The structure of the Leonid meteor stream was studied using the IAU MDC Photographic Orbits Database. Two notable peaks of activity of photographic Leonids were identified at λ⊙ = 234.5° and λ⊙ = 235.5°. Two smaller peaks were tentatively found at λ⊙ = 236.6° and λ⊙ = 235.9°. The first identified peak of the shower activity is formed merely by the meteors observed in the year 1998; the second one is composed mainly of Leonids observed in the years 1998 and 1999. The smaller peaks of activity are formed by the meteors observed in the years 2001 and 2002. The peaks of activity of three different types of meteors - photographic, visual, and radar as well, were in the year 1999 observed almost at the same solar longitude. This feature of the Leonid trail which caused the 1999 shower is in contrast to many other meteor streams (e.g. Orionids) that are characterized by a shift in the peak of activity depending on the mass of recorded meteoroids. In a comparison with other showers with comparable numbers of meteors listed in the IAU MDC database, the Leonids seems to have an incomparable inner structure. Each of six identified associations of orbits is composed of meteors observed mainly in one individual year. Declination of two associations composed of meteors observed mainly from 1999 does not fit the theoretical trend of the daily motion of the radiant. The results confirm the observation of a spatially separated dust trail of Leonids in 1999.