COMMISSION 27 OF THE I. A. U.
       INFORMATION BULLETIN ON VARIABLE STARS
                    NUMBER 729

                                 Konkoly Observatory
                                 Budapest
                                 1972 October 23


   EIGHT NEW LONG PERIOD VARIABLES IN SAGITTARIUS

   Among the variables discovered with the Rodman Blink
Microscope in the summer of 1971 by students at the Maria
Mitchell Observatory are eight new long period variables,
three with apparently changing periods.


No. Position 1900      Max    Min  Type J.D.Period  D* C*  Note
---------------------------------------------------------------
1   18h20m19s-32d20.7' 12.2   13.6  SR  41180 200   EH PK
2      20 46 -28 35.8  12.5  [14.   M   36780 239   EH PK
3      22 52 -28 27.8  12.6  [14.5  SR  36035 115.3 KK PK   1
                                        39370 114.5
4      22 55 -22 50.9  13.3 [15.    M   37140 249   EH BH
5      24 35 -20  7.0  12.3  14.9:  M   31970 358   PB BH   2
                                        41140 367
6      27 17 -20 10.4  11.6 [14.2   M   30090 345   PB BH   3
                                        36830 358
7      35 49 -27 55.9  13.0 [14.5   M   37490 270   EH DH
8      36 40 -28 12.0  12.5 [14.5   M   40120 345   EH DH
--------------------------------------------------------------

    D*, Discoverer: PB, Pamela Bonnell; EH, Esther Hu; KK, Karen
        Kwitter.
    C*, Computer: BH, Barbara Hatfield; DH, Dorrit Hoffleit; PK,
        Pamela Knight.


                      [FIGURE 1]

                         Notes:
1. The period of 115.3 days holds for JD 26000-38000; from
38000 to 41500 the period is 114.5 days.
2. For JD 23900-33000 the period of 358 days holds, while
367 days fits the observations for 31500-41500. In the overlap 
interval either of these periods satisfies the available
observations. In chart 5 the variable is marked A; star B is
a suspected short period variable.
3. For JD 23900-32000 the period of 345 days fits the observations, 
whereas 358 days (fortuitously the same as for the early 
observations of the preceding star) fits the observations
for 36000-41500.
    Of the students listed as discoverers (D) or computers
(C), Miss Pamela Knight was a 1972 NSF Undergraduate Research
Participant; the others were all employed under the 1971 NSF
Grant GP-30065. We all wish to express our appreciation to the
U.S. National Science Foundation.





                        DORRIT  HOFFLEIT
                        Maria Mitchell Observatory
                        Nantucket, Mass., U.S.A.