COMMISSION 27 OF THE I. A. U.
       INFORMATION BULLETIN ON VARIABLE STARS
                    NUMBER 371

                            Konkoly Observatory
                            Budapest
                            1969 August 18

    UBV OBSERVATIONS OF NOVA DELPHINI 1967 (=HR Del)
           AND NOVA VULPECULAE 1968 No. 1

      The series of observation of both novae at Ondrejov
Observatory (1,2,3) was discontinued in April, 1969. Since
no new observations are planned, it was decided to publish
the remaining data without further delay. Comparison stars
for HR Del and Nova Vul 1968 No. 1 were published in (1) and
(3), respectively. There is also described the method of
observation and reduction. EMI 6256 unrefrigerated 
photomultiplier attached to the 65 cm refractor was used and
differential extinction and conversion to the international
UBV system was always applied. Quality q (3 is the best) is
approximately proportional to the number of individual 
observation in a given night.

               Nova HR Delphini
JD hel. 
2440...    V         B-V     U-B     q
286.689   7.53      0.63:   -0.52    1
287.677   7.55      0.54    -0.49    2
319.619   7.68      0.60    -0.59    2
321.623   7.73      0.63    -0.54    1
326.611   7.68      0.67    -0.50    2

Comparison stars e and f from (1) were used



         Nova Vulpeculae 1968 No. 1

JD hel.
2440...        V     B-V     U-B     q
286.682      11.04   1.60    0.32    3
287.656      11.04   1.54    0.32    3
319.598      11.22   1.56    0.39    2
321.603      11.69   1.52     -      1
326.595      11.33   1.56    0.40    2

Comparison stars e and f from (3) were used


      The V magnitudes of both novae are considerably
brighter (about -0.7m) than those obtained by Tempesti
(4, 5) in about the same time. Only minor part of the 
difference may be explained by colour terms in the equations
of transformation that were apparently not known in Tempesti's
measurements (at least one of his comparison stars was of
late spectral type K0). However, the differences caused by
emission features of the nova may be significant, but even
this effect seems to be insufficient to explain the large
shift of both magnitude scales.


References

(1) Grygar, J., Kohoutek, L., Harmanec, P., 1968, Bull. Astr,
   Inst. Csl. 19, 101. [BIBCODE 1968BAICz..19..101G ]
(2) Grygar, J., Kohoutek, L., 1969, Bull. Astr. Inst. Csl. 20,
   156. [BIBCODE 1969BAICz..20..156G ]
(3) Grygar, J., Kohoutek, L., 1969, Bull. Astr. Inst. Csl. 20,
   No. 4 (in press).
(4) IAU Circ No. 2139, 1969.
(5) IAU Circ No. 2154, 1969.




                        J. GRYGAR
            Astronomical Institute of the Czechoslovak
                   Academy of Sciences,
                   Observatory Ondrejov,
                      Czechoslovakia