The Canadian Meteor Orbit Radar Meteor Stream Catalogue

At the present time the orbit of the Quadrantid meteor stream not only intersects the orbit of Earth but also passes very close to the orbit of the planet Jupiter. This causes considerable perturbations. In a series of three papers (1,2,3) the authors replaced the myriad of meteoroids in the stream by ten test particles set at equal intervals of eccentric anomaly around the orbit. The equations of motion of these particles in the solar system were solved using a standard fourth order Runge–Kutta technique with self–adjusting step lengths. The orbits of the test particles were output at ten year intervals going back from the present to the year 300 B.C. and forward into the future to the year A.D. 3780.

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The Influence of the Atmosphere on Radar Meteor Rates

Symposium - International Astronomical Union ◽

10.1017/s0074180900066547 ◽

1980 ◽

Vol 90 ◽

pp. 101-104

Author(s):

W.G. Elford.

Keyword(s):

Initial Diameter ◽

Meteor Trail ◽

Radio Studies ◽

The Difference ◽

Sporadic Meteors ◽

Radar Meteor ◽

Sharp Cutoff ◽

Selection Of

The majority of radio studies of meteors have been carried out at frequencies higher than 17MHz and most of the rate observation at frequencies above 30MHz. At these frequencies a severe height selection of meteors occurs. In Figure 1(a) are shown the normalized height distributions of sporadic meteors observed at Adelaide on frequencies of 27MHz and 2MHz (Brown, 1976). The sharp cutoff of the latter distribution below 87 km is instrumental. The difference in the height distributions is due to the effect of the finite diameter of a meteor trail on its radar detectability. If the trail diameter is ≪ λ signals from the near and far edges reinforce but as the trail expands due to diffusion and the diameter becomes ≃ λ/4, interference reduces the amplitude. A meteor trail, produced by a particle with a velocity of 30 km s−1, has an initial diameter of 0.4m at 80 km, 2.0m at 104 km and 4.0m at 116 km.

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The Lyrid Meteor Stream: Orbit and Structure

Advances in Meteoroid and Meteor Science ◽

10.1007/978-0-387-78419-9_14 ◽

2008 ◽

pp. 91-94

Author(s):

Vladimir Porubčan ◽

Leonard Kornoš

Keyword(s):

Meteor Stream

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Modelling the Ejection of Meteoroids from Comets

International Astronomical Union Colloquium ◽

10.1017/s0252921100501432 ◽

1996 ◽

Vol 150 ◽

pp. 137-140

Author(s):

J. Jones ◽

P. Brown

Keyword(s):

Active Area ◽

Adiabatic Expansion ◽

Process Change ◽

Meteor Stream ◽

Spherical Cap ◽

Ejection Process

AbstractWe have reworked Whipple's (1951) theory of the ejection of meteoroids from comets to include the effects of cooling by the sublimation of the cometary ice and the adiabatic expansion of the escaping gases. We consider only those particles moving significantly slower than the gas speed and find that the inclusion of these effects does not yield results much different from Whipple's theory. We have extended the theory to include the case of an active area in the form of a spherical cap and have shown how the characteristics of the ejection process change when the cap is in the form of a pit or a depression. We present a empirical formulae which should be useful to modellers of meteor stream evolution.

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The connection between comet P/Machholz and the Quadrantid meteor stream

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/254.4.627 ◽

1992 ◽

Vol 254 (4) ◽

pp. 627-634 ◽

Cited By ~ 25

Author(s):

R. Gonczi ◽

H. Rickman ◽

C. Froeschle

Keyword(s):

Meteor Stream

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The orbital evolution of meteor streams at the 2/1 resonance with Jupiter

International Astronomical Union Colloquium ◽

10.1017/s0252921100083895 ◽

1985 ◽

Vol 83 ◽

pp. 179-180

Author(s):

Cl. Froeschlé

Keyword(s):

Major Axis ◽

Orbital Evolution ◽

The Sun ◽

Orbital Elements ◽

Meteor Stream ◽

Semi Major Axis ◽

Meteor Streams ◽

Gravitational Forces ◽

Resonant Effect

We investigated the orbital evolution of Quadrantid-like meteor streams situated in the vicinity of the 2/1 resonance with Jupiter. For the starting orbital elements we took the values of the orbital elements of the Quadrantid meteor stream except for the semi-major axis which was varied between a = 3.22 and a = 3.34 AU. We considered these meteor streams as a ring and we investigated the resonant effect on the dispersion of this ring over a period of 13 000 years. Only gravitational forces due to the Sun and due to Jupiter were taken into account.

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