Mathematical modelling of the Geminid meteoroid stream (original) (raw)
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A preliminary numerical model of the Geminid meteoroid stream
Monthly Notices of the Royal Astronomical Society
A pilot numerical model of the Geminid meteoroid stream is presented. This model implies cometary origin of the stream. Ejection of relatively small amount of particles (90 000 test meteoroids with masses 0.02, 0.003 and 0.0003 g) from the asteroid (3200) Phaethon (the parent body) was simulated, and their evolution was followed till the present time. The particles close to the Earth orbit were considered as the 'shower'. It was found that the width of the model shower is at least twice less comparatively the real shower. The maximum activity of the model shower is dislocated and occurs about one day late. The most probable reason for both discrepancies is the drastic transformation of the parent body orbit during rapid release of the volatiles in the process of the stream initial formation. The dispersion of the model stream was evaluated in terms of the Southworth-Hawkins D-criterion.
60 years of modelling the Geminid meteoroid stream
A brief historical review of the mathematical modelling of the Geminid mete-oroid stream is given. The 'hollow stream' model by Jones (1985) and '4-showers' model by Babadzhanov and Obrubov (1986) were revised.
Meteoroid streams: mathematical modelling and observations
Proceedings of the International Astronomical Union, 2005
Mathematical modelling of meteoroid streams formation and evolution is a very fruitfull method for obtaining not only cosmogonical knowledges, but information about the stream up-to-date structure as well. In this review we consider advances of the method, and applications to meteoroid streams of different schemes of formation. We also discuss the part played by observations, and feedback between models and observations. Attention is also drawn to some unresolved problems and promising areas of application.
The orbit and evolution of the Geminid meteoroid stream
Il Nuovo Cimento C
The orbit and radiant of the Geminid meteoroid stream based on an analysis of the current version of the IAU MDC catalogue of photographic meteors are studied and discussed. The mean orbit, shape, size and ephemeris of the radiant are derived. The radiant area of the central part of the stream is more concentrated with the densest part of the size of 2°×2°. The orbital evolution of the stream is investigated and compared with the evolution of its potential parent asteroid 3200 Phaethon.
The Dynamics of Meteoroid Streams
2002
Meteors are streaks of light seen in the upper atmosphere when particles from the interplanetary dust complex collide with the Earth. Meteor showers originate from the impact of a coherent stream of such dust particles, generally assumed to have been recently ejected from a parent comet. The parent comets of these dust particles, or meteoroids, fortunately, for us tend not to collide with the Earth. Hence there has been orbital changes from one to the other so as to cause a relative movement of the nodes of the meteor orbits and that of the comet, implying changes in the energy and/or angular momentum. In this review, we will discuss these changes and their causes and through this place limits on the ejection process. Other forces also come into play in the longer term, for example perturbations from the planets, and the effects of radiation pressure and Poynting-Robertson drag. The effect of these will also be discussed with a view to understanding both the observed evolution in some meteor streams. Finally we will consider the final fate of meteor streams as contributors to the interplanetary dust complex.
The Geminid Meteor Stream Activity Profile
2001
The existence of two maxima of the activity of the Geminid meteor stream and the general shape of the stream activity (rate curve) are discussed. The data of visual and radar observations are compared to the results of mathematical simulation. The distribution of the orbits of meteoroids, which are observed on the Earth, is determined from the mathematical model. This distribution cannot as yet be confirmed or disproved because of the absence of appropriate experimental data.
The Evolution of Meteoroid Streams
International Astronomical Union Colloquium
The existence of meteoroid streams is indicated by the regular appearance of coherent meteor activity at specified times during the year. Since it is the interaction of the meteoroid with the atmosphere that is detected, the meteoroid has to be greater than about 100 micrometers in radius. Observation of these interactions gives information on individual meteoroids as well as collective phenomena. It is generally agreed that streams form through the ejection of dust particles from the surfaces of comets and asteroids at speeds considerably lower than the orbital speed. The subsequent motion of these particles is affected by gravitational perturbations from the planets and the effects of solar radiation forces. This review is intended to present an overview of the development of the subject and of our current state of knowledge.
The comet Halley meteoroid stream: just one more model
Monthly Notices of the Royal Astronomical Society, 2003
The present attempt to simulate the formation and evolution of the comet Halley meteoroid stream is based on a tentative physical model of dust ejection of large particles from comet Halley. Model streams consisting of 500-5000 test particles have been constructed according to the following ejection scheme. The particles are ejected from the nucleus along the cometary orbit (r < 9 au) within the sunward 70 • cone, and the rate of ejection has been taken as proportional to r −4 . Two kinds of spherical particles have been considered: 1 and 0.001 g with density equal to 0.25 g cm −3 . Ejections have been simulated for 1404 BC, 141 AD and 837 AD. The equations of motion have been numerically integrated using the Everhart procedure. As a result, a complicated fine structure of the comet Halley meteoroid stream, consisting not of filaments but of layers, has been revealed.
Meteoroid orbits from video meteors. The case of the Geminid stream
Planetary and Space Science, 2017
We use the Slovak and Czech video meteor observations, as well as video meteoroid orbits collected in the CAMS, SonotaCo, EDMOND and DMS catalogues, for an analysis of the distribution of meteoroid orbits within the stream of the Geminids and of the dispersion of their radiants. We concentrate on the influence of the measurement errors on the precision of the orbits obtained from the video networks that are based on various meteordetection software packages and various meteor orbital element softwares. The Geminids radiant dispersion obtained from the large video catalogues reaches the dispersion of the radio observed Geminids, wherby the diffused marginal regions are affected mostly by meteoroids with extreme values (small or large) of the semi-major axes. Meteoroids of shorter semimajor axes concentrate at the eastern side of the radiant area and those of longer semi-major axes at the western part. The observed orbital dispersions in the Geminid stream described by the median absolute deviation range from 0.029 to 0.042 AU −1 for the video catalogues. The distribution of the semi-major axes of video meteors in all the databases, except for the Ondřejov (Czech) data, seem to be systematically biased in comparison with the photographic and radio meteors. The determined velocities of the video data are underestimated, probably as a consequence of the methods used for the positional and velocity measurements. The largest shift is observed in the EDMOND and SonotaCo catalogues.
Earth Moon Planet, 1995
Numerical integration of a meteor stream over a long period is a very time consuming process, especially if a number of different models have to be investigated. In this paper we demonstrate that using the distribution of orbital energy as a vector in a Markov process can be a useful tool and that meaningful results can be obtained with far less computation than is normally required. comet as 1862 III. Fol]owing the recovery of the come as 1992t and the consequent improvement in its orbital elements, Yau, Yeomans and Weissman (1994) identified two earlier observed apparitions of the comet, in AD 188 and 69 BC. They found no evidence for a significant change in the brightness of the comet. Records of the meteor shower also date back to AD 36 though the first good record was probably not until AD 830 (Hasegawa 1993). The alm of this paper is to discuss the very long term general evolution of the Perseid meteoroid stream