Meteors and Meteor Streams

Unusually long activity of the Taurid meteor complex, extending over 3-5 months according to new estimations based on various orbital similarity criteria, has been evoking controversies about the possible origin and dynamical evolution of this unique complex of meteor streams. It even casts doubts on the reality of the extension of the complex. In the present paper orbital elements and the extension of the Taurid meteor complex are re-examined on the bases of the most precise photographic meteor orbits available from the IAU Meteor Data Center in Lund. The results are evaluated and discussed from the viewpoint of various proposals on the origin and dynamical evolution of the complex.

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On the Production of Meteor Streams by Cometary Nuclei

Symposium - International Astronomical Union ◽

10.1017/s0074180900006999 ◽

1972 ◽

Vol 45 ◽

pp. 498-502

Author(s):

L. A. Katasev ◽

N. V. Kulikova

Keyword(s):

Monte Carlo ◽

Cometary Nucleus ◽

Cometary Nuclei ◽

Meteor Streams ◽

Monte Carlo Techniques

An attempt is made to use Monte-Carlo techniques to model the process of formation of meteor streams. It is supposed that meteor streams are formed as the result of ejection of meteoroids from a cometary nucleus at perihelion. Possible ejection velocities are determined for the Draconids, Perseids, Leonids, and Taurids. In general the values do not exceed 100 m s-1. The data obtained can also be used to estimate the ages of the streams.

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Lifetime of Meteor Streams Associated with Comet Halley

International Astronomical Union Colloquium ◽

10.1017/s0252921100067051 ◽

1991 ◽

Vol 126 ◽

pp. 323-326

Author(s):

M. Hajdukova ◽

A. Hajduk

Keyword(s):

Mass Loss ◽

Structural Features ◽

Critical Examination ◽

Meteor Showers ◽

Orbital Parameters ◽

Loss Process ◽

Meteor Streams ◽

Flux Data ◽

Large Particles ◽

Comet Halley

AbstractCritical examination of the orbital parameters of particles ejected from comet Halley rejects the low age hypotheses for meteor showers associ- ated with the comet. The diffusion of the orbits of large particles is too slow for explaining the observed structural features of the stream. The mass-loss process as derived from space observations compared with the mass of the stream of particles deduced from flux data lead to comet lifetimes of the order of 105years.

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The formation and evolution of meteor streams

International Astronomical Union Colloquium ◽

10.1017/s0252921100083846 ◽

1985 ◽

Vol 83 ◽

pp. 115-127

Author(s):

I.P. Williams

Keyword(s):

Radiation Pressure ◽

Physical Processes ◽

Meteor Streams ◽

Formation And Evolution

AbstractThe physical processes which may affect the evolution of meteor streams are discussed and a review is then given of the work carried out to date on the evolution of meteor streams. It is clear that they evolve principally due to the effect of planetary perturbations and radiation pressure. The formation of streams from the breakup of a comet is also discussed. All the evidence, including the recent, discovery of 1983TB points to the correctness of this hypothesis.

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Physical Processes in Cometary Atmospheres

Symposium - International Astronomical Union ◽

10.1017/s0074180900006604 ◽

1972 ◽

Vol 45 ◽

pp. 253-259 ◽

Cited By ~ 1

Author(s):

A. Z. Dolginov

Keyword(s):

Rotation Period ◽

Dust Particles ◽

Molecular Flow ◽

Physical Parameters ◽

Charged Dust ◽

Nuclear Surface ◽

Cometary Dust ◽

Meteor Streams ◽

Cometary Tail ◽

Dust Component

Formulae are obtained for the distribution of molecules in the cometary head, taking into account the conditions of hydrodynamic and free molecular flow in various regions around the nucleus. Experimental data are used to derive physical parameters near the nuclei of comets 1952 III, 1955 V, 1957 III, and 1960 II and the rate of decrease of mass. The possibility of chemical reactions in the region close to the nucleus is discussed. Gas condensation is shown to be a possible cause of dust formation under the conditions existing near the nucleus, and this process may be responsible for the major portion of the cometary dust component. The observed grouping of synchrones in the cometary tail can be explained on the assumption that the nuclear surface comprises two (or more) areas differing essentially in evaporation rate, the amount of matter ejected varying over the rotation period of the nucleus. Charged dust particles are shown to form, with electrons and ions, a common medium, i.e., dust plasma, which can be treated by the same methods used for ordinary plasma. Special investigations appear to be desirable when comets intersect meteor streams.

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