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4.9 On the Structure of Hyperbolic Interplanetary Dust Streams

Published online by Cambridge University Press:  12 April 2016

L. Kresák  and
E.M. Pittich
L. Kresák
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, Bratislava, Czechoslovakia
E.M. Pittich
Affiliation:
Astronomical Institute, Slovak Academy of Sciences, Bratislava, Czechoslovakia

Extract

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The only type of concentration of cometary dust with a reasonable probability of being detected by deep-space probes, are the dust tails emanating from passing comets. Essentially all the dust released from long-period comets leaves the solar system on hyperbolic orbits, because the radiation pressure limit is high (corresponding to centimetre-sized grains emitted in the vicinity of the Earth’s orbit by comets of the Oort’s Cloud). For the short-period comets the dynamical conditions for retention of emitted particles within the solar system are much more favourable, but those which remain in circumsolar orbits tend to disperse rather rapidly (Kresák, 1976a).

Type
4 Meteors and their Relation to Interplanetary Dust
Information
International Astronomical Union Colloquium , Volume 31: Interplanetary Dust and Zodiacal Light , 1976 , pp. 396 - 399
Copyright
Copyright © Springer-Verlag 1976

References

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