COMMISSION 27 OF THE I. A. U.
	INFORMATION BULLETIN ON VARIABLE STARS
		    Number 2640


			          Konkoly Observatory
			          Budapest
			          11 December 1984

			          HU ISSN 0374 - 0676


	 A NEW PULSATING VARIABLE IN VELA


   In April 1978 a new variable star was found at the
European Southern Observatory, La Silla, among early-type
stars in the field of planetary nebula NGC 3132. Further
UBV measurements in 1979 and 1980 ( 50 cm and 1 m telescopes
and pulse counting photometers with EMI 6256A photomultipliers) 
revealed this star to be a short-period pulsating
variable. Stars in the E-regions (Cousins, 1973; Vogt et al,,
1981) served as photoelectric standards.
   The coordinates of the variable as well as of three
comparison stars, measured on a Schmidt plate (ESO 100/162
cm Schmidt camera) are given in Table I. It also contains
the UBV data together with their r.m.s. errors ( n denotes
the number of observations) and the estimated spectral
types; the positions of the variable and of the comparison
stars are marked on the finding chart.

                    [FIGURE 1]


		    Table I
	 Positions, magnitudes and spectral types
----------------------------------------------------------------------
Star	    A.R.       Decl.	  V	  B-V	  U-B	  n	   Sp
		  1950
----------------------------------------------------------------------
Var	 10h05m59s78-40d25'22"3   12.55   0.39    0.17    193      A8
Comp.1	    05 43.55    22 50.9	  10.986  1.211   1.072     5	   G8:
				  +-.004 +-.007  +-.007
Comp.2	    05 24.56    19 52.0	  11.577  0.553   0.041     24	   F8
				  +-.002 +-.003  +-.005
Comp.3	    06 00.90    27 21.1	  13.103  0.629   0.147      7	   G0:
				  +-.002 +-.004  +-.006
----------------------------------------------------------------------


    Two objective-prism plates (ESO Schmidt camera, dispersion 
450 A/mm at H_gamma, Kodak IIa-O and IIIa-J, March 1978)
show, that the spectrum of the variable is of type A8.
    The light curve of the variable star can be approximated 
by a sine curve with the period of P = 0.088 days and the
mean visual amplitude of A_V = 0.07 mag. The detailed analysis
of the observing data including the more accurate determination 
of the pulsating period will be presented later.
    I wish to thank H.-E. Schuster for taking the Schmidt
camera plates, and H.-M. Steinbach for assistance with the
reduction. The observations have been collected at the European 
Southern Observatory, La Silla, Chile.




			       L. KOHOUTEK
			    Hamburger Sternwarte
			     D-2050 Hamburg 80
				 F R G



References:

Cousins, A.W.J., 1973, Mem.Roy.Astron.Soc. 77, 223 [BIBCODE 1973MmRAS..77..223C ]
Vogt, N., Geisse, H.S., Rojas, S., 1981, Astron.Astrophys.
    Suppl. 46, 7 [BIBCODE 1981A&AS...46....7V ]