COMMISSION 27 OF THE I. A. U.
        INFORMATION BULLETIN ON VARIABLE STARS
                     NUMBER 706
                                    Konkoly Observatory
                                    Budapest
                                    1972 August 4



      PHOTOELECTRIC UBV MEASURES OF NOVA CEPHEI 1971



    The early decline stage of Nova Cephei 1971 was observed 
by us in the UBV system on 14 nights in July, August, and
September 1971. Our equipment consisted of a single-channel
photometer with refrigerated 1P21 photomultiplier, a direct-
current amplifier, and stript-chart recorder at the Cassegrain 
focus of the 132 cm telescope of The University of 
Michigan.
    The values obtained are presented in Table I. An average
of 9 standards was observed each night; about half of the standards 
each night were taken from among the brighter stars in
NGC 7160 with values obtained from Hoag et al.(1961).The mean
standard deviations in the least squares fits for the standards 
are +-0.025, 0.016, 0.021 mag. in V, B-V, U-B, respectively.
Extinction coefficients were determined on most of the nights;
in the column labelled "Extinction" in Table I "n" indicates
that a nightly extinction value was used and "m" that a mean
value was applied. All observations of the nova were made 
between 1.019 and 1.088 air masses.



                          Table I
---------------------------------------------------------------
1971                              1971
U.T.Date V     B-V   U-B          U.T.Date V     B-V  U-B  
July                   Extinction  Aug.                  Extinction
---------------------------------------------------------------
  14.28 8.21  0.51 -0.44   m      05.29   9.31  0.62 -0.55   m
    .29 8.23   .51 - .43   m        .37   9.43   .66 - .53   m
    .38 8.33   .52 - .42   m      06.22   9.55   .63 - .54   n
  15.29 8.42   .60 - .46   m        .31   9.55   .64 - .58   n
  16.25 8.46   .60 - .46   n      07.23   9.88   .62 - .55   n
    .34 8.50   .61 - .45   n      12.25  10.25   .51 - .59   m
  20.26 8.65   .65 - .49   n      16.23  10.68   .45 - .39   m
    .34 8.63   .64 - .49   n      18.31  10.64   .42 - .35   n
  21.29 8.68   .67 - .50   n      Sep.
    .36 8.73   .68 - .55   n      22.13  11.26   .33 - .34   n
  27.27 9.35   .63 - .55   n      24.18  11.47   .28 - .26   n
    .35 9.37   .63 - .54   n
---------------------------------------------------------------



    The light-curve in V would be classed as fast/moderately
fast according to Payne-Gaposchkin (1957) and has similarities
to that of XX Tauri. We are unaware of further photoelectric
observations of Nova Cephei 1971 other than those reported here
and in I.A.U. Circulars No. 2343, 2351, and 2353.



Department of Astronomy
The University of Michigan
Ann Arbor, Michigan 48104       D. J. MacCONNELL
                                J. C. THOMAS


References

Hoag, A.A., Johnson, H.L., Iriarte, B., Mitchell, R.I., Hallam,
   K.L., and Sharpless, A. (1961) Publ.U.S.Naval Obs. Vol. 17, Part
   7, 474. [BIBCODE 1961PUSNO..17....1H ]
Payne-Gaposchkin, C. (1957) "The Galactic Novae" (Amsterdam:
   North-Holland Publ. Co.), pp. 12, 24.