Pub Date : 2020-09-01DOI: 10.5140/JASS.2020.37.3.171
Daniela Espitia, E. Quintero, I. D. Arellano-Ramírez
This paper presents a methodology for Initial Orbit Determination (IOD) based on a modification of the Laplace’s geocentric method. The orbital elements for Near-Earth asteroids (1864) Daedalus, 2003 GW, 2019 JA8, a Hungaria-type asteroid (4690) Strasbourg, and the asteroids of the Main Belt (1738) Oosterhoff, (2717) Tellervo, (1568) Aisleen and (2235) Vittore were calculated. Input data observations from the Minor Planet Center MPC database and Astronomical Observatory of the Technological University of Pereira (OAUTP; MPC code W63) were used. These observations cover observation arcs of less than 22 days. The orbital errors, in terms of shape and orientation for the estimated orbits of the asteroids, were calculated. The shape error was less than 53 × 10–3 AU, except for the asteroid 2019 JA8. On the other hand, errors in orientation were less than 0.1 rad, except for (4690) Strasbourg. Additionally, we estimated ephemerides for all bodies for up to two months. When compared with actual ephemerides, the errors found allowed us to conclude that these bodies can be recovered in a field of vision of 95’ × 72’ (OAUTP field). This shows that Laplace’s method, though simple, may still be useful in the IOD study, especially for observatories that initiate programs of minor bodies observation.
{"title":"Determination of Orbital Elements and Ephemerides using the Geocentric Laplace’s\u0000 Method","authors":"Daniela Espitia, E. Quintero, I. D. Arellano-Ramírez","doi":"10.5140/JASS.2020.37.3.171","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.3.171","url":null,"abstract":"This paper presents a methodology for Initial Orbit Determination (IOD) based on\u0000 a modification of the Laplace’s geocentric method. The orbital elements for Near-Earth\u0000 asteroids (1864) Daedalus, 2003 GW, 2019 JA8, a Hungaria-type asteroid (4690)\u0000 Strasbourg, and the asteroids of the Main Belt (1738) Oosterhoff, (2717) Tellervo,\u0000 (1568) Aisleen and (2235) Vittore were calculated. Input data observations from the\u0000 Minor Planet Center MPC database and Astronomical Observatory of the Technological\u0000 University of Pereira (OAUTP; MPC code W63) were used. These observations cover\u0000 observation arcs of less than 22 days. The orbital errors, in terms of shape and\u0000 orientation for the estimated orbits of the asteroids, were calculated. The shape error\u0000 was less than 53 × 10–3 AU, except for the asteroid 2019 JA8. On the other hand, errors\u0000 in orientation were less than 0.1 rad, except for (4690) Strasbourg. Additionally, we\u0000 estimated ephemerides for all bodies for up to two months. When compared with actual\u0000 ephemerides, the errors found allowed us to conclude that these bodies can be recovered\u0000 in a field of vision of 95’ × 72’ (OAUTP field). This shows that Laplace’s method,\u0000 though simple, may still be useful in the IOD study, especially for observatories that\u0000 initiate programs of minor bodies observation.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"91142154","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-09-01DOI: 10.5140/JASS.2020.37.3.187
Mi-Jin Jeong, D. Cho, Hae-Dong Kim
In order to avoid the high cost and high risk of demonstration mission of rendezvous-docking technology, missions using nanosatellites have recently been increasing. However, there are few successful mission cases due to many limitations of nanosatellites like small size, power limitation, and limited performances of sensor, thruster, and controller. To improve the probability of rendezvous-docking mission success using nanosatellite, a rendezvous-docking phase analysis tool for nanosatellites is developed. The tool serves to analyze the relative position and attitude control of the chaser satellite at the docking phase. In this tool, the Model Predictive Controller (MPC) is implemented as a controller, and Extended Kalman Filter (EKF) is adopted as a filter for noise filtering. To verify the performance and effectiveness of the developed tool for nanosatellites, simulation study was conducted. Consequently, we confirmed that this tool can be used for the analysis of relative position and attitude control for nanosatellites in the rendezvous-docking phase.
{"title":"A Development of Docking Phase Analysis Tool for Nanosatellite","authors":"Mi-Jin Jeong, D. Cho, Hae-Dong Kim","doi":"10.5140/JASS.2020.37.3.187","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.3.187","url":null,"abstract":"In order to avoid the high cost and high risk of demonstration mission of\u0000 rendezvous-docking technology, missions using nanosatellites have recently been\u0000 increasing. However, there are few successful mission cases due to many limitations of\u0000 nanosatellites like small size, power limitation, and limited performances of sensor,\u0000 thruster, and controller. To improve the probability of rendezvous-docking mission\u0000 success using nanosatellite, a rendezvous-docking phase analysis tool for nanosatellites\u0000 is developed. The tool serves to analyze the relative position and attitude control of\u0000 the chaser satellite at the docking phase. In this tool, the Model Predictive Controller\u0000 (MPC) is implemented as a controller, and Extended Kalman Filter (EKF) is adopted as a\u0000 filter for noise filtering. To verify the performance and effectiveness of the developed\u0000 tool for nanosatellites, simulation study was conducted. Consequently, we confirmed that\u0000 this tool can be used for the analysis of relative position and attitude control for\u0000 nanosatellites in the rendezvous-docking phase.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80299705","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-09-01DOI: 10.5140/JASS.2020.37.3.157
A. Yushchenko, Chulhee Kim, Yeuncheol Jeong, D. Doikov, V. Yushchenko, S. V. Khrapatyi, A. Demessinova
High resolution spectroscopic observation of V1719 Cyg were made at 1.8 meter telescope of Bohyunsan Optical Astronomy observatory in Korea. Spectral resolving power was R=45,000, signal to noise ratio S/N>100. The abundances of 28 chemical elements from carbon to dysprosium were found with the spectrum synthesis method. The abundances of oxygen, titanium, vanadium and elements with Z>30 are overabundant by 0.2–0.9 dex with respect to the solar values. Correlations of derived abundances with condensation temperatures and second ionization potentials of these elements are discussed. The possible influence of accretion from interstellar environment is not so strong as for ρ Pup and other stars with similar temperatures. The signs of accretion are absent. The comparison of chemical composition with solar system r- & s-process abundance patterns shows the enhancement of the photosphere by s-process elements.
{"title":"The Chemical Composition of V1719 Cyg: δ Scuti Type Star without the Accretion of\u0000 Interstellar Matter","authors":"A. Yushchenko, Chulhee Kim, Yeuncheol Jeong, D. Doikov, V. Yushchenko, S. V. Khrapatyi, A. Demessinova","doi":"10.5140/JASS.2020.37.3.157","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.3.157","url":null,"abstract":"High resolution spectroscopic observation of V1719 Cyg were made at 1.8 meter\u0000 telescope of Bohyunsan Optical Astronomy observatory in Korea. Spectral resolving power\u0000 was R=45,000, signal to noise ratio S/N>100. The abundances of 28 chemical elements\u0000 from carbon to dysprosium were found with the spectrum synthesis method. The abundances\u0000 of oxygen, titanium, vanadium and elements with Z>30 are overabundant by 0.2–0.9 dex\u0000 with respect to the solar values. Correlations of derived abundances with condensation\u0000 temperatures and second ionization potentials of these elements are discussed. The\u0000 possible influence of accretion from interstellar environment is not so strong as for ρ\u0000 Pup and other stars with similar temperatures. The signs of accretion are absent. The\u0000 comparison of chemical composition with solar system r- & s-process abundance\u0000 patterns shows the enhancement of the photosphere by s-process elements.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80054043","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-09-01DOI: 10.5140/JASS.2020.37.3.199
Min-Sup Song, Sang-Young Park, Youngkwang Kim, J. Yim
This paper presents a kinematic ephemeris generator for Korea Pathfinder Lunar Orbiter (KPLO) and its performance test results. The kinematic ephemeris generator consists of a ground ephemeris compressor and an onboard ephemeris calculator. The ground ephemeris compressor has to compress desired orbit propagation data by using an interpolation method in a ground system. The onboard ephemeris calculator can generate spacecraft ephemeris and the Sun/Moon ephemeris in onboard computer of the KPLO. Among many interpolation methods, polynomial interpolation with uniform node, Chebyshev interpolation, Hermite interpolation are tested for their performances. As a result of the test, it is shown that all the methods have some cases that meet requirements but there are some performance differences. It is also confirmed that, the Chebyshev interpolation shows better performance than other methods for spacecraft ephemeris generation, and the polynomial interpolation with uniform nodes yields good performance for the Sun/Moon ephemeris generation. Based on these results, a Kinematic ephemeris generator is developed for the KPLO mission. Then, the developed ephemeris generator can find an approximating function using interpolation method considering the size and accuracy of the data to be transmitted.
{"title":"Development of Kinematic Ephemeris Generator for Korea Pathfinder Lunar Orbiter\u0000 (KPLO)","authors":"Min-Sup Song, Sang-Young Park, Youngkwang Kim, J. Yim","doi":"10.5140/JASS.2020.37.3.199","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.3.199","url":null,"abstract":"This paper presents a kinematic ephemeris generator for Korea Pathfinder Lunar\u0000 Orbiter (KPLO) and its performance test results. The kinematic ephemeris generator\u0000 consists of a ground ephemeris compressor and an onboard ephemeris calculator. The\u0000 ground ephemeris compressor has to compress desired orbit propagation data by using an\u0000 interpolation method in a ground system. The onboard ephemeris calculator can generate\u0000 spacecraft ephemeris and the Sun/Moon ephemeris in onboard computer of the KPLO. Among\u0000 many interpolation methods, polynomial interpolation with uniform node, Chebyshev\u0000 interpolation, Hermite interpolation are tested for their performances. As a result of\u0000 the test, it is shown that all the methods have some cases that meet requirements but\u0000 there are some performance differences. It is also confirmed that, the Chebyshev\u0000 interpolation shows better performance than other methods for spacecraft ephemeris\u0000 generation, and the polynomial interpolation with uniform nodes yields good performance\u0000 for the Sun/Moon ephemeris generation. Based on these results, a Kinematic ephemeris\u0000 generator is developed for the KPLO mission. Then, the developed ephemeris generator can\u0000 find an approximating function using interpolation method considering the size and\u0000 accuracy of the data to be transmitted.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-09-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82609570","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-06-01DOI: 10.5140/JASS.2020.37.2.117
S. Ayana, Seongmin Lim, D. Cho, Hae-Dong Kim
In a Satellite communication system, a link budget analysis is the detailed investigation of signal gains and losses moving through a channel from a sender to receiver. It inspects the fading of passed on data signal waves due to the process of spreading or propagation, including transmitter and receiver antenna gains, feeder cables, and related losses. The extent of the proposed tool is to make an effective, efficient, and user-friendly approach to calculate link budget analysis. It is also related to the satellite communication correlation framework by building up a graphical interface link analysis tool utilizing STK® software with the interface of C# programming. It provides better kinds of graphical display techniques, exporting and importing data files, printing link information, access data, azimuth-elevation-range (AER), and simulation is also possible at once. The components of the link budget analysis tool include transmitter gain, effective isotropic radiated power (EIRP), free space loss, propagation loss, frequency Doppler shift, flux density, link margin, elevation plot, etc. This tool can be useful for amateur users (e.g., CubeSat developers in the universities) or nanosat developers who may not know about the RF communication system of the satellite and the orbital mechanics (e.g., orbit propagators) principle used in the satellite link analysis.
{"title":"A Development of Satellite Communication Link Analysis Tool","authors":"S. Ayana, Seongmin Lim, D. Cho, Hae-Dong Kim","doi":"10.5140/JASS.2020.37.2.117","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.2.117","url":null,"abstract":"In a Satellite communication system, a link budget analysis is the detailed\u0000 investigation of signal gains and losses moving through a channel from a sender to\u0000 receiver. It inspects the fading of passed on data signal waves due to the process of\u0000 spreading or propagation, including transmitter and receiver antenna gains, feeder\u0000 cables, and related losses. The extent of the proposed tool is to make an effective,\u0000 efficient, and user-friendly approach to calculate link budget analysis. It is also\u0000 related to the satellite communication correlation framework by building up a graphical\u0000 interface link analysis tool utilizing STK® software with the interface of C#\u0000 programming. It provides better kinds of graphical display techniques, exporting and\u0000 importing data files, printing link information, access data, azimuth-elevation-range\u0000 (AER), and simulation is also possible at once. The components of the link budget\u0000 analysis tool include transmitter gain, effective isotropic radiated power (EIRP), free\u0000 space loss, propagation loss, frequency Doppler shift, flux density, link margin,\u0000 elevation plot, etc. This tool can be useful for amateur users (e.g., CubeSat developers\u0000 in the universities) or nanosat developers who may not know about the RF communication\u0000 system of the satellite and the orbital mechanics (e.g., orbit propagators) principle\u0000 used in the satellite link analysis.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77066634","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-06-01DOI: 10.5140/JASS.2020.37.2.85
K. Min, Kaijun Liu
Equatorial noise, also known magnetosonic waves (MSWs), are one of the frequently observed plasma waves in Earth’s inner magnetosphere. Observations have shown that wave amplitudes maximize at the magnetic equator with a narrow extent in their latitudinal distribution. It has been understood that waves are generated from an equatorial source region and confined within a few degrees magnetic latitude. The present study investigates whether the MSW instability and saturation amplitudes maximize at the equator, given an energetic proton ring-like distribution derived from an observed wave event, and using linear instability analysis and particle-in-cell simulations with the plasma conditions at different latitudes along the dipole magnetic field line. The results show that waves initially grow fastest (i.e., with the largest growth rate) at high latitude (20°–25°), but consistent with observations, their saturation amplitudes maximize within ±10° latitude. On the other hand, the slope of the saturation amplitudes versus latitude revealed in the present study is not as steep as what the previous statistical observation results suggest. This may be indicative of some other factors not considered in the present analyses at play, such as background magnetic field and plasma inhomogeneities and the propagation effect.
{"title":"Linear Instability and Saturation Characteristics of Magnetosonic Waves along the\u0000 Magnetic Field Line","authors":"K. Min, Kaijun Liu","doi":"10.5140/JASS.2020.37.2.85","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.2.85","url":null,"abstract":"Equatorial noise, also known magnetosonic waves (MSWs), are one of the frequently\u0000 observed plasma waves in Earth’s inner magnetosphere. Observations have shown that wave\u0000 amplitudes maximize at the magnetic equator with a narrow extent in their latitudinal\u0000 distribution. It has been understood that waves are generated from an equatorial source\u0000 region and confined within a few degrees magnetic latitude. The present study\u0000 investigates whether the MSW instability and saturation amplitudes maximize at the\u0000 equator, given an energetic proton ring-like distribution derived from an observed wave\u0000 event, and using linear instability analysis and particle-in-cell simulations with the\u0000 plasma conditions at different latitudes along the dipole magnetic field line. The\u0000 results show that waves initially grow fastest (i.e., with the largest growth rate) at\u0000 high latitude (20°–25°), but consistent with observations, their saturation amplitudes\u0000 maximize within ±10° latitude. On the other hand, the slope of the saturation amplitudes\u0000 versus latitude revealed in the present study is not as steep as what the previous\u0000 statistical observation results suggest. This may be indicative of some other factors\u0000 not considered in the present analyses at play, such as background magnetic field and\u0000 plasma inhomogeneities and the propagation effect.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"82289161","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-06-01DOI: 10.5140/JASS.2020.37.2.131
Bogyeong Kim, H. Yun
As the laws of physics are expressed in a manner that makes their invariance under coordinate transformations manifest, they should be written in terms of tensors. Furthermore, tensors make manifest the characteristics and behaviors of electromagnetic fields through inhomogeneous, anisotropic, and compressible media. Electromagnetic fields are expressed completely in tensor form, Fαβ, which implies both electric field E → and magnetic field B → rather than separately in the vector fields. This study presents the Mathematica platform that generates and transforms a second-rank antisymmetric field-strength tensor Fαβ and whiskbroom pattern in Minkowski space. The platforms enhance the capabilities of students and researchers in tensor analysis and improves comprehension of the elegant features of complete structure in physics.
{"title":"Creating and Transforming a Second-Rank Antisymmetric Field-Strength Tensor Fαβ in\u0000 Minkowski Space using MATHEMATICA","authors":"Bogyeong Kim, H. Yun","doi":"10.5140/JASS.2020.37.2.131","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.2.131","url":null,"abstract":"As the laws of physics are expressed in a manner that makes their invariance\u0000 under coordinate transformations manifest, they should be written in terms of tensors.\u0000 Furthermore, tensors make manifest the characteristics and behaviors of electromagnetic\u0000 fields through inhomogeneous, anisotropic, and compressible media. Electromagnetic\u0000 fields are expressed completely in tensor form, Fαβ, which implies both electric field E\u0000 → and magnetic field B → rather than separately in the vector fields. This study\u0000 presents the Mathematica platform that generates and transforms a second-rank\u0000 antisymmetric field-strength tensor Fαβ and whiskbroom pattern in Minkowski space. The\u0000 platforms enhance the capabilities of students and researchers in tensor analysis and\u0000 improves comprehension of the elegant features of complete structure in physics.\u0000","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"87638612","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-06-01DOI: 10.5140/JASS.2020.37.2.143
Young-bae Ham, G. Jee, Changsup Lee, H. Kwon, Jeong‐Han Kim, N. Zabotin, T. Bullett
Korea Polar Research Institute (KOPRI) installed an ionospheric sounding radar system called Vertical Incidence Pulsed Ionospheric Radar (VIPIR) at Jang Bogo Station (JBS) in 2015 in order to routinely monitor the state of the ionosphere in the auroral oval and polar cap regions. Since 2017, after two-year test operation, it has been continuously operated to produce various ionospheric parameters. In this article, we will introduce the characteristics of the JBS-VIPIR observations and possible applications of the data for the study on the polar ionosphere. The JBS-VIPIR utilizes a log periodic transmit antenna that transmits 0.5–25 MHz radio waves, and a receiving array of 8 dipole antennas. It is operated in the Dynasonde B-mode pulse scheme and utilizes the 3-D inversion program, called NeXtYZ, for the data acquisition and processing, instead of the conventional 1-D inversion procedure as used in the most of digisonde observations. The JBS-VIPIR outputs include the height profiles of the electron density, ionospheric tilts, and ion drifts with a 2-minute temporal resolution in the bottomside ionosphere. With these observations, possible research applications will be briefly described in combination with other observations for the aurora, the neutral atmosphere and the magnetosphere simultaneously conducted at JBS.
{"title":"Observations of the Polar Ionosphere by the Vertical Incidence Pulsed Ionospheric\u0000 Radar at Jang Bogo Station, Antarctica","authors":"Young-bae Ham, G. Jee, Changsup Lee, H. Kwon, Jeong‐Han Kim, N. Zabotin, T. Bullett","doi":"10.5140/JASS.2020.37.2.143","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.2.143","url":null,"abstract":"Korea Polar Research Institute (KOPRI) installed an ionospheric sounding radar\u0000 system called Vertical Incidence Pulsed Ionospheric Radar (VIPIR) at Jang Bogo Station\u0000 (JBS) in 2015 in order to routinely monitor the state of the ionosphere in the auroral\u0000 oval and polar cap regions. Since 2017, after two-year test operation, it has been\u0000 continuously operated to produce various ionospheric parameters. In this article, we\u0000 will introduce the characteristics of the JBS-VIPIR observations and possible\u0000 applications of the data for the study on the polar ionosphere. The JBS-VIPIR utilizes a\u0000 log periodic transmit antenna that transmits 0.5–25 MHz radio waves, and a receiving\u0000 array of 8 dipole antennas. It is operated in the Dynasonde B-mode pulse scheme and\u0000 utilizes the 3-D inversion program, called NeXtYZ, for the data acquisition and\u0000 processing, instead of the conventional 1-D inversion procedure as used in the most of\u0000 digisonde observations. The JBS-VIPIR outputs include the height profiles of the\u0000 electron density, ionospheric tilts, and ion drifts with a 2-minute temporal resolution\u0000 in the bottomside ionosphere. With these observations, possible research applications\u0000 will be briefly described in combination with other observations for the aurora, the\u0000 neutral atmosphere and the magnetosphere simultaneously conducted at JBS.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89469514","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-06-01DOI: 10.5140/JASS.2020.37.2.105
Jin Choi, J. Jo, E. Choi, Jiwoong Yu, Byung-Kyu Choi, Myung-Jin Kim, H. Yim, D. Roh, Sooyoung Kim, Jang-Hyun Park, Sungki Cho
The Korean Institute of Technology Satellite (KITSAT-1) is the first satellite developed by the Satellite Technology Research Center and the University of Surrey. KITSAT-1 is orbiting the Earth’s orbit as space debris with a 1,320 km altitude after the planned mission. Due to its relatively small size and altitude, tracking the KITSAT-1 was a difficult task. In this research, we analyzed the tracking results of KITSAT-1 for one year using the Midland Space Radar (MSR) in Texas and the Poker Flat Incoherent Scatter Radar (PFISR) in Alaska operated by LeoLabs, Inc. The tracking results were analyzed on a weekly basis for MSR and PFISR. The observation was conducted by using both stations at an average frequency of 10 times per week. The overall corrected range measurements for MSR and PFISR by LeoLabs were under 50 m and 25 m, respectively. The ionospheric delay, the dominant error source, was confirmed with the International Reference of Ionosphere-16 model and Global Navigation Satellite System data. The weekly basis orbit determination results were compared with two-line element data. The comparison results were used to confirm the orbital consistency of the estimated orbits.
{"title":"Space Surveillance Radar Observation Analysis: One-Year Tracking and Orbit\u0000 Determination Results of KITSAT-1, “우리별 1호”","authors":"Jin Choi, J. Jo, E. Choi, Jiwoong Yu, Byung-Kyu Choi, Myung-Jin Kim, H. Yim, D. Roh, Sooyoung Kim, Jang-Hyun Park, Sungki Cho","doi":"10.5140/JASS.2020.37.2.105","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.2.105","url":null,"abstract":"The Korean Institute of Technology Satellite (KITSAT-1) is the first satellite\u0000 developed by the Satellite Technology Research Center and the University of Surrey.\u0000 KITSAT-1 is orbiting the Earth’s orbit as space debris with a 1,320 km altitude after\u0000 the planned mission. Due to its relatively small size and altitude, tracking the\u0000 KITSAT-1 was a difficult task. In this research, we analyzed the tracking results of\u0000 KITSAT-1 for one year using the Midland Space Radar (MSR) in Texas and the Poker Flat\u0000 Incoherent Scatter Radar (PFISR) in Alaska operated by LeoLabs, Inc. The tracking\u0000 results were analyzed on a weekly basis for MSR and PFISR. The observation was conducted\u0000 by using both stations at an average frequency of 10 times per week. The overall\u0000 corrected range measurements for MSR and PFISR by LeoLabs were under 50 m and 25 m,\u0000 respectively. The ionospheric delay, the dominant error source, was confirmed with the\u0000 International Reference of Ionosphere-16 model and Global Navigation Satellite System\u0000 data. The weekly basis orbit determination results were compared with two-line element\u0000 data. The comparison results were used to confirm the orbital consistency of the\u0000 estimated orbits.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80828311","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2020-06-01DOI: 10.5140/JASS.2020.37.2.77
K. Park, Dae‐Young Lee, Khan‐Hyuk Kim
We performed high-resolution three-dimensional global magnetohydrodynamic (MHD) simulations to study the interaction between the Earth’s magnetosphere and a prolonged steady southward interplanetary magnetic field (IMF) (Bz = –2nT) and slow solar wind. The simulation results show that dayside magnetic reconnection continuously occurs at the subsolar region where the magnetosheath magnetic field is antiparallel to the geomagnetic field. The plasmoid developed on closed plasma sheet field lines. We found that the vortex was generated at the magnetic equator such as (X, Y) = (7.6, 8.9) RE due to the viscous-like interaction, which was strengthened by dayside reconnection. The magnetic field and plasma properties clearly showed quasiperiodic variations with a period of 8–10 min across the vortex. Additionally, double twin parallel vorticity in the polar region was clearly seen. The peak value of the cross-polar cap potential fluctuated between 17 and 20 kV during the tail reconnection.
{"title":"Global MHD Simulation of a Prolonged Steady Weak Southward Interplanetary Magnetic\u0000 Field Condition","authors":"K. Park, Dae‐Young Lee, Khan‐Hyuk Kim","doi":"10.5140/JASS.2020.37.2.77","DOIUrl":"https://doi.org/10.5140/JASS.2020.37.2.77","url":null,"abstract":"We performed high-resolution three-dimensional global magnetohydrodynamic (MHD)\u0000 simulations to study the interaction between the Earth’s magnetosphere and a prolonged\u0000 steady southward interplanetary magnetic field (IMF) (Bz = –2nT) and slow solar wind.\u0000 The simulation results show that dayside magnetic reconnection continuously occurs at\u0000 the subsolar region where the magnetosheath magnetic field is antiparallel to the\u0000 geomagnetic field. The plasmoid developed on closed plasma sheet field lines. We found\u0000 that the vortex was generated at the magnetic equator such as (X, Y) = (7.6, 8.9) RE due\u0000 to the viscous-like interaction, which was strengthened by dayside reconnection. The\u0000 magnetic field and plasma properties clearly showed quasiperiodic variations with a\u0000 period of 8–10 min across the vortex. Additionally, double twin parallel vorticity in\u0000 the polar region was clearly seen. The peak value of the cross-polar cap potential\u0000 fluctuated between 17 and 20 kV during the tail reconnection.","PeriodicalId":44366,"journal":{"name":"Journal of Astronomy and Space Sciences","volume":null,"pages":null},"PeriodicalIF":0.5,"publicationDate":"2020-06-01","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"79366630","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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