COMMISSION 27 OF THE I. A. U.
          INFORMATION BULLETIN ON VARIABLE STARS
                       Number 2896



                                       Konkoly Observatory
                                       Budapest
                                       14 May 1986

                                       HU ISSN 0374-0676


       THE LIGHT CURVE OF KR AURIGAE IN THE SEASON 1985/86

  In completing the long-time light curve of KR Aurigae the star was
measured on 27 blue-sensitive plates (ORWO-ZU21+GG13+BG12) from 19 nights
obtained with the Schmidt camera 50/70/172 cm of Sonneberg Observatory,
covering the time interval between 12 September 1985 and 1 March 1986, using
the comparison star sequence given by Popova (1965). The observations are
given in Table I.

                   Table I


J.D.          m(B)      J.D.         m(B)
244...                  244...

6321.631     13.15m     6387.573    15.10m
6322.605     13.4 :     6405.390    14.40
6327.607     13.1 :     6440.435    14.70
6327.622     13.25      6463.340    13.30
6358.590     14.90      6466.324    13.30
6358.606     14.70      6466.344    13.40
6359.540     15.0 :     6469.315    13.57
6359.565     15.10      6469.335    13.66
6360.602     14.70      6474.312    13.65
6360.626     14.80      6474.338    13.70
6361.619     15.20      6488.285    14.10
6364.665     14.80      6489.256    14.15
6385.528     15.35      6491.305    14.30
6385.548     15.35


                           [FIGURE 1]


    It can be seen from Figure 1 that KR Aurigae was in a minimum phase
in the time interval between J.D. 244 6358 and J.D. 244 6440.
The decrease from the maximum brightness (m(B)~13.2m) to the faint light
(m(B)~15.0m) as well as the increase from that state to the maximum brightness
(m(B)~13.3m) could not be observed, unfortunately. But there is no doubt
that the decrease to the faint light took place within less than 31d.
    Slow temporal light fluctuations are superimposed on the mean light
curve. At the end of the series a continuous decrease in the brightness from
m(B) = 13.3m to m(B) = 14.3m is indicated.
    Concerning the minimum phase our own observations in B are in agreement
with visual estimations given by Ducoty (1985), which are marked by circles
in Figure 1.







                            W. GOTZ
                       Akademie der Wissenschafcen
                       der DDR, Zentralinstitut fur
                       Astrophysik, Sternwarte Sonneberg
                       DDR


References:
Popova, M., 1965, Peremennye Zvezdy, 15, 534 [BIBCODE 1965PZ.....15..534P ]
Ducoty, R., 1985, IAU-Circ. No. 4150 [BIBCODE 1985IAUC.4150....2D ]