COMMISSION 27 OF THE I.A.U.
              INFORMATION BULLETIN ON VARIABLE STARS
                           Number 1221

                                             Konkoly Observatory
                                             Budapest
                                             1976 December 23


    ON THE PERIOD BETWEEN FLARES OF V1216 SAGITTARII

Since 1969 numerous observations have been made at Boyden
Observatory of the flare star V1216 Sagittarii (R.A. 18h47m42s,
declination -23deg52', visual magnitude 10.5).
   The telescope used during this work was the 41 cm Nishimura 
Reflector, fitted with a cooled EMI 6256A photomultiplier
tube and a standard Johnson B. filter.
   The following table gives a summary of the observations:

Interval between flares      Total Monitoring Reference
                                        time

1  and   6   47h38m00s               25h11m0s  (1)
3   "    6   46 48 45
3   "    7   48 35 35
5   "    8   45 13 10
7   "   10   46 47 56
8   "   11  145 47 01
8   "   12  144 43 00

1   "    6   48 26 30                50 24 0   (2)
3   "    6   46 51 45
3   "    7   48 39 30
5   "    8   46 59 45
7   "   10   46 47 42

1   "    3   46 02 42                41 54 0   (3)
3   "    4   45 09 48
4   "    5   97 57 48

1   "    3   45 53 54                41 54 0   (4)
2   "    3   46 02 42
3   "    4   45 09 48
4   "    5   97 57 48

1   "    2   48 06 48                24 42 0   (5)
1   "    5   95 10 00                20 03 0   (6)
2   "    3   50 25 30
5   "    7   94 23 30

(1) I.B.V.S. No. 379, September 15, 1969,
    A.H. Jarrett and J.P. Eksteen.
(2) MNASSA, 28, 11 and 12, p. 131, 1969,
    A.H. Jarrett and J.P. Eksteen.
(3) I.B.V.S. No. 481, October 31, 1970,
    A.H. Jarrett.
(4) MNASSA, Vol. 30, No.7, July 1971, p. 94,
    A.H. Jarrett and J.P. Eksteen.
(5) I.B.V.S. No. 711, August 31, 1972,
    A.H. Jarrett and J.P. Eksteen.
(6) I.B.V.S., No. 968, March 3, 1975,
    A.H. Jarrett and G. Grabner.

   From the above the mean period for the interval between
flares is 47h55m45s. Although realizing that it by no means 
provides conclusive evidence, it is a fact that a significant 
number of the flares observed (just over 87%) indicate an interval
between flares of approximately 48h, 2x48h or 3x48h. This might
be regarded as further support for the 48h interval previously
reported for this star (Andrews, 1966).


                              A.H. JARRETT and G. GRABNER

                              Boyden Observatory,
                              Department of Astronomy,
                              University of the O.F.S.,
                              Bloemfontein.
                              Republic of South Africa



Reference:

Andrews, A.D. 1966, P.A.S.P. 78, 542 [BIBCODE 1966PASP...78..542A ]