COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                      Number 2631



                                   Konkoly Observatory
                                   Budapest
                                   26 November 1984

                                   HU ISSN 0374 - 0676



     NEAR-INFRARED LIGHT ELEMENTS OF 13 VERY COOL MIRA VARIABLES



Near-infrared narrow-band photoelectric photometry of unidentified
sources in the Two Micron Sky Survey ("IRC") has led to the discovery
of 13 new Mira variables. The observations were made between 1969 and
1975. These stars all attain photometric spectral types later than
M9.5 at minimum light, which makes them the coolest Miras known whose
photospheres are directly observable. Their mean periods and
amplitudes at 1.04 micron substantially exceed the mean amplitudes and
periods of previously observed visually bright Miras that reach M9.5
(Lockwood 1985). Light elements at 1.04 micron and observed characteristics
of these stars are given in Table I.





                           G. W. LOCKWOOD
                           Lowell Observatory
                           Post Office Box 1269
                           Flagstaff, Arizona 56002





Reference: Lockwood, G. W. (1985). Astrophys. J. Suppl., in press. [BIBCODE 1985ApJS...58..167L ]


                                                Table I. New Mira Variables.
---------------------------------------------------------------------------------------------------------------------------------------
                                                        104       104         V       V           Spectral               Adopted
Designation   IRC      a(1950)+   5(1950)+    I-K       max    amplitude     max   amplitude         type     Period      epoch      n
---------------------------------------------------------------------------------------------------------------------------------------
              -30023   2h35m08s   -27d11'4    5.22      2.53m     1.84m       9.8m  5.0m         M7.8-10.1   480+-30d   2,441,340    5
              -30217  14 10 37    -29 40.5    5.20      1.46      1.46       12.1   3.7          M8.6-10.1   450+- 20    2,442,566   11
              +00102   6 19 22    -3  50.3    6.59      6.10      2.39        -      -           M8.0-10.7   490+-20    2,441,125   10
              +00266  15 26 17    +3  59.8    5.45      5.28      1.65       13.1    -           M6.5-9.9    470+- 20    2,441,737   14
V2108 Oph     +10322  17 11 56    +8  59.3    6.31      3.85      2.25       13.6    -           M8.5-10.2   580+- 30    2,441,834   13
V1111 Oph     +10365  18 34 59    +10 23.0    6.08      2.99      1.76       11.8   3.6          M8.9-10.4   460:       2,441,402    5
              +10525  22 59 37    +10 20.0    5.73      4.92      2.20       14.5    -           M8.4-10.3   520+- 30    2,441,251    8
              +30021   1 08 30    +30 22.0    6.10      5.29      2.83       14.7    -           M8.5-11.0   560+-20    2,441,655   20
V697 Her      +30292  16 25 59    +34 54.6    6.34      5.54      2.54       15.3    -           M8.5-9.6    520+- 20    2,442,566   12
KU And        +40004   0 04  17   +42 47.9    6.59      5.41      3.210      15.2    -           M5.0-9.8    660:       2,442,345    
NV Aur        +50137   5 07 20    +52 48.8    6.57      9.73      1.04        -      -           M8.2-9.6    635*       2,441,221    6
              +60092   2 31 43    +64 56.6    5.47      4.82      2.21?      12.8    -           M8.4-10.3   600:       2,441,221    8
              +60169   6 30 02    +60 58.9    6.26      2.89      1.62?      10.9   3.8          M8.5-9.5    440+- 30    2,441,340    9


 * Period from GCVS.
 + Positions from the Two Micron Sky Survey.