Pub Date : 2024-06-17DOI: 10.1134/s0010952524600379
S. Sharakin, D. Barghini, M. Battisti, A. Belov, M. Bertaina, M. Bianciotto, F. Bisconti, C. Blaksley, S. Blin, G. Cambiè, F. Capel, M. Casolino, T. Ebisuzaki, J. Eser, F. Fenu, M. A. Franceschi, A. Golzio, P. Gorodetsky, F. Kajino, H. Kasuga, P. Klimov, M. Manfrin, L. Marcelli, W. Marszal, H. Miyamoto, M. Mignone, A. Murashov, T. Napolitano, H. Ohmori, A. Olinto, E. Parizot, P. Picozza, L. W. Piotrowski, Z. Plebaniak, G. Prévôt, E. Reali, M. Ricci, G. Romoli, N. Sakaki, K. Shinozaki, J. Szabelski, C. De La Taille, Y. Takizawa, M. Vrábel, L. Wiencke, M. Zotov
Abstract
More than three dozen submillisecond events of ELVES type (“elves”), which are the result of the interaction of the front of an electromagnetic pulse from a lightning discharge and the lower layer of the ionosphere, have been identified in the data of a UV Atmosphere orbital multichannel detector (Mini-EUSO). Each event has a characteristic annular glow pattern and occupies a significant part of the detector’s field of view, and the signal in a separate channel has an asymmetric profile with a pronounced peak. The distribution of peak times contains information about both the localization of the discharge and the altitude of the glow. In this paper, we propose a Bayesian (probabilistic) model for reconstructing ELVES events, implemented using probabilistic programming methods in PyMC-5. The capabilities of the model for determining the position of the discharge are shown using the example of several events. Methods for modifying the model to restore the discharge orientation and refine the glow height are outlined.
{"title":"ELVES Measurements in the “UV Atmosphere” (Mini-EUSO) Experiment Onboard the ISS and Their Reconstruction","authors":"S. Sharakin, D. Barghini, M. Battisti, A. Belov, M. Bertaina, M. Bianciotto, F. Bisconti, C. Blaksley, S. Blin, G. Cambiè, F. Capel, M. Casolino, T. Ebisuzaki, J. Eser, F. Fenu, M. A. Franceschi, A. Golzio, P. Gorodetsky, F. Kajino, H. Kasuga, P. Klimov, M. Manfrin, L. Marcelli, W. Marszal, H. Miyamoto, M. Mignone, A. Murashov, T. Napolitano, H. Ohmori, A. Olinto, E. Parizot, P. Picozza, L. W. Piotrowski, Z. Plebaniak, G. Prévôt, E. Reali, M. Ricci, G. Romoli, N. Sakaki, K. Shinozaki, J. Szabelski, C. De La Taille, Y. Takizawa, M. Vrábel, L. Wiencke, M. Zotov","doi":"10.1134/s0010952524600379","DOIUrl":"https://doi.org/10.1134/s0010952524600379","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>More than three dozen submillisecond events of ELVES type (“elves”), which are the result of the interaction of the front of an electromagnetic pulse from a lightning discharge and the lower layer of the ionosphere, have been identified in the data of a UV Atmosphere orbital multichannel detector (Mini-EUSO). Each event has a characteristic annular glow pattern and occupies a significant part of the detector’s field of view, and the signal in a separate channel has an asymmetric profile with a pronounced peak. The distribution of peak times contains information about both the localization of the discharge and the altitude of the glow. In this paper, we propose a Bayesian (probabilistic) model for reconstructing ELVES events, implemented using probabilistic programming methods in PyMC-5. The capabilities of the model for determining the position of the discharge are shown using the example of several events. Methods for modifying the model to restore the discharge orientation and refine the glow height are outlined.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"22 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141506772","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 : 2024-06-17DOI: 10.1134/s0010952524600409
L. S. Novikov, V. N. Chernik, E. N. Voronina, N. P. Chirskaya
Abstract
The paper describes a magnetoplasmodynamic accelerator and the laboratory facility based on it that have been developed at the Skobeltsyn Institute of Nuclear Physics of Moscow State University to simulate the impact of atomic oxygen in the Earth’s upper atmosphere on materials of low-orbit satellites. The simulation methodology for accelerated ground-based testing of spacecraft materials is described in detail. Some results of laboratory research and numerical modelling of polymeric materials destruction by atomic oxygen are presented.
{"title":"Modeling the Impact of Atomic Oxygen on Materials of Artificial Earth Satellites","authors":"L. S. Novikov, V. N. Chernik, E. N. Voronina, N. P. Chirskaya","doi":"10.1134/s0010952524600409","DOIUrl":"https://doi.org/10.1134/s0010952524600409","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The paper describes a magnetoplasmodynamic accelerator and the laboratory facility based on it that have been developed at the Skobeltsyn Institute of Nuclear Physics of Moscow State University to simulate the impact of atomic oxygen in the Earth’s upper atmosphere on materials of low-orbit satellites. The simulation methodology for accelerated ground-based testing of spacecraft materials is described in detail. Some results of laboratory research and numerical modelling of polymeric materials destruction by atomic oxygen are presented.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"36 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141531814","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 : 2024-06-17DOI: 10.1134/s0010952524600367
K. D. Shchelkanov, A. A. Belov, P. A. Klimov, V. D. Nikolaeva, R. E. Saraev, S. A. Sharakin
Abstract
In the autumn of 2021, a multichannel imaging photometer of the Pulsating Aurora Imaging Photometer System was installed at the Verkhnetulomsky Observatory. During the first season of operation (2021/2022), measurements were made over the course of 163 nights in three modes of temporal resolution: 2.5 μs, 320 μs, and 41 ms. The high temporal resolution makes it possible to investigate the fine temporal structure of the emission, which are short (less than 1 s) bursts of UV radiation, so-called “microbursts” that can be single or follow in series. The long-term series of microbursts registered on November 27–29, 2021, were analyzed. It is shown that the series of bursts have a complex temporal structure, individual bursts have several peaks with intervals of 100–400 ms, the intervals between bursts are of the order of 1 s, and they appear in packs lasting from several seconds to minutes. The series appear both in quiet geomagnetic conditions and during substorms; the frequency and amplitude of bursts in the second case are significantly larger.
{"title":"UV Microbursts in the Auroral Zone Measured by a Multichannel Imaging Photometer","authors":"K. D. Shchelkanov, A. A. Belov, P. A. Klimov, V. D. Nikolaeva, R. E. Saraev, S. A. Sharakin","doi":"10.1134/s0010952524600367","DOIUrl":"https://doi.org/10.1134/s0010952524600367","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>In the autumn of 2021, a multichannel imaging photometer of the Pulsating Aurora Imaging Photometer System was installed at the Verkhnetulomsky Observatory. During the first season of operation (2021/2022), measurements were made over the course of 163 nights in three modes of temporal resolution: 2.5 μs, 320 μs, and 41 ms. The high temporal resolution makes it possible to investigate the fine temporal structure of the emission, which are short (less than 1 s) bursts of UV radiation, so-called “microbursts” that can be single or follow in series. The long-term series of microbursts registered on November 27–29, 2021, were analyzed. It is shown that the series of bursts have a complex temporal structure, individual bursts have several peaks with intervals of 100–400 ms, the intervals between bursts are of the order of 1 s, and they appear in packs lasting from several seconds to minutes. The series appear both in quiet geomagnetic conditions and during substorms; the frequency and amplitude of bursts in the second case are significantly larger.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"34 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141529474","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 : 2024-06-17DOI: 10.1134/s0010952524600355
N. V. Yagova, N. S. Evsina
Abstract
Spectral and spatial parameters of nonstorm Pc5/Pi3 geomagnetic pulsations in the geomagnetic tail are studied based on magnetic measurements on Cluster satellites under different conditions in the interplanetary medium. Both the average values of the magnetic field components in front of the bow shock and fluctuations in the pulsations’ frequency range are considered. Special attention is paid to the conditions of small amplitudes of fluctuations (“zero” perturbation) in order to localize the source of pulsations starting under these conditions. For this purpose, simultaneous data from two satellites located on one or different sides of the magnetopause are used. It is shown that, along with a decrease in the amplitude of fluctuations in front of the bow shock, the amplitude and spatial scale of fluctuations in the magnetosheath change and the coherence between fluctuations on different sides of the magnetopause decreases sharply. This allows us to conclude that the pulsations occurring in the geomagnetic tail under “zero” level fluctuations in front of the bow shock are an intramagnetospheric phenomenon weakly related to the processes beyond the magnetopause.
{"title":"Geomagnetic Pulsations in the 1–4 mHz Frequency Range (Pc5/Pi3) in the Magnetotail. Internal and Extramagnetospheric Sources","authors":"N. V. Yagova, N. S. Evsina","doi":"10.1134/s0010952524600355","DOIUrl":"https://doi.org/10.1134/s0010952524600355","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Spectral and spatial parameters of nonstorm Pc5/Pi3 geomagnetic pulsations in the geomagnetic tail are studied based on magnetic measurements on <i>Cluster</i> satellites under different conditions in the interplanetary medium. Both the average values of the magnetic field components in front of the bow shock and fluctuations in the pulsations’ frequency range are considered. Special attention is paid to the conditions of small amplitudes of fluctuations (“zero” perturbation) in order to localize the source of pulsations starting under these conditions. For this purpose, simultaneous data from two satellites located on one or different sides of the magnetopause are used. It is shown that, along with a decrease in the amplitude of fluctuations in front of the bow shock, the amplitude and spatial scale of fluctuations in the magnetosheath change and the coherence between fluctuations on different sides of the magnetopause decreases sharply. This allows us to conclude that the pulsations occurring in the geomagnetic tail under “zero” level fluctuations in front of the bow shock are an intramagnetospheric phenomenon weakly related to the processes beyond the magnetopause.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"177 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141506813","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 : 2024-06-17DOI: 10.1134/s0010952524600380
A. N. Turundaevskiy, N. I. Nikolaeva, A. D. Panov, M. V. Podzolko, D. M. Podorozhny, K. R. Rakhimchanova
Abstract
Estimates of doses inside the spacecraft were carried out for flights to the Moon using low-thrust engines. The characteristics of the trajectory, which is significantly different from the Hohmann trajectory, are taken into account. Such a trajectory causes a long stay inside the radiation belts, which can cause disruptions in the operation of onboard equipment. It turned out that, during long-term transportation of food products, they may be damaged under the influence of radiation. This is extremely important in the case of the creation of habitable stations on the Moon surface or near-Moon orbit. The presented results can be used in the preparation of future space experiments.
{"title":"Estimating Expected Radiation Doses in a Flight to the Moon Using Low-Thrust Engines","authors":"A. N. Turundaevskiy, N. I. Nikolaeva, A. D. Panov, M. V. Podzolko, D. M. Podorozhny, K. R. Rakhimchanova","doi":"10.1134/s0010952524600380","DOIUrl":"https://doi.org/10.1134/s0010952524600380","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Estimates of doses inside the spacecraft were carried out for flights to the Moon using low-thrust engines. The characteristics of the trajectory, which is significantly different from the Hohmann trajectory, are taken into account. Such a trajectory causes a long stay inside the radiation belts, which can cause disruptions in the operation of onboard equipment. It turned out that, during long-term transportation of food products, they may be damaged under the influence of radiation. This is extremely important in the case of the creation of habitable stations on the Moon surface or near-Moon orbit. The presented results can be used in the preparation of future space experiments.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"15 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141523929","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 : 2024-06-17DOI: 10.1134/s0010952524600392
Y. I. Stozhkov, V. P. Okhlopkov
Abstract
Experimental data on solar activity (sunspot number, induction of solar polar magnetic field Bp, and others), characteristics of interplanetary space, and cosmic ray fluxes testify that the Sun has entered a deep minimum of its activity similar to the Dalton minimum. An almost functional relationship was found between maximum values of Bpmax observed in the solar activity minimum of the 11-year cycle and the next sunspot maximum. Based on this relationship, a simple method of forecasting maximum number of sunspots Rzmax and time course Rz(t) was developed. A forecast of the 25th solar cycle is given.
{"title":"Solar Activity in the Last 20 Years and a Forecast of the 25th Solar Cycle","authors":"Y. I. Stozhkov, V. P. Okhlopkov","doi":"10.1134/s0010952524600392","DOIUrl":"https://doi.org/10.1134/s0010952524600392","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>Experimental data on solar activity (sunspot number, induction of solar polar magnetic field <i>B</i><sub>p</sub>, and others), characteristics of interplanetary space, and cosmic ray fluxes testify that the Sun has entered a deep minimum of its activity similar to the Dalton minimum. An almost functional relationship was found between maximum values of <i>B</i><sub>pmax</sub> observed in the solar activity minimum of the 11-year cycle and the next sunspot maximum. Based on this relationship, a simple method of forecasting maximum number of sunspots <i>R</i><sub>zmax</sub> and time course <i>R</i><sub>z</sub>(t) was developed. A forecast of the 25th solar cycle is given.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"29 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141506774","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 : 2024-06-17DOI: 10.1134/s0010952524600422
A. A. Vakhrusheva, K. B. Kaportseva, Yu. S. Shugay, V. E. Eremeev, V. V. Kalegaev
Abstract
The paper demonstrates results of modeling arrival time of coronal mass ejections (CME) to near-Earth space with parameters of coronal dimmings in 2010–2018. We use drag-based model (DBM) for CME propagation and empirical model for quasi-stationary solar wind streams. We compared the ICME arrival time and speed forecast for events with coronal source in the central region of the solar disk based on the CME initial speed using (1) CACTus database; (2) dimming maximum intensity drop from Solar Demon database to calculate the initial speed of the CME. Results show that the methods result in similar errors. To study the possibility of predicting ICME, for which a CME may not be observed in the coronagraph for some reason, modeling of ICME was carried out using dimming parameters. In 43% of cases, ICME arrival time were forecasted with an accuracy of 24 h using parameters of dimmings in the central region of solar disk that could not be associated with any CMEs.
{"title":"Modeling Arrival Time of Coronal Mass Ejections to Near-Earth Orbit Using Coronal Dimming Parameters","authors":"A. A. Vakhrusheva, K. B. Kaportseva, Yu. S. Shugay, V. E. Eremeev, V. V. Kalegaev","doi":"10.1134/s0010952524600422","DOIUrl":"https://doi.org/10.1134/s0010952524600422","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The paper demonstrates results of modeling arrival time of coronal mass ejections (CME) to near-Earth space with parameters of coronal dimmings in 2010–2018. We use drag-based model (DBM) for CME propagation and empirical model for quasi-stationary solar wind streams. We compared the ICME arrival time and speed forecast for events with coronal source in the central region of the solar disk based on the CME initial speed using (1) CACTus database; (2) dimming maximum intensity drop from Solar Demon database to calculate the initial speed of the CME. Results show that the methods result in similar errors. To study the possibility of predicting ICME, for which a CME may not be observed in the coronagraph for some reason, modeling of ICME was carried out using dimming parameters. In 43% of cases, ICME arrival time were forecasted with an accuracy of 24 h using parameters of dimmings in the central region of solar disk that could not be associated with any CMEs.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"9 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141506775","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 : 2024-06-17DOI: 10.1134/s0010952524600410
N. A. Vlasova, V. V. Kalegaev
Abstract
The paper presents the results of studying the dynamics of the magnetic field and electron fluxes of the Earth’s outer radiation belt with an energy of >2 MeV according to the GOES-15 geostationary satellite during a fairly long period (October 16, 2016 to February 16, 2017) of moderate and weak magnetospheric activity caused by the arrival of a sequence of high-speed solar wind streams. The main variations in the electron flux in the geostationary orbit are caused by the movement, deceleration and acceleration of particles in the outer radiation belt of the Earth under the influence of geomagnetic activity. The results of a comparative analysis of variations in electron fluxes and components of the magnetospheric field testify to the predominant influence of the magnitude and structure of the magnetospheric field on the dynamics of relativistic electron fluxes in the outer radiation belt. Changes in the components of the magnetospheric magnetic field and in electron fluxes are results of a single process that occurs together with changes in the magnetosphere as a whole.
{"title":"On Consistent Dynamics of the Magnetic Field and Relativistic Electron Fluxes in the Geostationary Orbit Region","authors":"N. A. Vlasova, V. V. Kalegaev","doi":"10.1134/s0010952524600410","DOIUrl":"https://doi.org/10.1134/s0010952524600410","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The paper presents the results of studying the dynamics of the magnetic field and electron fluxes of the Earth’s outer radiation belt with an energy of >2 MeV according to the <i>GOES-15</i> geostationary satellite during a fairly long period (October 16, 2016 to February 16, 2017) of moderate and weak magnetospheric activity caused by the arrival of a sequence of high-speed solar wind streams. The main variations in the electron flux in the geostationary orbit are caused by the movement, deceleration and acceleration of particles in the outer radiation belt of the Earth under the influence of geomagnetic activity. The results of a comparative analysis of variations in electron fluxes and components of the magnetospheric field testify to the predominant influence of the magnitude and structure of the magnetospheric field on the dynamics of relativistic electron fluxes in the outer radiation belt. Changes in the components of the magnetospheric magnetic field and in electron fluxes are results of a single process that occurs together with changes in the magnetosphere as a whole. </p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"14 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141506773","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 : 2024-06-04DOI: 10.1134/s0010952524600240
A. A. Burov, V. I. Nikonov
Abstract
For asteroid (433) Eros, a multipole representation of the gravitational potential is determined up to multipoles of the fourth order. The obtained expression for the potential is used in constructing the areas of possible motion of the spacecraft in the vicinity of the celestial body under consideration.
{"title":"A Multipole Representation for the Gravitational Field of Asteroid (433) Eros","authors":"A. A. Burov, V. I. Nikonov","doi":"10.1134/s0010952524600240","DOIUrl":"https://doi.org/10.1134/s0010952524600240","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>For asteroid (433) Eros, a multipole representation of the gravitational potential is determined up to multipoles of the fourth order. The obtained expression for the potential is used in constructing the areas of possible motion of the spacecraft in the vicinity of the celestial body under consideration.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"25 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141256335","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 : 2024-06-04DOI: 10.1134/s0010952524600276
V. S. Vaskova, A. V. Rodnikov
Abstract
The paper considers the possibility of cargo relocation without fuel costs along a tether connecting two heavy space stations by a spacecraft with a controlled solar sail. The spacecraft’s relative motion dynamics is studied within the context of a model problem that assumes that the stations describe one heliocentric orbit, the solar sail is a perfect reflective flat panel, and the tether realizes an ideal unilateral handrail constraint that restricts the spacecraft relative motion to an ellipsoid. It is noted that, if the distance between stations is sufficiently small and the ratio of the sail area to the spacecraft mass is on the same order of magnitude as in already-implemented space missions, solar radiation is the main factor that influences the spacecraft’s motion in the orbital frame of reference. The problem of searching a set of pairs of points, between which relocation with a permanently oriented sail is possible, is solved for the pairs that belong to the intersection of the ellipsoid boundary and the plane of the stations’ orbit. The duration of the spacecraft relocation between the ellipsoid poles is estimated for the case of the sail oriented orthogonally to the solar rays. Also, the duration of the fastest relocation between poles is computed using special sail orientation control laws, including the case of zero initial and final velocities.
{"title":"A Model Problem of Motion along the Handrail Constraint by a Solar Sail","authors":"V. S. Vaskova, A. V. Rodnikov","doi":"10.1134/s0010952524600276","DOIUrl":"https://doi.org/10.1134/s0010952524600276","url":null,"abstract":"<h3 data-test=\"abstract-sub-heading\">Abstract</h3><p>The paper considers the possibility of cargo relocation without fuel costs along a tether connecting two heavy space stations by a spacecraft with a controlled solar sail. The spacecraft’s relative motion dynamics is studied within the context of a model problem that assumes that the stations describe one heliocentric orbit, the solar sail is a perfect reflective flat panel, and the tether realizes an ideal unilateral handrail constraint that restricts the spacecraft relative motion to an ellipsoid. It is noted that, if the distance between stations is sufficiently small and the ratio of the sail area to the spacecraft mass is on the same order of magnitude as in already-implemented space missions, solar radiation is the main factor that influences the spacecraft’s motion in the orbital frame of reference. The problem of searching a set of pairs of points, between which relocation with a permanently oriented sail is possible, is solved for the pairs that belong to the intersection of the ellipsoid boundary and the plane of the stations’ orbit. The duration of the spacecraft relocation between the ellipsoid poles is estimated for the case of the sail oriented orthogonally to the solar rays. Also, the duration of the fastest relocation between poles is computed using special sail orientation control laws, including the case of zero initial and final velocities.</p>","PeriodicalId":56319,"journal":{"name":"Cosmic Research","volume":"25 1","pages":""},"PeriodicalIF":0.6,"publicationDate":"2024-06-04","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141256254","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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