell–McPherron effect

Earth’s aurora is a luminescent phenomenon generated by the interaction between magnetospheric precipitating particles and the upper atmosphere; it plays an important role in magnetosphere–ionosphere (M-I) coupling. The transpolar arc (TPA) is a discrete auroral arc distributed in the noon-midnight direction poleward of the auroral oval and connects the dayside to the nightside sectors of the auroral oval. Studying the seasonal variation of TPA events can help us better understand the long-term variation of the interaction between the solar wind, the magnetosphere, and M-I coupling. However, a statistical study of the seasonal variation of TPA incidence has not previously been carried out. In this paper, we have identified 532 TPA events from the IMAGE database (2000–2005) and the Polar database (1996–2002), and calculated the incidence of TPA events for different months. We find a semiannual variation in TPA incidence. Clear peaks in the incidence of TPAs occur in March and September; a less pronounced peak appears in November. We also examine seasonal variation in the northward interplanetary magnetic field (IMF) over the same time period. The intensity and occurrence rate of the northward IMF exhibit patterns similar to that of the TPA incidence. Having studied IMF Bz before TPA onset, we find that strong and steady northward IMF conditions are favorable for TPA formation. We suggest that the semiannual variation observed in TPA incidence may be related to the Russell–McPherron (R-M) effect due to the projection effect of the IMF By under northward IMF conditions.

Update on the ESA-CAS Joint Solar Wind Magnetosphere Ionosphere Link Explorer (SMILE) Mission

The SMILE (Solar wind Magnetosphere Ionosphere Link Explorer) mission aims at deepening our understanding of the interaction of the solar wind with the Earth magnetosphere. It is the first time that ESA and CAS jointly select, design, implement, launch, and operate a space mission. The mission was adopted by CAS in November 2016 and by ESA in March 2019 with a target launch date by the end of 2023.

Progress and Prospects of the Strategic Priority Program on Space Science

In May 2018, the second phase of the Strategic Priority Program on Space Science (SPP II) was officially approved by the Chinese Academy of Sciences, in view of the significant scientific achievements of the first phase of the Strategic Priority Program on Space Science (SPP I) which includes 4 space science missions:the Dark Matter Particle Explorer (DAMPE), ShiJian-10 (SJ-10), Quantum Experiments at Space Scale (QUESS) and Hard X-ray Modulation Telescope (HXMT). Aiming to address fundamental scientific questions, SPP II focuses on two major themes:How the universe and life originate and evolve and What is the relationship between the solar system and human beings. In areas that Chinese scientists have advantages, new space science missions including Graviational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM), the Advanced space-based Solar Observatory (ASO-S), the Einstein Probe (EP), and Solar wind Magnetosphere Ionosphere Link Explorer (SMILE) have been approved in the framework of SPP II. This paper presents the research highlights of the SPP I, introduces the recent progress of SPP II, and puts forward the prospects for future development.

Geomagnetic effect of the Albanian earthquake on November 26, 2019

Background. The main cause of geomagnetic disturbances is known to be space sources, processes acting in the solar wind and in the interplanetary medium, as well as falling large celestial bodies. Earthquakes also give rise to geomagnetic effects. In accordance with the systems paradigm, the Earth–atmosphere–ionosphere–magnetosphere system comprises the single system where direct and reverse, positive and negative coupling take place. The mechanism of the earthquake effect on the magnetic field is poorly understood. A rock cracking, a fluctuating movement of fluids in pores, a corona discharge of the high-voltage static charge, etc., are thought to be the processes that give rise to the geomagnetic effect. In the course of earthquakes, seismic, acoustic, atmospheric gravity, and magnetohydrodynamic waves are generated, which provide for coupling between the subsystems in the Earth–atmosphere–ionosphere–magnetosphere system. Purpose of Work. The paper describes the possible response in the level of the geomagnetic field to the earthquake of 26 November 2019 that took place in Albania. Techniques and Methodology. The measurements were taken with the fluxmeter magnetometer at the V. N. Karazin Kharkiv National University Magnetometer Observatory. It delivers 0.5 – 500 pT sensistivity in the 1–1000 s period range over a quite large frequency band of 0.001 to 1 Hz. To study the quasi-periodic processes in detail, the systems spectral analysis of the temporal dependences of the horizontal (H, D) geomagnetic field components has been employed. It includes the short-time Fourier transform, the Fourier transform in a sliding window with a width adjusted to be equal to a fixed number of harmonic periods, and wavelet transform, simultaneously. The wavelet transform employs the Morlet wavelet as a basis function. Results. The quasi-periodic variations in the level of the geomagnetic field observed to appear with a 6 min lag and to last for 70–80 min could be due to the earthquake. These disturbances could be transferred by the magnetohydrodynamic waves. The quasi-periodic variations that were observed to appear with a 97–106 min lag and to last for about 130–140 min were most likely due to the earthquake. They were transferred by the atmospheric gravity waves with a period of 7–14 min. A relative disturbance in the electron density in the atmospheric gravity wave field was observed to be approximately 5.3%. The results obtained from observations of Albanian and Turkish earthquakes show agreement. Conclusions: The magnetic variations in the 1–1000 s period range that were observed to occur before and during the earthquake have been studied.

Design and implementation of electron diverters for lobster eye space-based X-ray optics.

Micropore optics have recently been implemented in a lobster eye geometry as a compact X-ray telescope. Fields generated by rare-earth magnets are used to reduce the flux of energetic electrons incident upon the focal plane detector in such a setup. We present the design and implementation of the electron diverters for X-ray telescopes of two upcoming missions: the microchannel X-ray telescope onboard the space-based multiband astronomical variable objects monitor and the soft X-ray instrument onboard the solar wind magnetosphere ionosphere link explorer. Electron diverters must be configured to conform to stringent limits on their total magnetic dipole moment and be compensated for any net moment arising from manufacturing errors. The two missions have differing designs, which are presented and evaluated in terms of the fractions of electrons reaching the detector, as determined by relativistic calculations of electron trajectories. The differential flux of electrons to the detector is calculated, and the integrated electron background is determined for both designs.

Physical Effects of the Lipetsk Meteoroid: 3

Comprehensive modeling studies of the processes induced in all geospheres by the passage and explosion of the meteoroid near the city of Lipetsk (Russia) on June 21, 2018, have been conducted. Magnetic, electric, electromagnetic, ionospheric, and seismic effects, as well as the effects of acoustic-gravity waves have been estimated. The magnetic effect of turbulence has been shown to be insignificant. The magnetic effect of the ionospheric currents and the current in the wake of the meteoroid could be substantial (~1 nT). Under the action of an external electric field, a transient current pulse with the strength of current up to 104 A could occur. The electrostatic effect could be accompanied by the accumulation of an electric charge of 1 mC producing the electric field intensity of 0.01–1 MV/m. The flow of the electric current in the wake of the meteoroid could result in the generation of an electromagnetic pulse in the 40–80 kHz band with the electric field intensity of 1–10 V/m. The electromagnetic effect of infrasound has been determined to be significant (1–10 V/m and 1–10 nT). The absorption of the shock wave at ionospheric dynamo region altitudes (100–150 km) could generate secondary atmospheric gravity waves with the 0.1–1 relative amplitude. The passage of the meteoroid acted to produce a plasma wake and noticeable disturbance not only in the lower but also in the upper atmosphere in the range of no less than 1000 km. The possibility of occurrence of the electrophonic effect, the generation of the ion and magnetic sound by infrasound, and the generation of gradient-drift and drift-dissipative instabilities are discussed. A conclusion is drawn that magnetic, electric, and electromagnetic effects dealt with in this paper significantly fill in the gaps in the theory of physical effects produced by meteoroids in the Earth–atmosphere–ionosphere–magnetosphere system. The magnitudes of magnetic, electric, electromagnetic, ionospheric, and acoustic effects were significant. The magnitude of the earthquake caused by the meteoroid explosion did not exceeded 1.7. The mean rate of the fall of celestial bodies similar to the Lipetsk meteoroid is equal to 0.68 yr–1.