A Numerical Examination of the Long-Term Coherency of Meteoroid Streams in Near-Earth Orbit

Details A Numerical Examination of the Long-Term Coherency of Meteoroid Streams in Near-Earth Orbit A Numerical Examination of the Long-Term Coherency of Meteoroid Streams in Near-Earth Orbit

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dda....31.0402g&link_type=abstract

American Astronomical Society, DDA Meeting #31, #04.02; Bulletin of the American Astronomical Society, Vol. 32, p.859

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The statement that some small bodies in the Solar System--asteroids, comets, meteors (of cometary origin)--travel in co-orbital streams, would be accepted by planetary scientists without argument. After all, streams have been observed of fragments of at least one comet (Scotti and Melosh, 1993; Weaver et al., 1993), asteroids (Drummond, 1991; Rabinowitz et al., 1993; Binzel and Xu, 1993) and meteoroids of asteroidal origin, like Innisfree (Halliday et al., 1990; cf. Drummond, 1991). Whether members of a stream can be recognized from compositional studies of meteorites recovered on Earth and linked to a common source is more controversial since such linkage would imply variations in the Earth's sampling of extraterrestrial material that persist for tens of Myr. The dates of fall of H chondrites show that many - including Clusters in May, 1855-1895, September, 1812-1831 and Sept.-Oct., 1843-1992 -- apparently derive from specific meteoroids (Lipschutz et al., 1997). Contents of highly volatile elements in these 3 Clusters (selected by one criterion, fall circumstances), when analyzed using multivariate statistical techniques demonstrate that members of each Cluster (i.e. stream) are recognizable by a totally different characteristic criterion: a thermal history distinguishable from those of random H chondrite falls (cf. Lipschutz et al., 1997, for specific references). Antarctic H chondrites with terrestrial ages 50 Myr (Michlovich et al., 1995) also show this. Metallographic and thermoluminescence data for these H chondrites also reflect their thermal histories, and support the existence of such meteoroid streams (Sears et al., 1991; Benoit and Sears, 1993), but cosmogenic noble gas contents do not (Loeken et al., 1993; Schultz and Weber, 1996). Important unanswered orbital dynamic questions are how long a meteoroid stream should be recognizable and what dynamic conditions are implied by Clusters, whose members have cosmic ray exposure ages of some Myr. To begin to address these open issues, we simulate the trajectories of several near-Earth meteoroid streams--some with orbital elements corresponding to suspected streams, others randomly chosen. To integrate the trajectories as accurately as possible, we use an error-optimized modified 13th order Störmer integration scheme, capable of handling close planet/meteoroid approaches (Grazier et al., 1998). Using Drummond's (1979) d' criteria to determine stream membership and coherency as a function of time, we find that stream coherency beyond 100 Ky--certainly beyond 1 My--exists but is rare.

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