Leonid Radiant Project 2001

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McNaught and Asher (2001) predicted the precise positions ofradiant points due to the4-rev (1866 yr.) and 9-rev (1699 yr) dust trails of the Leonids. To establish the dust trail theoryand to measure the flux and magnitude distribution of faint meteors, we performed telescopicobservations with the CCD camera, obtaining the high-resolution dust trail structure from thedeep imaging of the radiant point. 7 sites in Japan performed such coordinated observations; (i)Akeno observatory, (ii) RIBOTS at Bisei observatory; (iii) RIMOTS at Miyazaki Univ., (iv) Kisoobservatory, (v) KSC Schmidt, (vi) Miyazaki Univ., (vii) NAOJ Mitaka. We observed the Leonidsmeteor storm Nov.18 2001, and succeeded to separate the radiant points due to the 4-rev and9-rev dust trails. We also succeeded to detect the faint meteors under 10 magnitude. This paperdescribes the detailed observation circumstances and presents a highlight of preliminary results.Mainly, we report the distribution of faint meteors from 7th to 12th magnitude combining the dataof each sites. The cumulative flux of faint meteors is exponential growth with the index numberof 2.0, and the flux (4.2 ± 2.1) x l0-4km-2s-2(mag≦ +12). We have found no apparent cutoff inthe magnitude range brighter than 〜12 mag.
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