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Astron. Astrophys. 357, 777-781 (2000)

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5. Conclusions

We can deduce from our observations during previous returns of Leonid meteor shower that both in 1965 and 1966 years the peak activity was observed at almost the same solar longitude near [FORMULA]. The activity pattern in 1965 showed two well pronounced peaks separated by 23 hours where the second one appeared to be the principal. This is true both with respect to activity as well as the flux. Our observations indicate that the main outburst of this Leonid return occurred in 1966 the activity ratio to 1965 was 1.2 while the corresponding ratio in fluxes was 3.7. Since the maximum activity peak in 1966 was deduced from an uncertain correction for high [FORMULA] we suggest that the latter value is closer to reality. The 1967 activity is characterized by a large scatter of observed hourly echo counts fluctuating around 15 which is slightly above the level in intermediate years of Leonid activity (Brown et al. 1997). We confirmed that single station observation of the Leonid shower limited to the period when the radiant is above the horizon cannot yield a complete picture of the activity pattern. Organization of international Leonid watch during the 1999 return promised a better picture of the stream.

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© European Southern Observatory (ESO) 2000

Online publication: June 5, 2000