COMMISSIONS 27 AND 42 OF THE IAU
               INFORMATION BULLETIN ON VARIABLE STARS
                            Number 3881
                                                                
                                               Konkoly Observatory
                                               Budapest
                                               19 May 1993 

                                               HU ISSN 0374 - 0676


             A NEW SEMIREGULAR VARIABLE STAR IN LYRA


A new variable star (alpha =19h10m52.2s, delta =+30d14'30", equinox 1950.0,
epoch 1973.4) was discovered by one of us (A.P.K.).  Figure 1 presents the
finding chart.  The comparison stars have the following B magnitudes:  a
- 16.18, b - 16.35, c - 16.69, d - 17.10; these values were found 
photographically,
using the photoelectric and photographic sequences in the globular cluster M 56
(Barbon, 1965).  The variable was subsequently studied on 252 plates of Moscow
collection, taken at JD 2433034-2448459 with the 40 cm astrograph of the
Sternberg Institute Crimean Laboratory; the eye estimates were performed by A.
Katsyka.


                              [FIGURE 1]

           Figure 1. The finding chart for the new variable.


The new variable turns out to be a semiregular star, its cycle length being
about 60 to 70 days.  The following cycle length values were found for
different time intervals:  JD 2437118-2439406, ~70 days; JD 2440764-2442684,
64.1d; JD 2445847-2446732, 74.3d.  The observations cannot be represented
with a single set of linear light elements.  The limits of brightness variation
are from 16.4m to 17.1m B, the amplitude is about 0.7m.

The star does not seem obviously red on Palomar Sky Survey prints, so the
variable most probably belongs to the SRD type.  Its galactic latitude is b
=+9.1d, and the star might be rather far from the galactic plane.  The cycle
length values given above contain a hint to alternating periods.  Taking all
this into account, the new variable could be a candidate to the UU Her class of
semiregulars (Sasselov et al., 1987).  The new variable deserves more detailed
investigation to reveal its properties and improve classification.



           A. P. KATSYKA                       N.N. SAMUS
           Kolomna Pedagogical Institute       Institute for Astronomy,
           30, Zelyonaya Str.,                 Russian Academy of Science,
           Kolomna, Moscow Region 140410,      48, Pyatnitskaya Str.,
           Russia                              Moscow 109017, Russia

References:

Barbon, R., 1965, Asiago Contrib., No. 175, 63
Sasselov, D., Zsoldos, E., Fernie, J.D., Arellano Ferro A., 1987, Publ. Astron.
     Soc. Pacif., 99, 967 [BIBCODE 1987PASP...99..967S ]