The orbital elements of a meteoroid after its ejection from a comet.

Details The orbital elements of a meteoroid after its ejection from a comet. The orbital elements of a meteoroid after its ejection from a comet.

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...317..594p&link_type=abstract

Astronomy and Astrophysics, v.317, p.594-600

Astronomy and Astrophysics

Astrophysics

6

Solar System: Comets, Meteors, Meteoroids

Scientific paper

This article examines the changes in the orbital elements of particles ejected from the nucleus of an active comet. We extend the work of Plavec (1957PAICz..30...93P) to include changes in all the orbital elements resulting from the ejection process. We take into account the constraints that must be met before a meteoroid particle can be observed as a meteor. In addition we constrain particle ejection to take place only on the sun-ward hemisphere of the cometary nucleus and only when the comet is less than 1.88 AU from the Sun. For a given true anomaly of the ejection event, our equations allow the determination of the speed and direction of the ejected particle. Using the ejection of particles from comet P/Swift-Tuttle, we applied our approach in an attempt to explain whether or not a new filament of activity first seen in 1986 could be attributed to particles ejected from the comet near the time of its 1862 perihelion passage. Observed Perseid meteor rates in 1986 - 1995, expressed as a function of the solar longitude, cannot be used to uniquely determine the time the corresponding particles were ejected from the parent comet.The observed meteor shower activity could have been caused by particles that were ejected from the nucleus at a variety of times, velocities and ejection angles.

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