Abstract
Observations of the Perseid meteor stream in the period 1987–1994 were characterized by an appearance of a new filament the maximum activity of which was found near solar longitude L ⊙ = 138.9° (eq. 1950.0). Its activity culminated in 1993 while 1991 and 1995 observations showed no abnormal increase of meteors in that region. The mass distribution within the new filament has been studied in the interval 138.62° ⩽ L ⊙ < 139.10° during the period of its activity and compared with analogous results from 1958–1986, 1991, and 1995 within the same L ⊙ interval. The mass distribution indices, s, for overdense radio-meteor echoes associated with the new filament show slightly lower values comared with those determined during the activity of the regular stream.
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