COMMISSION 27 OF THE I. A. U.
           INFORMATION BULLETIN ON VARIABLE STARS
                       Number 2740

                                      Konkoly Observatory
                                      Budapest
                                      5 June 1985

                                      HU ISSN 0374 - 0676

              NEW FLARE STAR SVS 2559 PERSEI

 The variability of SVS 2559 was discovered by Kurochkin (Astron.Tsirk.
No. 1325, p. 5; 1984), who already suspected that the object might be a
flare star. His plate material, however, accidentally did not allow to trace
completely one of the eruptions.
 On 343 suitable Sonneberg 40 cm astrograph exposures of the years 1964 to
1983 one conspicuous flare could be detected confirming the UV Ceti type.
It is recorded by two of five plates of a night series of 1971 Oct. 19 as
follows:


         J.D.hel  244 1244.283    16.7mag pg
                          .346    16.7
                          .401    15.1
                          .457    16.4
                          .557    16.7


 As the exposure times of the plates amount to 80 minutes each, the
observed range of the eruption is flattened, by an unknown amount.
 The distribution of brightness data of our material very nearly resembles
that given by Kurochkin (l.c.). We should note that the star is never 
invisible on good plates. Therefore the "faint tail" of the distribution is
supposed not to be caused by observational bias. The comparison stars used
are those of Kurochkin.

 This variable is (besides QZ Persei, of similar brightness) one of the
two UV Ceti stars to lie in the Sonneberg 100 square degrees field centred
at rho Persei.





                    W. WENZEL

                    Sternwarte Sonneberg
                    Zentralinstitut fur Astrophysik
                    der Akademie der Wissenschaften
                    der DDR