Pub Date : 2024-04-15DOI: 10.1134/s0010952523600336
J. A. Antonov, V. I. Zakharov, I. N. Myagkova, N. A. Suhareva, J. S. Shugai
Abstract
The paper applies the methods of information theory to the study of the interplanetary magnetic field and its variations as a result of solar activity. The statistical regularities of the projections of the vectors of the interplanetary magnetic field and the speed of the flow of solar wind particles do not carry information about the order of realization for the available states of the studied physical system. At the same time, such characteristics can be obtained from phase diagrams or phase portraits created on the basis of experimental samples in subspaces of the phase space, which display both the values of vector quantities and the sequence order in a particular time series. The paper proposes a method for synthesizing vector graphs in the phase subspace of the interplanetary magnetic field (IMF). Results are considered of the reconstruction and analysis of implemented graphs based on the time series of satellite monitoring of the state of the IMF, provided by the database of the NASA Goddard Space Flight Center since the beginning of 2023. The graph is constructed on the basis of experimental samples for projections of magnetic field vectors. Field vectors converge and diverge at the nodes of the graph, the edges of the graph allow one to control the analyzed trajectory of the system in the phase subspace and restore the transition tree for a particular vector field. The concept of a spherical reference surface of a vector graph is introduced, which allows one to bring the compared implementations of graphs to a single linear scale and a single curvature of the reference surface. Examples are considered under the action of various external factors associated with the solar magnetic field and coronal mass ejections.
{"title":"Structure and Dynamics for Graphs of Interplanetary Magnetic Field Vectors","authors":"J. A. Antonov, V. I. Zakharov, I. N. Myagkova, N. A. Suhareva, J. S. Shugai","doi":"10.1134/s0010952523600336","DOIUrl":"https://doi.org/10.1134/s0010952523600336","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The paper applies the methods of information theory to the study of the interplanetary magnetic field and its variations as a result of solar activity. The statistical regularities of the projections of the vectors of the interplanetary magnetic field and the speed of the flow of solar wind particles do not carry information about the order of realization for the available states of the studied physical system. At the same time, such characteristics can be obtained from phase diagrams or phase portraits created on the basis of experimental samples in subspaces of the phase space, which display both the values of vector quantities and the sequence order in a particular time series. The paper proposes a method for synthesizing vector graphs in the phase subspace of the interplanetary magnetic field (IMF). Results are considered of the reconstruction and analysis of implemented graphs based on the time series of satellite monitoring of the state of the IMF, provided by the database of the NASA Goddard Space Flight Center since the beginning of 2023. The graph is constructed on the basis of experimental samples for projections of magnetic field vectors. Field vectors converge and diverge at the nodes of the graph, the edges of the graph allow one to control the analyzed trajectory of the system in the phase subspace and restore the transition tree for a particular vector field. The concept of a spherical reference surface of a vector graph is introduced, which allows one to bring the compared implementations of graphs to a single linear scale and a single curvature of the reference surface. Examples are considered under the action of various external factors associated with the solar magnetic field and coronal mass ejections.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"12 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140613218","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}
Pub Date : 2024-04-15DOI: 10.1134/s0010952523600300
A. B. Struminsky, A. M. Sadovskii, I. Yu. Grigorieva
Abstract
From the beginning of January 2021 to the end of August 2023, the radiation monitor of the Spektr-RG spacecraft registered three enhancements in the count rate, which exceed the background variations during the solar activity cycle and have a comparable maximum value. These enhancements are associated with solar proton events (SPEs) from the flares X1.0 on October 28, 2021; M6.3 on February 25, 2023; and M5.7 on July 17, 2023. Using the example of these events, as well as smaller SPEs from the flares M3.7 on February 24, 2023, and M4.0 on July 16, 2023, threshold criteria for “proton” flares are discussed. In powerful SPEs, the contribution of solar protons to the radiation dose can exceed the total contribution of galactic cosmic rays (GCR) over a sufficiently long period of time. Therefore, such SPEs are sources of increased radiation hazard and require prediction based on real-time observations. It was shown that, in these five flares, thresholds were overcome according to three criteria: plasma temperature >12 MK (soft X-ray source), duration (>5 min) of microwave or hard X-ray (HXR) radiation (electron acceleration >100 keV), and height of flare development process >60 Mm (radio emission at plasma frequencies <610 MHz). The arrival of the first solar protons >100 MeV to the Earth’s orbit was expected no earlier than 10 min relative to the beginning of HXR or microwave radiation, i.e., could have been predicted in advance. To study the relationship between solar flares and SPEs, we used data from the anticoincidence shield of the spectrometer on INTEGRAL (ACS SPI), which is an effective but uncalibrated detector of HXR >100 keV and protons >100 MeV, as well as patrol observations of radio emission at fixed frequencies (Radio Solar Telescope Network). It is noted that the X2.2 (N25E64) flare on February 17, 2023 satisfied all three “protonity” criteria and could become the source of a powerful SPE near the Earth in a case of favorable location on the Sun. In the M8.6 (N27W29) flare on February 28, 2023, the third criterion was not met, and it did not lead to an SPE as expected (it developed in a plasma with a density >2.5 × 1010 cm–3 and plasma frequency >1415 MHz).
{"title":"Sources of Solar Protons in the Events of February 24–25 and July 16–17, 2023","authors":"A. B. Struminsky, A. M. Sadovskii, I. Yu. Grigorieva","doi":"10.1134/s0010952523600300","DOIUrl":"https://doi.org/10.1134/s0010952523600300","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>From the beginning of January 2021 to the end of August 2023, the radiation monitor of the <i>Spektr-RG</i> spacecraft registered three enhancements in the count rate, which exceed the background variations during the solar activity cycle and have a comparable maximum value. These enhancements are associated with solar proton events (SPEs) from the flares X1.0 on October 28, 2021; M6.3 on February 25, 2023; and M5.7 on July 17, 2023. Using the example of these events, as well as smaller SPEs from the flares M3.7 on February 24, 2023, and M4.0 on July 16, 2023, threshold criteria for “proton” flares are discussed. In powerful SPEs, the contribution of solar protons to the radiation dose can exceed the total contribution of galactic cosmic rays (GCR) over a sufficiently long period of time. Therefore, such SPEs are sources of increased radiation hazard and require prediction based on real-time observations. It was shown that, in these five flares, thresholds were overcome according to three criteria: plasma temperature >12 MK (soft X-ray source), duration (>5 min) of microwave or hard X-ray (HXR) radiation (electron acceleration >100 keV), and height of flare development process >60 Mm (radio emission at plasma frequencies <610 MHz). The arrival of the first solar protons >100 MeV to the Earth’s orbit was expected no earlier than 10 min relative to the beginning of HXR or microwave radiation, i.e., could have been predicted in advance. To study the relationship between solar flares and SPEs, we used data from the anticoincidence shield of the spectrometer on <i>INTEGRAL</i> (ACS SPI), which is an effective but uncalibrated detector of HXR >100 keV and protons >100 MeV, as well as patrol observations of radio emission at fixed frequencies (Radio Solar Telescope Network). It is noted that the X2.2 (N25E64) flare on February 17, 2023 satisfied all three “protonity” criteria and could become the source of a powerful SPE near the Earth in a case of favorable location on the Sun. In the M8.6 (N27W29) flare on February 28, 2023, the third criterion was not met, and it did not lead to an SPE as expected (it developed in a plasma with a density >2.5 × 10<sup>10</sup> cm<sup>–3</sup> and plasma frequency >1415 MHz).</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"48 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140613689","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}
Pub Date : 2024-04-15DOI: 10.1134/s0010952523600324
A. S. Lavrukhin, I. I. Alexeev, E. S. Belenkaya, V. V. Kalegaev, I. S. Nazarkov, D. V. Nevsky
Abstract
We discuss the reasons for the extreme compression of the magnetosphere during the storm on February 27, 2023, when the magnetopause crossed the geostationary orbit. At the same time, aurora was observed at middle latitudes. The global parameters of magnetospheric current systems were calculated from data on the parameters of the interplanetary medium and geomagnetic indices characterizing the evolution of the ring current and the westward auroral electrojet, using a paraboloid model of the magnetosphere. We have calculated the contributions of various current systems to the observed value of the ({{D}_{{st}}}) index. The contribution of the tail current sheet is comparable with the contribution of the ring current for this storm. The calculated modelled field is compared with the data of the GOES-16, 18 magnetometers; the results are in good agreement with observations.
{"title":"Magnetosphere and Auroral Oval Dynamics during February 27, 2023 Magnetic Storm","authors":"A. S. Lavrukhin, I. I. Alexeev, E. S. Belenkaya, V. V. Kalegaev, I. S. Nazarkov, D. V. Nevsky","doi":"10.1134/s0010952523600324","DOIUrl":"https://doi.org/10.1134/s0010952523600324","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>We discuss the reasons for the extreme compression of the magnetosphere during the storm on February 27, 2023, when the magnetopause crossed the geostationary orbit. At the same time, aurora was observed at middle latitudes. The global parameters of magnetospheric current systems were calculated from data on the parameters of the interplanetary medium and geomagnetic indices characterizing the evolution of the ring current and the westward auroral electrojet, using a paraboloid model of the magnetosphere. We have calculated the contributions of various current systems to the observed value of the <span>({{D}_{{st}}})</span> index. The contribution of the tail current sheet is comparable with the contribution of the ring current for this storm. The calculated modelled field is compared with the data of the GOES-16, 18 magnetometers; the results are in good agreement with observations.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"10 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140617568","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}
Pub Date : 2024-04-15DOI: 10.1134/s001095252360035x
A. V. Dmitriev
Abstract
Geosynchronous magnetopause crossings (GMCs) were analyzed during geomagnetic storms on February 26, March 23, and April 23, 2023. GMC-associated magnetosheath intervals were identified using magnetic data acquired from the GOES-16 and GOES-17 spacecraft. A comparative analysis of various magnetopause models was performed on the base of solar wind conditions measured by the THEMIS-E spacecraft and the Wind interplanetary monitor. The analysis of models was based on statistical parameters for determining magnetosheath intervals. It was shown that for all three storms, the model presented in [1] demonstrated the best accuracy. For events of moderate magnetic storms against the background of small negative Bz component of the interplanetary magnetic field (IMF), good results are obtained with the model described in [2]. For extreme events with very high solar wind pressures and/or very strong negative IMF Bz, the model shown in [3] exhibits good accuracy, and satisfactory accuracy is also demonstrated by models presented in [4, 5]. It was shown that the accuracy of the models was affected by the following factors and effects: the choice of interplanetary monitor, the dependence of the model on the solar wind pressure, the Bz saturation effect, the dawn–dusk magnetopause asymmetry, and the effect of prehistory.
{"title":"Geosynchronous Magnetopause Crossings in February–April 2023","authors":"A. V. Dmitriev","doi":"10.1134/s001095252360035x","DOIUrl":"https://doi.org/10.1134/s001095252360035x","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Geosynchronous magnetopause crossings (GMCs) were analyzed during geomagnetic storms on February 26, March 23, and April 23, 2023. GMC-associated magnetosheath intervals were identified using magnetic data acquired from the <i>GOES-16</i> and <i>GOES-17</i> spacecraft. A comparative analysis of various magnetopause models was performed on the base of solar wind conditions measured by the <i>THEMIS-E</i> spacecraft and the <i>Wind</i> interplanetary monitor. The analysis of models was based on statistical parameters for determining magnetosheath intervals. It was shown that for all three storms, the model presented in [1] demonstrated the best accuracy. For events of moderate magnetic storms against the background of small negative <i>Bz</i> component of the interplanetary magnetic field (IMF), good results are obtained with the model described in [2]. For extreme events with very high solar wind pressures and/or very strong negative IMF <i>Bz</i>, the model shown in [3] exhibits good accuracy, and satisfactory accuracy is also demonstrated by models presented in [4, 5]. It was shown that the accuracy of the models was affected by the following factors and effects: the choice of interplanetary monitor, the dependence of the model on the solar wind pressure, the <i>Bz</i> saturation effect, the dawn–dusk magnetopause asymmetry, and the effect of prehistory.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"47 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140613137","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}
Pub Date : 2024-04-15DOI: 10.1134/s0010952523600312
S. A. Starodubtsev, P. Yu. Gololobov, V. G. Grigoryev, A. S. Zverev
Abstract
A study of MHD waves in solar wind plasma during two geoeffective space weather events in February–March 2023 is reported. At that time, various geophysical phenomena were observed on Earth: intense magnetic storms, decreases in the intensity of galactic cosmic rays, auroras, and a number of other manifestations of space weather. To study the situation in near-Earth outer space, we used data from direct measurements of the parameters of the interplanetary medium with the DSCOVR and ACE spacecraft. The application of spectral analysis methods to the data of direct measurements of the solar wind parameters onboard the DSCOVR spacecraft made it possible to study the characteristics and dynamics of Alfén, fast, and slow magnetosonic waves in the inertial frequency range (from ∼0.0001 to ∼0.01 Hz) of the observed solar wind turbulence spectrum during these events.
{"title":"MHD Waves in Solar Wind Plasma during Geomagnetic Storm Events in February–March 2023","authors":"S. A. Starodubtsev, P. Yu. Gololobov, V. G. Grigoryev, A. S. Zverev","doi":"10.1134/s0010952523600312","DOIUrl":"https://doi.org/10.1134/s0010952523600312","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>A study of MHD waves in solar wind plasma during two geoeffective space weather events in February–March 2023 is reported. At that time, various geophysical phenomena were observed on Earth: intense magnetic storms, decreases in the intensity of galactic cosmic rays, auroras, and a number of other manifestations of space weather. To study the situation in near-Earth outer space, we used data from direct measurements of the parameters of the interplanetary medium with the <i>DSCOVR</i> and <i>ACE</i> spacecraft. The application of spectral analysis methods to the data of direct measurements of the solar wind parameters onboard the <i>DSCOVR</i> spacecraft made it possible to study the characteristics and dynamics of Alfén, fast, and slow magnetosonic waves in the inertial frequency range (from ∼0.0001 to ∼0.01 Hz) of the observed solar wind turbulence spectrum during these events.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"15 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-04-15","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140613179","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}
Pub Date : 2024-03-08DOI: 10.1134/s0010952523700776
U. V. Monakhova, S. A. Shestakov, Ya. V. Mashtakov, D. S. Ivanov
Abstract
Control of the motion of a swarm of small satellites after a cluster launch is proposed to keep the satellites trajectories in a given area and provide intersatellite communications. The goal of the motion control algorithm is to eliminate the average drift parameter and achieve the required relative trajectory shift in the along-track direction. An analytical study of the proposed motion algorithm is carried out using a linear model of relative motion. The verification of analytical results is performed by swarm motion numerical simulation.
{"title":"Decentralized Swarm Control of Small Satellites for Communication Connectivity Maintenance","authors":"U. V. Monakhova, S. A. Shestakov, Ya. V. Mashtakov, D. S. Ivanov","doi":"10.1134/s0010952523700776","DOIUrl":"https://doi.org/10.1134/s0010952523700776","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Control of the motion of a swarm of small satellites after a cluster launch is proposed to keep the satellites trajectories in a given area and provide intersatellite communications. The goal of the motion control algorithm is to eliminate the average drift parameter and achieve the required relative trajectory shift in the along-track direction. An analytical study of the proposed motion algorithm is carried out using a linear model of relative motion. The verification of analytical results is performed by swarm motion numerical simulation.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"27 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140071364","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}
Pub Date : 2024-03-08DOI: 10.1134/s001095252370079x
L. S. Novikov, A. A. Makletsov, V. V. Sinolits, N. P. Chirskaya
Abstract
The Coulomb software complex for modeling of spacecraft charging in magnetosphere plasma in high and low Earth orbits is described. Physical mechanisms of spacecraft charging and methods of mathematical modeling of this phenomenon in various areas of space are considered. Examples of the calculation results of electrical potential distribution on the spacecraft surface and in the vicinity of the spacecraft in geosynchronous and the low Earth orbits are presented.
{"title":"Mathematical Modeling of Spacecraft in Magnetosphere Plasma","authors":"L. S. Novikov, A. A. Makletsov, V. V. Sinolits, N. P. Chirskaya","doi":"10.1134/s001095252370079x","DOIUrl":"https://doi.org/10.1134/s001095252370079x","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The Coulomb software complex for modeling of spacecraft charging in magnetosphere plasma in high and low Earth orbits is described. Physical mechanisms of spacecraft charging and methods of mathematical modeling of this phenomenon in various areas of space are considered. Examples of the calculation results of electrical potential distribution on the spacecraft surface and in the vicinity of the spacecraft in geosynchronous and the low Earth orbits are presented.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"25 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140071363","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}
Pub Date : 2024-03-08DOI: 10.1134/s001095252370082x
L. V. Ksanfomality
Abstract
Venus was the first of the planets of the Solar System in the atmosphere of which electrical phenomena similar to lightning in the Earth’s atmosphere were discovered. Electrical discharges (lightning in the atmosphere of Venus) were discovered in 1978 in the Venera-12, -11, and Pioneer Venus missions, based on their electromagnetic radiation. The paradox, however, was that the search for optical flares remained unsuccessful for the past 40 years. In 2015, the Akatsuki spacecraft of the Japan Aerospace Exploration Agency was launched into orbit Venus satellite. It was designed to search for lightning and other studies of the meteorology of Venus by recording radiation in selected spectral ranges. In 2016, the Akatsuki orbiter successfully performed detailed observations of Venus in the near-infrared range in the “transparency windows” of the planet’s atmosphere, as well as in the ultraviolet and other ranges. The article presents the results of an alternative search for and successful detection of lightning flashes according to the Akatsuki project, but not in the ultraviolet or visible ranges, but in the near-IR range. A comparison of the results of calculations based on models of terrestrial lightning with the results of measurements made by the IR2 camera of the Akatsuki mission on Venus at a wavelength of 2.26 μm shows a close agreement between the experimental and calculated data.
{"title":"Lightning Flares in the Cloud Layer of Venus Detected in the Near-Infrared Range","authors":"L. V. Ksanfomality","doi":"10.1134/s001095252370082x","DOIUrl":"https://doi.org/10.1134/s001095252370082x","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Venus was the first of the planets of the Solar System in the atmosphere of which electrical phenomena similar to lightning in the Earth’s atmosphere were discovered. Electrical discharges (lightning in the atmosphere of Venus) were discovered in 1978 in the <i>Venera-12</i>, <i>-11</i>, and <i>Pioneer Venus</i> missions, based on their electromagnetic radiation. The paradox, however, was that the search for optical flares remained unsuccessful for the past 40 years. In 2015, the <i>Akatsuki</i> spacecraft of the Japan Aerospace Exploration Agency was launched into orbit Venus satellite. It was designed to search for lightning and other studies of the meteorology of Venus by recording radiation in selected spectral ranges. In 2016, the <i>Akatsuki</i> orbiter successfully performed detailed observations of Venus in the near-infrared range in the “transparency windows” of the planet’s atmosphere, as well as in the ultraviolet and other ranges. The article presents the results of an alternative search for and successful detection of lightning flashes according to the <i>Akatsuki</i> project, but not in the ultraviolet or visible ranges, but in the near-IR range. A comparison of the results of calculations based on models of terrestrial lightning with the results of measurements made by the IR2 camera of the <i>Akatsuki</i> mission on Venus at a wavelength of 2.26 μm shows a close agreement between the experimental and calculated data.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"5 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140071528","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}
Pub Date : 2024-03-08DOI: 10.1134/s0010952523700855
O. V. Antonenko, A. S. Kirillov
Abstract
Experimental data on the characteristic concentrations of atomic oxygen in the upper atmospheres of the Earth and Mars are considered in the paper. The values of the integrated intensities of Herzberg I bands for the middle latitudes and the equatorial zone of the Earth are calculated, as well as for the northern latitudes and the equatorial zone of Mars. The correlation of theoretically calculated results for the emission intensities of the bands of electronically excited molecular oxygen in the Earth’s atmosphere in the spectral range of 250–370 nm and of experimental data on the glow of molecular oxygen obtained from the Discovery cosmic shuttle (STS-53) is discussed. The calculated values of the column integrated intensities of the Herzberg I band system in the Earth’s atmosphere for various seasons and for points of the equinox of Mars are presented. It is shown that at the middle latitudes of the Earth during the period of low solar activity, the maximum values of integral intensities are typical for July, but in the equatorial zone they are typical for April. In the northern latitudes of Mars, the maximum values occur at the moment of the autumn equinox.
摘要 本文研究了地球和火星高层大气中原子氧特征浓度的实验数据。计算了地球中纬度和赤道区以及火星北纬度和赤道区赫茨伯格 I 波段的综合强度值。讨论了地球大气中电子激发的分子氧在 250-370 纳米光谱范围内的波段发射强度的理论计算结果与发现号宇宙飞船（STS-53）获得的分子氧辉光实验数据的相关性。介绍了地球大气中赫兹伯格 I 波段系统在不同季节和火星春分点的柱积分强度计算值。结果表明，在太阳活动较少的时期，地球中纬度地区积分强度的最大值一般出现在七月，而在赤道地区则一般出现在四月。在火星北纬，最大值出现在秋分时刻。
{"title":"An Investigation of the Influence of Seasonal and Latitudinal Variations of Atomic Oxygen on the Intensity of Self-Emission of the Night Atmospheres of the Earth and Mars","authors":"O. V. Antonenko, A. S. Kirillov","doi":"10.1134/s0010952523700855","DOIUrl":"https://doi.org/10.1134/s0010952523700855","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Experimental data on the characteristic concentrations of atomic oxygen in the upper atmospheres of the Earth and Mars are considered in the paper. The values of the integrated intensities of Herzberg I bands for the middle latitudes and the equatorial zone of the Earth are calculated, as well as for the northern latitudes and the equatorial zone of Mars. The correlation of theoretically calculated results for the emission intensities of the bands of electronically excited molecular oxygen in the Earth’s atmosphere in the spectral range of 250–370 nm and of experimental data on the glow of molecular oxygen obtained from the Discovery cosmic shuttle (STS-53) is discussed. The calculated values of the column integrated intensities of the Herzberg I band system in the Earth’s atmosphere for various seasons and for points of the equinox of Mars are presented. It is shown that at the middle latitudes of the Earth during the period of low solar activity, the maximum values of integral intensities are typical for July, but in the equatorial zone they are typical for April. In the northern latitudes of Mars, the maximum values occur at the moment of the autumn equinox.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"21 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140076419","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}
Pub Date : 2024-03-08DOI: 10.1134/s0010952523700740
I. N. Abezyaev
Abstract
The developed spatial (3D) orbital gyrocompass allows performing all the necessary functions of angular orientation of a spacecraft relative to the orbital coordinate system. In this regard, it is no different from the astronavigation system (ANS), except for the use of different types of external information sensors. In the first case, it is the Earth orientation device; in the second case, it is the star sensor. Each system has its advantages and disadvantages. The advantage of the ANS is higher orientation accuracy. The undeniable advantage of the 3D gyrocompass is the ability to control the orientation of the spacecraft for an extended period without using ballistic data. The sufficiently high functionality of the 3D gyrocompass makes the orientation system built on its basis quite competitive with astronavigation-based orientation systems. Thus, the task of studying the properties and improving the accuracy characteristics of the device becomes relevant.
{"title":"Spatial Orbital Gyrocompass. Questions of Theory and Application","authors":"I. N. Abezyaev","doi":"10.1134/s0010952523700740","DOIUrl":"https://doi.org/10.1134/s0010952523700740","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The developed spatial (3D) orbital gyrocompass allows performing all the necessary functions of angular orientation of a spacecraft relative to the orbital coordinate system. In this regard, it is no different from the astronavigation system (ANS), except for the use of different types of external information sensors. In the first case, it is the Earth orientation device; in the second case, it is the star sensor. Each system has its advantages and disadvantages. The advantage of the ANS is higher orientation accuracy. The undeniable advantage of the 3D gyrocompass is the ability to control the orientation of the spacecraft for an extended period without using ballistic data. The sufficiently high functionality of the 3D gyrocompass makes the orientation system built on its basis quite competitive with astronavigation-based orientation systems. Thus, the task of studying the properties and improving the accuracy characteristics of the device becomes relevant.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"53 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-03-08","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140071819","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}
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