The Lyrid Meteor Stream: Orbit and Structure

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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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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The Micrometeoroid in the Upper Atmosphere

International Astronomical Union Colloquium ◽

10.1017/s0252921100067002 ◽

1991 ◽

Vol 126 ◽

pp. 303-306 ◽

Cited By ~ 1

Author(s):

F. Kamijo

Keyword(s):

Deep Sea ◽

Initial Velocity ◽

Upper Atmosphere ◽

Meteor Stream ◽

Secondary Particles ◽

Radius Variation ◽

Gas Molecules

AbstractThe temperature and the radius variation of micrometeoroids in the thermosphere and the mesosphere are calculated theoretically. If the radius and the initial velocity are 100μm and 30 km/sec respectively, the evaporation height and the velocity coincide almost exactly with those of the Capricornids and the Virginids from the meteor stream observation.Moreover, it is shown that the not evaporated debris till the end of the sublimation may become spherules in the bottom of deep sea; and that fluffy micrometeoroids (10μsize) floating in the stratosphere are also consistent with our calculation.The recondensation and the coagulation of the evaporated gas molecules from the meteoroid are also calculated, and it is shown that these secondary particles are very small and few.

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