COMMISSION 27 OF THE I. A. U.
		 INFORMATION BULLETIN ON VARIABLE STARS
		             Number 2400

						Konkoly Observatory
						Budapest
						20 September 1983

						HU ISSN 0374-0676

			FOUR NEW RED VARIABLES


  On the photographs taken with four cameras of focal lengths 20, 30, 50 and
85 cm, the following four red variables were found. The emulsion was Tri-X
and the brightness very close to visual magnitude was obtained with green-
yellow filter. The positions of the stars are as follows:

Star    R.A.(1950.0)     Decl.
No.1      6h30m47s    +28d19.6'
No.2     19 49 43     +43 30.0
No.3     19 50  0     +44  6.7
No.4     20 53 53     +23 44.7= BD + 23d4183

  (Star No. 1) On more than 540 photographs taken in 1977 through 1982 with
f50 and 85 cm cameras, the star was found to be probably SRa type with a 
period of 188d. The range was 11.9m-13.1m(v) so far. The variation is well 
expressed by the following elements:

Max. = J.D. 244 3490 + 188d E.

The light variation in the recent years is shown in Figure 1.

                        [FIGURE 1]

   Figure 1. Light variation of star No. 1.

  (Star No. 2) On about 450 photographs taken in 1976 through 1983 centered
at delta Cygni, the star was found to be SRa type having fairly regular variation. 
The range was 10.3m-11.5m(v). The maxima were well expressed by the 
following elements with O-C's less than 10 days:

       Max. = J.D. 244 2910 + 119.3d E.

The light variation only in the recent years is shown in Fig. 2.

                        [FIGURE 2]

   Figure 2. Light variation of star No. 2.

(Star No. 3) On the same photographs as of No. 2,   the star was found to
be probably SRa type with the range of 11.0m-12.5m(v). The periodicity became
sometimes irregular, but the overall variation is generally expressed by the
following elements:

           Max. = J.D. 244 3640 + 146d E.

The light variation in the recent years is shown in Figure 3.

                        [FIGURE 3]

   Figure 3. Light variation of star No. 3.

  (Star No. 4 = B.D. + 23d4183d) On more than 300 photographs taken with the
f30 cm camera in 1975 through 1982 centered at 31 Vulpeculae, the star was
found to be probably SRa or SRb type. The amplitude was 10.3m-11.4m(v) so far.
The variation was fairly regular in some years, but not apparent in some years
as in 1977 and 1978. The variation is generally expressed by the following
elements:

            Max. = J.D. 244 2775 + 116d*E.
The light variation is shown in Figure 4.

                        [FIGURE 4]

   Figure 4. Light variation of star No. 4.

                        [FIGURE 5]

   Figure 5. Finding chart of star No. 1, No. 2, and No. 3



                        MASAAKI HURUHATA
                         Hodozawa 88
                         Gotemba-shi,
                         412 Japan