Galligan and Baggaley [4] introduce a method of detecting, and testing the significance of, shower structure in the ~ 5 x 105 meteoroid orbit data set provided by the amor system [2] from 1995 to mid-1999, amor is a particularly sensitive system with a limiting meteoroid size of ~ 40 /im; it is expected that many meteoroids having sizes close to this limit will have no detectable shower affiliation owing to the higher mass distribution index expected for showers relative to that of the non-shower background.

The four year data set is formed into a virtual equinoctial year stretching between vernal equinoxes with time measured in terms of the mean solar longitude (A0). (All angular parameters are here referred to the J2000.0 equinox.) Partitioning based on overlapping geocentric speed (VG) ranges and sliding windows in time is applied as discussed in Galligan and Baggaley [4], Wavelet enhancement of the resultant meteor radiant position distributions in the antihelion, helion and apex apparent source regions is found to be useful in probing the sparse structure.

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