COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                      Number 1868

                                  Konkoly Observatory
                                  Budapest
                                  1980 November 13

                                  HU ISSN 0374-0676




      RESULTS OF THE PHOTOELECTRIC OBSERVATIONS OF 88 Her



     In 1974 Harmanec, Koubsky and Krpata (1974) confirmed both the
spectral duplicity and the 87-days period for the Be shell star
88 Her, discovered by the above authors earlier. Having used
the radial velocity curve obtained by Harmanec et al., with
allowance for that eclipses can be expected at the phase of
0.29 and 0.80, Haupt (1974) estimated and published the moments
of possible eclipse of 88 Her for the nearest future (1974,1975).
     Based on the photometry in UBV system performed at five
observatories in 1968-1977, Harmanec et al.,(1978) found a long-
term variation of light and colour for 88 Her. In 1978 Hirata
(1978) pointed to the similarity of photometric and spectral behaviour 
of 88 Her and Pleione. Unlike 88 Her, which represents
a spectroscopic double system, the properties indicating the
double nature of Pleione have not been discovered.
     Our attention was drawn by P. Koubsky to 88 Her in 1975.
We observed 88 Her in the UBV system from June 1977 through August
1980 with the electrophotometer attached to the 48-cm reflector
AZT-14 A. The recording was performed using the photon counting
method. HD 162132 = BD +47d2537 served as the comparison star.
     Our observations of 1977-78 show the light variation near
the phase of 0.8 with an amplitude of 0.14m, 0.10m and 0.07m in UBV,
respectively. The phases were calculated by the formula:
     T_maxRV = HJD 2419429.251d + 86.7207d E.
     Further observations of 88 Her in 1979-80 show that the
star has constant maximum brightness (Figures 1,2) both near
0.8 and at other phases, which proofs that the light decrease of
88 Her observed in 1977-78 is not of eclipsing pattern, but it
has the character similar to the light variation of Pleione.

                       [FIGURE 1]
                       [FIGURE 2]

                      N.L. MAGALASHVILI
                      J.I. KUMSISHVILI

                      Abastumani Astrophysical Observatory 
                      of the Academy of Sciences
                      of Georgian SSR

References:
1. Harmanec,P.,Koubsky,P.,and Krpata,J.,1974,Astron.Astrophys.
        33, 117 [BIBCODE 1974A&A....33..117H ]
2. Haupt,H., 1974, I.B.V.S. No. 928
3. Harmanec,P.,Horn,J.,Koubsky,P.,Kriz,S.,Zdarsky,F.,Papousek,J.,
        Doazan, V.,Bourdonneau,B.,Baldinelli,L.Ghedini,S.,
        and Pavlovski, K., 1978, Bull.Inst.Czech. 29,No.5,278 [BIBCODE 1978BAICz..29..278H ]
4. Hirata, R., 1978, I.B.V.S. No. 1496