Mathematical modelling of the Geminid meteoroid stream

Ryabova, G. O.

doi:10.1111/j.1365-2966.2007.11392.x

Cited by 54 publications

(58 citation statements)

References 11 publications

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“…This has been noted before (e.g., Williams & Wu 1993). Several authors studied the possibility of a recent formation of the Geminids stream, including that near 0 AD when the perihelion had its last minimum (see, e.g., Ryabova 2007 or; for a more detailed overview, Jenniskens 2006). However, a detailed match of the observed activity of Geminids over years may require particle feeding over an extended interval of time (Jewitt et al 2015).…”

Section: Orbital Evolutionmentioning

confidence: 76%

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

100

110

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Context. The near-Earth asteroid (3200) Phaethon is an intriguing object: its perihelion is at only 0.14 au and is associated with the Geminid meteor stream. Aims. We aim to use all available disk-integrated optical data to derive a reliable convex shape model of Phaethon. By interpreting the available space-and ground-based thermal infrared data and Spitzer spectra using a thermophysical model, we also aim to further constrain its size, thermal inertia, and visible geometric albedo. Methods. We applied the convex inversion method to the new optical data obtained by six instruments and to previous observations. The convex shape model was then used as input for the thermophysical modeling. We also studied the long-term stability of Phaethon's orbit and spin axis with a numerical orbital and rotation-state integrator.Results. We present a new convex shape model and rotational state of Phaethon: a sidereal rotation period of 3.603958(2) h and ecliptic coordinates of the preferred pole orientation of (319 • , −39 • ) with a 5 • uncertainty. Moreover, we derive its size (D = 5.1 ± 0.2 km), thermal inertia (Γ = 600 ± 200 J m −2 s −1/2 K −1 ), geometric visible albedo (p V = 0.122 ± 0.008), and estimate the macroscopic surface roughness. We also find that the Sun illumination at the perihelion passage during the past several thousand years is not connected to a specific area on the surface, which implies non-preferential heating.

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Section: Orbital Evolutionmentioning

confidence: 76%

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

100

110

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“…Assuming an albite diffusion coefficient, meteoroids smaller than 200 − 100 μm will lose 90% of the initial sodium content after 1000−4000 years, which is the probable age of the Geminid stream (e.g. Ryabova, 2007;Beech, 2002;Williams and Wu, 1993;Gustafson, 1989). Using an orthoclase diffusion coefficient, 90% sodium loss occurs in bodies smaller than 30−60 μm.…”

Section: Results For Geminidsmentioning

confidence: 99%

Quantitative model of the release of sodium from meteoroids in the vicinity of the Sun: Application to Geminids

Čapek

Borovička

2009

Icarus

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International audienceA considerable depletion of sodium was observed in Geminid meteoroids. To explain this phenomenon, we developed a quantitative model of sodium loss from meteoroids due to solar heating. We found that sodium can be lost completely from Geminid meteoroids after several thousands of years when they are composed of grains with sizes up to ∼100 μm. The observed variations of sodium abundances in Geminid meteor spectra can be explained by differences in the grain sizes among these meteoroids. Sodium depletions are also to be expected for other meteoroid streams with perihelion distances smaller than ∼0.2 AU

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“…Williams & Ryabova (2011) have discussed their influence on the structure of meteoroid streams, and demonstrated that the dominant process depends on the stream and thus, for the stream models, it is important to consider both the initial processes of formation and the subsequent gravitational perturbations. There have not been any close encounters significantly affecting the Geminids' orbits during at least the last ten thousand years (Ryabova, 2007), so the initial structure caused by the ejection process should still be traceable in the stream. The deviations which may have accumulated since the formation of the stream can hardly exceed a few thousandths in 1/a (Kresáková, 1974).…”

Section: Models Versus Observationsmentioning

confidence: 99%

Meteoroid orbits from video meteors. The case of the Geminid stream

Hajduková

Koten

Kornoš

et al. 2017

Planetary and Space Science

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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.Except for the measurement errors which influence the analyses and their interpretations, we also point out the problem of the uncertainties of the numerical integration procedures that influence the simulations' results. Several experimental integrations of the Geminids parent asteroid, which we performed from the present to the past and then back to the year 2015, showed that a complete reproduction, including also the mean anomaly, is only possible for a time span of about 2700 years.

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Mathematical modelling of the Geminid meteoroid stream

Cited by 54 publications

References 11 publications

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Quantitative model of the release of sodium from meteoroids in the vicinity of the Sun: Application to Geminids

Meteoroid orbits from video meteors. The case of the Geminid stream

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