COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                      NUMBER 348

                               Konkoly Observatory
                               Budapest
                               1969 May 2

                  HD 116994

     At the beginning of 1968, the eclipsing variable
BV 513 was put on our photometric observing program in B
and V. Due to its proximity in the sky and its convenient
color index, the star HD 116994 was chosen for comparison.
Only after some five nights of observations, a preliminary
reduction of the records was begun, and it was then 
discovered that HD 116994 was itself variable. Another star was
then chosen for comparison and observations were continued
simultaneously on BV 513 and HD 116994. The observations of
BV 513 against HD 116994 could still be used, at least for
period study of HD 116994, once the light-curve and period
of BV 513 was well established by the later observations. A
total of about 1100 observations (B+V, and including those
at the beginning) were obtained between February 4 and May
24. Only in mid-March it was found that the variability of
HD 116994 had already been discovered in 1966 at Cerro
Tololo.
      HD 116994 is an intrinsic variable of very short
period, 0,10225d, and low amplitude, about 0,18m, and may
be classified as a dwarf cepheid.
      Two peculiarities were noted in the present 
observations: variation of amplitude and variation of period.
      The V-amplitude varied slowly between 0,16m and
0,20m. If there is any periodicity at all, a period of about
60d could be attributed, but some shorter period cannot be
ruled out entirely. The Cerro Tololo observations show even
an amplitude up to 0,22m; studying these, Kwan-Yu Chen finds
a modulation period of 0,338d, but such a short modulation
period could not be confirmed by the present observations.
      To study period variation, an O - C diagram was 
constructed with P = 0,10225d, including the Cerro Tololo 
observations. But it turned out that the variation of period
(lengthening during the present observations) was such, that
it is not possible to know the number of cycles between the
1966 and 1968 observations. So, any observation made between
1966 and 1968 would be of great value.
      The results given above are only preliminary. The
observations will be continued in 1969, as soon as possible
in three or more colors. We would be very glad to receive
any observation made since 1966 to improve the period and
amplitude study.
      Catalog data about this star are:
HD 116994 = SAO 240869; RA = 13h25m18s, D = -51deg01'58" (1950),
m_pg = 8,9, m_v = 8.7.


					R. G. QUAST
				The ITA Astronomical Observatory
				Sao Jose dos Campos, SP. Brazil