Meteor Research Research Articles

A Machine Learning Algorithm to Detect and Analyze Meteor Echoes Observed by the Jicamarca Radar

We present a machine-learning approach to detect and analyze meteor echoes (MADAME), which is a radar data processing workflow featuring advanced machine-learning techniques using both supervised and unsupervised learning. Our results demonstrate that YOLOv4, a convolutional neural network (CNN)-based one-stage object detection model, performs remarkably well in detecting and identifying meteor head and trail echoes within processed radar signals. The detector can identify more than 80 echoes per minute in the testing data obtained from the Jicamarca high power large aperture (HPLA) radar. MADAME is also capable of autonomously processing data in an interferometer mode, as well as determining the target’s radiant source and vector velocity. In the testing data, the Eta Aquarids meteor shower could be clearly identified from the meteor radiant source distribution analyzed automatically by MADAME, thereby demonstrating the proposed algorithm’s functionality. In addition, MADAME found that about 50 percent of the meteors were traveling in inclined and near-inclined circular orbits. Furthermore, meteor head echoes with a trail are more likely to originate from shower meteor sources. Our results highlight the capability of advanced machine-learning techniques in radar signal processing, providing an efficient and powerful tool to facilitate future and new meteor research.

Spectral observations at the Canary Island Long-Baseline Observatory (CILBO): calibration and datasets

Abstract. The Canary Island Long-Baseline Observatory (CILBO) is a double-station meteor camera setup located on the Canary Islands operated by ESA's Meteor Research Group since 2010. Observations of meteors are obtained in the visual wavelength band by intensified video cameras from both stations, supplemented by an intensified video camera mounted with a spectral grating at one of the locations. The cameras observe during cloudless and precipitation-free nights, and data are transferred to a main computer located at ESA/ESTEC once a day. The image frames that contain spectral information are calibrated, corrected, and finally processed into line intensity profiles. An ablation simulation, based on Bayesian statistics using a Markov chain Monte Carlo method, allows determining a parameter space, including the ablation temperatures, chemical elements, and their corresponding line intensities, to fit against the line intensity profiles of the observed meteor spectra. The algorithm is presented in this paper and one example is discussed. Several hundred spectra have been processed and made available through the Guest Archive Facility of the Planetary Science Archive of ESA. The data format and metadata are explained.

USE OF THE RESULTS OF THE WORK OF THE UKRAINIAN METEOR NETWORK IN THE PROCESS OF TEACHING PHYSICS TO STUDENTS OF THE EDUCATIONAL AND SCIENTIFIC INSTITUTE OF ENERGY, AUTOMATION AND ENERGY SAVING NULES OF UKRAINE

Features of meteor fixation methods are presented by organizing a network of corresponding observation points - permanently operating observation stations located on the territory of Ukraine with appropriate technical and software support for conducting basic and one-way observations of meteors in the radio range of electromagnetic wavelengths. This contributes to solving the strategic problems of meteor research, the structure and evolution of meteor showers and streams, the interaction of meteoroids with the Earth's atmosphere and their chemical composition. Scientific and technical products of observation stations are the results of high-precision basic or one-sided observations of meteors in the radio range of electromagnetic wavelengths, fundamental and applied scientific and technical research. The purpose of the study is to consider the principle of operation of the Ukrainian meteor observation network, a separate meteor hardware and software complex for observing meteors in the radio range of electromagnetic waves using the method of direct scattering on meteor trails of signals from powerful FM radio broadcasting stations with the possibility of further processing and presentation of data by students of specialties 141 "Electric power, electrical engineering and electromechanics", 144 "Thermal power engineering", 174 "Automation, computer-integrated technologies and robotics" of the Educational and Scientific Institute of Energy, Automation and Energy Saving of NULES of Ukraine in the process of studying physics. Processing of experimental data was carried out by students of the specified specialties under the guidance of the author while studying physics. The results of statistical data processing of meteor invasions and their graphic representation by students of the specified specialties in the process of mastering physics are described. Prospects - putting into operation by the end of 2024 the seventh receiving station in the city of Kyiv (student campus of NULES of Ukraine) - the seventh meteor hardware and software complex, as a component of the Ukrainian meteor observation network.

Creation of the Ukrainian meteor observation network: instruments, methods for processing, observatin possibilities

The development of meteor astronomy in modern Ukraine is considered. The specificity of meteor observation methods requires, first of all, the organization of a network of corresponding observation points. To achieve this goal, it is proposed to combine the scientific and technical capabilities of participating organizations in the form of the Ukrainian Meteor Observation Network (UMON). UMON is a set of two or more permanent observation stations located on the territory of Ukraine, which have the hardware and software for basic and one-sided observations of meteors in different wavelength ranges and conduct such observations. UMON aims to solve important problems of meteor research, structure and evolution of meteor streams and showers, the interaction of meteoroids with the Earth’s atmosphere and their chemical composition. The scientific and technical products of UMON stations are the results of high-precision basic or one-sided observations of meteors in different wavelength ranges, as well as of fundamental and applied scientific and technical research.

Eduard Heis, an early pioneer in meteor research

Abstract. At the beginning of the 19th century, meteor observations were not well established. One of its pioneers, who observed meteors on a regular basis, was Eduard Heis in Münster, Germany. We summarise the life of this scientist. Besides his main task of teaching mathematics in Aachen and Münster, he observed atmospheric phenomena and variable stars with exceptional perseverance. He was an editor of Wochenschrift für Astronomie and contributed to the circulation of astronomical reports and knowledge. We focus on his contributions to meteor astronomy, in which he predated the work of Schiaparelli by 30 years.

A spectroscopy pipeline for the Canary island long baseline observatory meteor detection system

We demonstrated the capability of the updated Canary Island Long Baseline Observatory (CILBO) meteor detection system to measure relative elements intensities of meteors. Meteor spectra provide valuable information on the chemical properties of individual meteoroids. In some cases, this may be the only information on the chemical composition of the parent bodies, and on transforming processes that occur during the meteoroid’s journey from its source to Earth. The CILBO spectroscopic program has been created with the intention of carrying out regular systematic spectroscopic observations. At the same time, the meteoroid trajectory and pre-atmospheric orbit are independently measured from data collected by the other cameras in the network. We presented the meteor spectroscopy pipeline developed by the Meteor Research Group of the European Space Agency, and it’s application to the spectroscopic survey of Geminid meteor shower observed by CILBO.

Development of meteor astronomy at the Odessa University during the period of Ukraine's independence

The article using the methods of bibliographic and source study analysis and systems approach highlights the state and main trends in the development of meteor astronomy in Odessa during the time of independent Ukraine. At the beginning of the 21st century, continuous meteor patrol was restored at the Odessa Astronomical Observatory, which was intensively conducted at the Observatory during Soviet times. It was based on the use of the television and telescopic method, which was used in the CIS for the first time. The advantages of using the television telescopic method in comparison with the photographic and radar methods for solving the fundamental problems of meteor astronomy are noted. The text gives valuable information on the features of continuous meteor patrols at the observation station Kryzhanovka and the work of the expeditionary automatic meteor patrol on Snake Island (Odessa region, Ukraine). The methods of conducting telescopic television observations and processing observational material developed by Odessa researchers are considered. The main directions of meteoric studies conducted in the Odessa Astronomical Observatory using television meteor patrol materials were determined. Studying the physics of meteoric phenomena, obtaining exact coordinates of individual meteor radiant, spectral observations of meteors, studying double and multiple meteors, studying the structure and density of meteoric dust particles, solving interaction problems meteor showers with the Earth’s atmosphere, statistics of meteor phenomena in the Earth’s atmosphere are the main directions of meteoric studies of Odessa Astronomical Observatory. The scientific potential of Yu. M. Gorbanev in the field of meteor astronomy of, the leader of the meteoric group, O. V. Holubaieva, the head of the meteor's television patrol at the Kryzhanovka observation station in 2003-2011, as well as participation in the meteor research S. H. Kimakovskyi, I. I. Kimakovskyi, S. V. Podlesniak, I. A. Stognieieva, L. A. Saresta, A. F. Prinzykov, V. A. Shestopalov, etc are noted. Conclusions are drawn about the importance of conducting meteoric research for the development of fundamental and applied science.

Meteor Sky in Time-Domain Astronomy

AbstractMulti-wave astronomy provides a means for researchers to see and ‘hear’ the sky. But that is only part of their perception of the cosmos. The hot handshake of the Universe in the form of a meteor substance burning in the Earth’s atmosphere, sometimes with the precipitation of meteorites threatening the environment, occurs every second. A major present challenge for meteor research is organizing observations and processing existing and new data in order to obtain information in the time domain of meteor astronomy for solving special problems. This poster discusses the concept of the meteor sky, and some approaches for constructing models of it. The database of meteors of Kharkiv National University of Radio Electronics was used.

Present State and Prospects for the Meteor Research in Ukraine

AbstractODESSA. Systematical study of the meteor events are being carried out since 1953. In 2003 complete modernization of the observing technique was performed, and TV gmeteor patrolh on the base of WATEC LCL902 cameras was created. @ wide variety of mounts and objectives are used: from Schmidt telescope F = 540 mm, F/D = 2.25 (field of view FOV = (0.68x0.51) deg, star limiting magnitude SLM = 13.5 mag, star astrometric accuracy 1-2 arcsec) up to Fisheye lenses F = 8 mm, F/D = 3.5 (FOV = (36x49) deg, SLM = 7 mag). The database of observations that was collected between 2003 and 2012 consists of 6176 registered meteor events. Observational programs on basis and non-basis observations in Odessa (Kryzhanovka station) and Zmeiny island are presented. Software suite of 12 programs was created for processing of meteor TV observations. It enables one to carry out the whole cycle of data processing: from image preprocessing up to orbital elements determination. Major meteor particles research directions: statistic, areas of streams, precise stream radiant, orbit elements, phenomena physics, flare appearance, wakes, afterglow, chemistry and density. KYIV. The group of meteor investigations has been functioning more than twenty years. The observations are carried out simultaneously from two points placed at the distance of 54 km. Super-isocon low light camera tubes are used with photo lens: F = 50mm, F/D = 1.5 (FOV = (23.5 x 19.0) deg, SLM = 9.5 mag), or F = 85, F/D = 1.5 (FOV = (13x11) deg, SLM = 11.5 mag). Astrometry, photometry, calculation of meteor trajectory in Earth atmosphere and computation of heliocentric orbit are realized in developed gFalling Starh software. KHARKOV. Meteor radio-observations have begun in 1957. In 1972, the radiolocation system MARS designed for automatic meteor registration was recognized as being the most sensitive system in the world. With the help of this system 250 000 faint meteors (up to 12 mag) were registered between 1972 and 1978 (frequency 31.1 MHz, particle masses 10−3 ~ 10−6 g). Simultaneously, millions of reflections were registered for even fainter meteors (up to 14 mag). Information about 250 000 meteors and 5160 meteor streams is included in database. This is an unique material that can be used for hypotheses testing, as well as for creation new theories about meteor phenomena. Models of the meteor matter distribution in the Earthfs atmosphere, near-Earth space and in the Solar system, influence on surface of spacecrafts were developed. NIKOLAEV. The optical and radio observations of meteors have begun in 2011. Two WATEC LCL902 cameras are used with photo lens F = 85 mm, F/D = 1.8 (FOV = (3.2x4.3), SLM = 12 mag, star astrometric accuracy 1-6 arcsec). Original software was developed for automatic on-line detection of meteor in video stream. During 2011 year 105 meteor events were registered (with angular length (0.5-4.5) deg and brightness (1-5) mag). Error of determination of the meteor trajectory arc ~ (10-12) arcsec. Error of determination of the large circle pole of the meteor trajectory is ~ (3-13) arcmin. In the radio band observations of meteors are performed by registration of signal reflected from the meteor wake. As a signal source the over-the-horizon FM station in Kielce (Poland) is used. Narrow-beam antenna, computer with TV/FM tuner and audio recording software are used to perform radio observations. Original software was developed for automatic detection of meteor in audio stream.

The Meteors, Meteoroids and Interplanetary Dust Program of the International Heliophysical Year 2007/9

Under the title ‘Meteors, Meteoroids and Interplanetary Dust’, meteor research is included in the program of the International Heliophysical Year 2007/9.We list issues for coordinated meteor research within the framework of this global international program.

전천 카메라를 이용한 2001 사자자리 유성우 관측: 1. 유성 등급 분포

2001년 사자자리 유성우는 수십년 이래 최대 빈도로 많은 유성이 발생하여 전세계적으로 관측되며 많은 관심을 불러 일으켰다. 특히 유성우 극대기 시간이 동아시아의 11월 19일 새벽으로, 달의 위상과 보현산의 날씨가 관측하기에 최적인 조건을 보였다. 본 논문은 보현산 천문대에 고층대기 관측용으로 설치된 전천 카메라를 이용해서 유성우 극대기가 예측된 2001년 11월 19일 01:00∼05:40(KST)동안 관측한68장의 전천 화상을 분석하였다. 이 기간 동안 전천 화상에 모두 172개의 유성이 기록되었다. 이 관측 개수에 International Meteor Organization에 육안 관측으로 보고된 천정 시간율(Zenith Hourly Rate, ZHR), 3000과 등급 분포 지수, 2를 적용하면, 전천 화상에 나타난 유성의 한계 등급이 약 3등급으로 추정된다. 이 중 화상 밝기가 분명한 83개의 유성에 대해 근처 표준성의 자기와 비교하여 등급을 결정하였다. 이 때 유성 통과 시간의 계산에 필요한 유성의 각속도는 유성 진입의 기하학적 성질을 이용하여 유성과 사자자리 방사점과의 사이각을 변수로 하는 간단한 식으로 유도하였다. 이렇게 결정된 83개의 유성이 -1∼-6등급 사이에 분포하며, -3등급 근처에서 최대를 보인다. 그러나 이 등급 분포는 육안 관측과 비교하여 추정한 전천 카메라의 한계 등급보다 상당히 작은(밝은) 범위에 있다. 이런 차이는 순간적인 육안 관측과 노출시간이 긴 CCD 관측과의 특성 차이에 기인하는 것으로 판단된다. 이 특성 차이를 분석하기 위해 육안 관측과 합치하도록 유성 지속 시간을 조절 변수로 하여 등급을 재결정하였다. 재결정된 등급의 상대적 분포는 원리적으로 결정한 등급 분포와 유사하며, 약 0등급 근처에서 최대를 가진다. 이 상대 분포는 육안 관측에 민감한, 희미한(1∼6등급)유성들이 등급이 감소함에 따라 일률적으로 개수가 감소하는 것과는 상당히 다른 분포이다. 따라서 우리의 관측 결과는 2001년 사자자리 유성우의 극대 시간 전후 2시간에 적어도 0등급 이하의 밝은 유성이 상대적으로 많이 발생하였을 것으로 해석된다. 이런 밝은 유성의 빈도는 유성우 특성 연구에 중요한 의미를 가진다. 그러나 표준성만을 이용해 결정된 유성 등급은 유성의 지속 시간에 대한 불확실성과 전천 카메라 감응도의 비선형성에 의한 불확실성을 내포하고 있음을 지적해 둔다. The 2001 Leonid meteor storm has been observed all over the world, and its most intense flux since the last few decades has caused great interest among both laymen and experts. Especially, its maximum hours occurred at dawn hours of Nov. 19 in the east Asia, during which moonless clear night at the Mt. Bohyun allowed us near perfect condition of observation. Observation was carried out in the period of 01:00∼05:40(KST), which include the predicted maximum hours, with all-sky camera installed for upper atmospheric airglow research. Tn this paper we analyze 68 all-sky images obtained in this period, which contain records of 172 meteors. Utilizing the zenith hourly rate(ZHR) of 3000 and magnitude distribution index of 2, which were reported to International Meteor Organization by visible observers in the east Asia, we estimate the limiting magnitude of about 3 for meteors detected in our all-sky images. We then derive magnitudes of 83 meteors with clear pixel brightness outlines among the initially detected 172 meteors by comparing with neighbor standard stars. Angular velocities of meteors needed for computing their passing times over an all-sky image are expressed with a simple formula of an angle between a meteor head and the Leonid radiant point. The derived magnitudes of 83 meteors are in the range of -6∼-1 magnitude, and its distribution shows a maximum new -3mag. The derived magnitudes are much smaller than the limiting magnitude inferred from the comparison with the result of naked-eye observations. The difference may be due to the characteristic difference between nearly instantaneuous naked-eye observations and CCD observations with a long exposure. We redetermine magnitudes of the meteors by adjusting a meteor lasting time to be consistent with the naked-eye observations. The relative distribution of the redetermined magnitudes, which has a maximum at 0 mag., resembles that of the magnitudes determined with the in-principle method. The relative distribution is quite different from ones that decrease monotonically with decreasing magnitudes for meteors(1∼6) sensitive to naked-eye observations. We conclude from the magnitude distribution of our all-sky observation that meteors brighter than about 0 mag., appeared more frequently during the 2001 Leonid maximum hours. The frequent appearance of bright meteors has significantly important implication for meteor research. We noted, however, considerably large uncertainties in magnitudes determined only by comparing standard stars due to the unknown lasting time of meteors and the non-linear sensitivity of all-sky camera.

The selectope for games with partial cooperation

In this paper we define and study some solution concepts for games in which there does not have to be total cooperation between the players. In particular, we show the relations of these solution concepts with the selectope. In this way, we extend the work of Derks, Haller and Peters, METEOR Research Memorandum, Maastricht, RM/97/016 (revised version, 1998).

Recent studies of meteors in South Africa

Recent meteor research in South Africa, arising largely from the development of forward and back scatter observing systems, is briefly reviewed. The main areas of investigation have been the use of single station radars to deduce meteor radiant structures, the study of upper atmospheric wind patterns, and research into the factors which influence the performance of meteor burst communication systems.

Very Wide-Field Monitoring of the Sky

There is a need for very wide-field monitoring of the sky in several branches of astronomy and astrophysics, ranging from meteor research to monitoring of optical transients and counterparts to gamma ray burst sources. The photographic very wide-field monitoring of the sky is run at the Ondřejov Observatory and other stations of the Czech Meteor Network and is sensitive enough to record stars up to 11 mag on 3–4 h exposures or 1-s flashes up to 3.0 mag over a field-of-view of 180 deg. diameter. A CCD device for very wide-field monitoring is also in development with sensitivity of 5.0 mag for 1-s flashes (and 10 mag for stars with 100 s exposure) over a field-of-view of 50 × 60 degrees. Both systems are briefly described and discussed.

Detection by HF radar of the Eta Aquarid meteor shower

Frequencies in the HF band below 15 MHz have in the past been little used for radar meteor research owing to the requirement for large antenna arrays and the confusion which may be presented by ionospheric echoes. However, radars employing such frequencies are potentially able to detect very many more underdense meteor echoes than are radars operating at the more conventional higher frequencies, above about 20 MHz. This occurs as a consequence of the greater limiting height for the detection of echoes at longer wavelengths which is set by the so-called underdense echo ceiling. The successful observation of the Eta Aquarid meteor shower reported below demonstrates the value of HF skywave radars operating at frequencies below 15 MHz for meteor detection. The results are consistent with the shower radiant having a diameter of about 6° centred on R.A. = 339°, Dec = 0°. If the cumulative distribution of meteoroidal particles exceeding a lower threshold mass m is described by a power law of the form N( m) ∼ m c , where the exponent c is assumed to equal −1.0 for sporadic meteors then, by comparison, the particles of the Eta Aquarid shower must belong to a flatter distribution with c in the range from −1.0 to −0.6.

Growth and decline of a scientific speacialty: The case of radar meteor research

This article traces the rise and eventual decline of a field of research devoted to the study of meteors by radar. It shows how a new experimental tool, radar, provided the impetus for the emergence of a new scientific specialty, and how this specialty later declined after its initial problems had been solved and after most of its participants had moved on to more promising fields. Radar meteor research provides an example of how new fields grow and how scientific developments affect the research careers of scientists.

10. Spectral studies of meteors at the tokyo astronomical observatory

Our program of meteor research has been changed since November, 1963, by introducing spectral photography at the Dodaira branch station of the Tokyo Astronomical Observatory, in addition to the direct photography at the Mitaka Station. Observations at these two stations are basic, and they have been supplemented in case of need by observations at the temporary station at Tatebayashi, situated about 40 km Northeast of Dodaira. Double- or triple-station observations were carried out mainly during the active period of the major streams, such as Quadrantids, Perseids, Leonids or Geminids, with the purpose of the dynamical and physical studies of meteors. The coordinates of these three stations are as given in Table 1.

The Harvard photographic meteor programme

The article is a description of current meteor research by the Harvard Observatory, using the new Baker-Super-Schmidt meteor cameras (aperture 12 in., focal length 8 in.) in New Mexico. The research involves the improvement of basic meteor theory, the determination of winds and other characteristics of the upper atmosphere, and the basic problems of the nature and origin of meteoritic material in the solar system.

Results of Rocket and Meteor Research *

Results are presented of rocket and meteor research in the upper atmosphere during the past three years. Both methods have been valuable in determining the pressures, densities and temperatures in the upper atmosphere and variations with time and place above an altitude of 30 km. The basic atmospheric data are now rather well determined to 130 km over New Mexico. Knowledge of the composition of the atmosphere to 72 km depends solely upon rocket sampling techniques. A great deal of information has been obtained from the rocket measures concerning radiation from the sun in the far ultraviolet to wavelength about 800 Å and in the soft X-ray region below 20 Å. A considerable section of the paper is devoted to the question of micro-meteorites, their existence and effect on the upper atmosphere. In addition, three Appendixes include some more recent information concerning temperatures and composition of the upper atmosphere and concerning high-frequency solar radiation.