Kinematics and Physics of Celestial Bodies最新文献

{"title":"Physical Parameters of Superhumps in Five Dwarf Nova Systems Based on TESS Observations","authors":"A. Dzygunenko,&nbsp;O. Baransky,&nbsp;V. Krushevska","doi":"10.3103/S0884591325050034","DOIUrl":"10.3103/S0884591325050034","url":null,"abstract":"<p>This study presents a detailed analysis of five cataclysmic variable systems of the dwarf nova class: Gaia21djh, Gaia19bwr, Gaia21akq, Gaia21enu, and Gaia18cjn. Using photometric data from the TESS space telescope and the ASAS-SN sky survey archive, the superhump periods (<i>P</i>_sh) and orbital periods (<i>P</i>_orb) for three SU UMa-type systems were determined. For Gaia21djh, <i>P</i>_sh = 0.08214 days and <i>P</i>_orb = 0.0786 days were obtained; similar values were determined for Gaia19bwr and Gaia21akq. For Gaia18cjn and Gaia21enu, the presence of stable superhumps was not confirmed, although Gaia18cjn shows an orbital period of <i>P</i>_orb = 0.189 days. The analysis of physical parameters, including mass ratios <i>q</i>, component masses <i>M</i>₁ and <i>M</i>₂ and radii <i>R</i>₁ and <i>R</i>₂ showed that all SU UMa systems have low <i>q</i> values (&lt;0.3) consistent with tidal instability. For example, Gaia21akq has <i>q</i> = 0.24 ± 0.03, which supports previous theoretical models. The study of superoutburst parameters revealed significant variability in the duration of different phases. Gaia19bwr exhibited the longest plateau phase duration (<i>D</i>_<i>P</i> = 9.6 ± 1.7 days), while it was <i>D</i>_<i>P</i> = 6.5 ± 0.6 days for Gaia21akq. The largest superoutburst amplitudes were observed in Gaia21djh (<i>A</i>_<i>SO</i> = 4.3 ± 0.2) and Gaia19bwr (4.2 ± 0.3). The obtained results are consistent with the thermal-tidal instability model for SU UMa-type systems and highlight the importance of high-precision photometric observations in studying accretion disk dynamics.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 5","pages":"187 - 196"},"PeriodicalIF":0.7,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145007934","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Seasonal Changes in the Activity Factor of Jupiter’s Hemispheres and Their Relationship with Solar Activity and Orbital Motion","authors":"A. P. Vidmachenko","doi":"10.3103/S0884591325050058","DOIUrl":"10.3103/S0884591325050058","url":null,"abstract":"<p>The authors analyze the long-term changes in the reflective properties of Jupiter’s atmosphere in order to study seasonal variations and the influence of solar activity. Jupiter has a very dynamic atmosphere consisting primarily of hydrogen and helium. Trace amounts of ammonia, methane, and other compounds form the visible cloud layers and haze above the clouds. The planet’s powerful magnetosphere plays an important role in the formation of the observed phenomena. The significant eccentricity of Jupiter’s orbit (<i>e</i> ≈ 0.0485) causes the solar energy input to the planet’s atmosphere to vary by 21% between perihelion and aphelion. The Northern Hemisphere receives significantly more energy because its summer solstice occurs during the planet’s passage through perihelion. This causes variations in the physical characteristics of the atmosphere and indicates the presence of seasonal changes. In order to quantify these changes, the brightness ratio of the northern and southern tropical and temperate regions <i>A</i>_J = <i>B</i>_N/<i>B</i>_S as a factor of photometric activity of atmospheric processes were used. Analysis of these data for the period 1960–2025 has revealed a clear periodicity in <i>A</i>_J changes with a period of approximately 11.87 years, which corresponds to Jupiter’s orbital period and indicates seasonal atmospheric restructuring processes. The effects of orbital eccentricity (a 21% variation in insolation) and solar activity (notably the 22-year Hale cycle and UV radiation) on Jupiter’s various atmospheric layers are analyzed. The characteristic radiative relaxation time of Jupiter’s atmosphere is found to be approximately 3.4 years (τ_R ≈ 1.07 × 10⁸ s) during intervals of coordinated orbital and solar forcings. A phase of imbalance from 1995 to 2012 and its subsequent recovery have been documented, accompanied by a decrease in the effective radiative constant to approximately 2.5 years (τ_R ≈ 0.79 × 10⁸ s), likely reflecting an enhanced influence of solar activity on the upper atmosphere.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 5","pages":"197 - 202"},"PeriodicalIF":0.7,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145007940","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Global Manifestations of a Unique Geospace Storm on May 10–13, 2024, in the F Region of the Ionosphere","authors":"L. F. Chernogor,&nbsp;V. O. Bessarabova","doi":"10.3103/S0884591325050022","DOIUrl":"10.3103/S0884591325050022","url":null,"abstract":"<p>Powerful transient processes on the Sun lead to solar storms and to geospace storms on Earth. Ionospheric storms are an integral part of geospace storms; they are extreme manifestations of ionospheric weather. Its variations have a significant impact on the functioning of civilization. It has been established that the manifestations of storms significantly depend not only on the characteristics of solar and geospace storms but also on the season, time of day, magnetic and geographical coordinates, etc. All this determines the relevance of studying each new ionospheric storm, especially when it comes to unique events. The purpose of this work is to study the features of the global manifestation of a unique geospace storm on May 10–13, 2024, in the F region of the ionosphere. The main features of the global manifestation of a unique geospace storm on May 10–13, 2024, in the F region of the ionosphere have been studied. The largest negative disturbances were observed on May 11, 2024, during the recovery phase of the geomagnetic storm. At most stations, the storm was strong or severe during the daytime. At night, manifestations of strong, severe, and extreme storms were mainly observed. The storm of May 13, 2024, was less intense compared to the storm of May 11, 2024. During the daytime, it was minor and moderate, while it was mainly strong and even severe at night. Negative and positive ionospheric storms sometimes replaced each other. Positive ionospheric storms were weaker. The duration of the blackout tended to decrease with decreasing geographical latitude of the station.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 5","pages":"209 - 220"},"PeriodicalIF":0.7,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145007939","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Observations of the Occultation of the Star TYC 1318-01031-1 by Asteroid (52) Europa on September 9, 2020","authors":"V. V. Kleshchonok,&nbsp;V. L. Karbovsky,&nbsp;V. I. Kashuba,&nbsp;O. V. Angelsky,&nbsp;M. V. Lashko","doi":"10.3103/S0884591325050046","DOIUrl":"10.3103/S0884591325050046","url":null,"abstract":"<p>This article presents the results of observations and data processing of the occultation of star TYC 1318-01031-1 by asteroid (52) Europa conducted at multiple sites. Data from both professional astronomers and experienced amateur observers are utilized. Professional observations have been conducted with an 80-cm diameter telescope equipped with a QHY174M GPS camera, which provides precise UTC time-stamping for each exposure via its integrated GPS receiver. Amateur observations have been carried out with various telescopes and cameras, with the data recorded in video format. The video recordings were processed using a unified methodology to derive the photometric occultation light curve. Ingress and egress times of the occultation at each observing site are determined from the extracted photometric light curves of TYC 1318-01031-1. A proprietary method is applied to combine occultation chords from geographically dispersed sites where observations have been acquired independently [1]. Subsequent processing employs the proposed combination method to compute each site’s offset from the occultation path centerline. Chords of asteroid (52) Europa for each observing site are then calculated from the measured ingress and egress times of the occultation. Calculated asteroid chords are compared to the 3D shape model of the asteroid from the Database of Asteroid Models from Inversion Techniques (DAMIT). This approach yields strong validation of the technique and demonstrates that amateur observations, taking into account potential UTC time-stamping errors, can be used to reconstruct asteroid shapes. The results also confirm that the shape and dimensions of asteroid (52) Europa in the DAMIT database are accurate.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 5","pages":"203 - 208"},"PeriodicalIF":0.7,"publicationDate":"2025-09-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145007938","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Black Hole Microstates and Entropy","authors":"S. K. Singh","doi":"10.3103/S088459132504004X","DOIUrl":"10.3103/S088459132504004X","url":null,"abstract":"<p>The black hole entropy problem, often framed through the semi-classical relation between horizon area and entropy, challenges the consistency of quantum gravity and thermodynamic principles. Within the framework of string theory, Fuzzball solutions offer a nontrivial resolution by positing that black holes are ensembles of horizonless microstates, whose degeneracy matches the leading-order entropy scaling predicted by <i>S</i> ~ <i>A</i>. This paper conducts a comparative analysis of Fuzzball microstate geometries against other competing proposals, such as holographic dualities, where <i>S</i>_CFT asymptotically approaches black hole entropy and approaches derived from loop quantum gravity, which quantize spacetime at the Planck scale. Recent advancements in the moduli space of supersymmetric and near-extremal Fuzzball solutions have pushed forward our understanding of microstate counting, though extending these solutions to nonextremal configurations remains a formidable challenge. Moreover, the emergence of Hawking radiation as a coherent quantum process, while preserving unitarity, raises new questions about the completeness of the Fuzzball paradigm in resolving the information paradox. In this work, we explore the complex interplay between gravitational entropy, quantum information, and the non-local structure of spacetime, ultimately confronting the limitations and future directions of Fuzzball theory in addressing the full range of gravitational entropy phenomena.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 4","pages":"176 - 185"},"PeriodicalIF":0.7,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145143971","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Impact of Electrical Storms of Magnetospheric-Ionospheric Origin on Geosphere Interactions","authors":"L. F. Chernogor","doi":"10.3103/S0884591325040026","DOIUrl":"10.3103/S0884591325040026","url":null,"abstract":"<p>The quantitative analysis of processes in the subsystems electric field–ionospheric current–atmosphere–ionosphere and electric field–atmosphere–lithosphere, triggered by powerful geomagnetic storms, is a relevant task. The study aims to assess the impact of the electrical storms of magnetospheric-ionospheric origin on the interaction between the external and internal geospheres. The study quantitatively evaluates the role of such electrical storms in the interaction between the external and internal geospheres within the SIMMIAE system. Due to the dissipation of ionospheric current under the action of the electric field, the atmospheric temperature at altitudes of 120–350 km increases by tens to hundreds of Kelvins during the day and by units to hundreds of Kelvins during the night. It has been shown that the heated atmospheric gas rises with a speed varying from tens to hundreds of meters per second depending on altitude. The characteristic time for the ascent of heated atmospheric gas decreases with altitude, from approximately 10 to 4 min during the day and from 40 to 8–9 min during the night. The heat flux density is maximal at an altitude of around 150 km, reaching 20 mW/m² during the day and 0.1–0.2 mW/m² during the night. The maximum power of Joule heating in the atmosphere is 200 GW during the day and 1–2 GW during the night. The quantity of Joule heat in the atmosphere reaches 200 TJ during the day and 5–6 TJ during the night. An electrical storm of magnetospheric-ionospheric origin also induces an electrical storm in the lithosphere. In this case, the electric field strength in the lithosphere can reach approximately 10–100 µV/m, the power of Joule heating ranges from 1 to 1000 MW, and the energy spans 1–40 000 GJ. Joule heating of the atmosphere and lithosphere acts as a triggering process in response to the electric field. The triggering coefficient ranges from 10¹⁰ to 10¹¹ for the thermosphere and from 10¹² to 10¹³ for the lithosphere. Seven-point scales for classifying electrical storms in the atmosphere and lithosphere are proposed.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 4","pages":"151 - 160"},"PeriodicalIF":0.7,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145143969","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Determination of Light Curve Parameters of Poorly Studied Eclipsing Variables Using Data from TESS and Other Sky Surveys","authors":"V. I. Marsakova,&nbsp;I. L. Andronov,&nbsp;V. O. Borshchenko,&nbsp;I. A. Garbazhii-Romanchenko,&nbsp;A. D. Lashkova,&nbsp;S. A. Kreminska,&nbsp;P. A. Dubovsky,&nbsp;V. V. Dubovskyi","doi":"10.3103/S0884591325040038","DOIUrl":"10.3103/S0884591325040038","url":null,"abstract":"<p>A group of poorly studied eclipsing variables (the classification of which is marked as uncertain and/or the period of brightness changes is uncertain) has been studied with the using of the photometric observations of the TESS mission and NSVS, ASAS-SN sky-surveys. We also obtained some observations covering the brightness minima of our variables by our group using the telescopes at Astronomical Observatory on Kolonica Saddle (Slovakia) and Observatory and Planetarium in Hlohovec (Slovakia) during the “Variable-2024” astrocamp. The periods and classification were corrected. For NSV 575 and NSV 014 the periods were found for the first time, but it is doubtful that NSV 014 is an eclipsing variable, because there are no eclipses but the asymmetric wave is present, which indicates that the variable star can be re-classified as a low-amplitude pulsating one. Different methods were used for approximation of the light curves and further calculation of stellar system’s parameters such as eclipse depths and durations, values of reflection effect and effect of ellipticity of stars. The initial period was estimated using the periodogram based on the trigonometrical polynomial fit of high order (up to 10). For better approximation of the complete eclipsing phase curve, the “New Algol Variable” (NAV) software was used. The methods of “asymptotic parabolas” and “wall-supported asymptotic parabolas” were used for calculation of moments of eclipses, which use only near-eclipse part of the observations instead of a complete curve. These methods were implemented in the software MAVKA among a larger set of features. For the variables NSV 489 and NSV 1884, our moments of eclipses and the ones found in the literature, were used for the <i>O</i>–<i>C</i> curves. For NSV 489, the period was adjusted taking into account the slope of the (<i>O</i>–<i>C</i>) diagram.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 4","pages":"161 - 168"},"PeriodicalIF":0.7,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145143924","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Effect of the Kinetic Temperature of Plasma Electrons on Dispersion and Rotation Measures","authors":"O. M. Ulyanov,&nbsp;C. Tiburzi,&nbsp;A. I. Shevtsova,&nbsp;V. V. Zakharenko,&nbsp;A. O. Konovalenko,&nbsp;P. Zarka,&nbsp;J.-M. Grieβmeier,&nbsp;M. V. Skoryk,&nbsp;A. O. Skoryk,&nbsp;S. M. Yerin,&nbsp;I. P. Kravtsov,&nbsp;A. I. Brazhenko,&nbsp;A. V. Frantsuzenko,&nbsp;I. M. Bubnov","doi":"10.3103/S0884591325040051","DOIUrl":"10.3103/S0884591325040051","url":null,"abstract":"<p>The aim of this work is to analyze the impact of the kinetic temperature of electrons in a warm anisotropic plasma and the strength of its magnetic field on the integral characteristics of pulsar pulsed radio emission propagation, such as the dispersion measure (DM) and rotation measure (RM). An important aspect in this context is the presence of magnetic fields in the plasma, their strength, and their configuration relative to the line of sight. The approach uniquely accounts for polarization splitting into ordinary and extraordinary waves in pulsar pulsed radio emission and considers the limiting cases of quasi-longitudinal and quasi-transverse propagation of these waves in a medium with magnetic fields of various strengths, with or without scattering. This makes it possible to predict a possible dependence of the DM and RM on frequency (not previously anticipated), magnetic field strength, and electron kinetic temperature as well as the amplification of this dependence with increasing magnetic field strength. Notably, the frequency dependence of the DM and RM is more pronounced at low frequencies, with both measures increasing as frequency decreases. Accounting for these dependences when analyzing DM and RM toward different pulsars makes it possible to estimate cosmic magnetoactive plasma parameters, including the range of electron kinetic temperatures and the strengths of longitudinal and transverse magnetic field components along the path of polarized radiation propagation. Thus, using pulsar pulses as probing radio emission makes it possible to study warm magnetoactive plasma with magnetic field strengths of the order of 1–10 G or higher, such as the solar corona, the Jupiter–Io flux tube, and the Earth’s ionosphere.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 4","pages":"169 - 175"},"PeriodicalIF":0.7,"publicationDate":"2025-07-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"145143970","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Photometric Parameters of the Canon EOS 6D Mark II Camera","authors":"V. O. Psaryov,&nbsp;Yu. I. Velikodsky,&nbsp;V. V. Konichek,&nbsp;I. E. Sinelnikov","doi":"10.3103/S0884591325030043","DOIUrl":"10.3103/S0884591325030043","url":null,"abstract":"<p>The paper presents metrological parameters of the full-frame camera Canon EOS 6D Mark II’s photosensor. The working range of output signal levels is from 0.1 to 15 870 reference units DN. Depending on ISO parameter value, the sensor solarization takes place when the output signal reaches levels from 11 318 up to 15 870 DN. According to the data of laboratory experiments, it is shown that the range of the photosensor output signal in the area of its linear response to changes in the active light flux is 20.2–20.4 dB (Δ<i>S</i> is 107.3–11 595.6, 142.0–14 819.9, and 132.2–14 309.0 DN in R, G, and B channels of the sensor, respectively.) When using the logarithmic function of photosensor sensitivity, the range of its linear response increases to 38.2 dB (Δ<i>S</i> = 2.24–14 819.9 DN). The sensor’s local response in the R, G, and B channels to changes in active light flux is 558.63, 1164.0, and 691.37 DN/s at ISO 100; 1283.5, 955.29, and 206.9 DN/s at ISO 12 800; and 4263.6, 3119.2, 698.42 DN/s at ISO 40 000, respectively. The dependence of the sensor output signal level on the ISO value at an exposure time of <i>T</i>_exp = 5.2 s remains linear within the entire range of ISO values from ISO 100 to ISO 102 400 in all spectral channels of the sensor when using a logarithmic dependence log Se(log ISO). In the case when the sensor transfer function is presented on natural numbers scale, the sensor linear response ranges in R, G, and B spectral channels differ and are ΔISO_R,G,B = 1600–102 400, 2016–102 400, 3200–102 400 DN, respectively. In the highest informativeness areas of the linear sensor response ranges, the signal-to-noise ratio (SNR) of the output signal takes values from 5.0 dB to 34.5 dB (Rose’s criterion); accordingly, the signal increases from 4.5 to 12 560 DN and is controlled by the ISO level. Similarly, when the signal intensity depends on exposure duration, at ISO 100 within the sensor linear response ranges, the critical SNR values of output signals are 5.0 dB at <i>S</i>_av = 14.0 DN and 47.6 dB at <i>S</i>_av = 14 820 DN. At ISO 40 000, the SNR parameter takes values from 5.0 dB to 33.6 dB at signal levels of 160–230 and 13 522 DN, respectively. Taking into account the results of conducted analysis, the use of digital cameras with a CMOS sensor in photometric studies can be considered acceptable.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 3","pages":"125 - 149"},"PeriodicalIF":0.5,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143938648","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Energetics of the Geospace Storm of April 23–24, 2023: from Solar Storm to Lithospheric Disturbance","authors":"L. F. Chernogor","doi":"10.3103/S088459132503002X","DOIUrl":"10.3103/S088459132503002X","url":null,"abstract":"<p>The aim of the paper is to assess the energy parameters of physical processes starting from the solar storm of April 21, 2023, and ending with the perturbations of the Earth’s lithosphere on April 23–24, 2023. The energy of processes in all subsystems of the Sun–interplanetary medium–magnetosphere–ionosphere–atmosphere–lithosphere system is analyzed. A comparative analysis of this storm with an extreme storm is performed. The storm of April 23–24, 2023, was unique due to the shift of the auroral zone to the midlatitudes to 50°. The international auroral brightness scale is improved. The auroral energy scale is proposed.</p>","PeriodicalId":681,"journal":{"name":"Kinematics and Physics of Celestial Bodies","volume":"41 3","pages":"97 - 107"},"PeriodicalIF":0.5,"publicationDate":"2025-05-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"143938649","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":4,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}