COMMISSION 27 OF THE I. A. U.
         INFORMATION BULLETIN ON VARIABLE STARS
                     NUMBER 139


					Konkoly Observatory
					Budapest
					14 June 1966

               PHOTOELECTRIC OBSERVATIONS
	           OF NOVA HER 1963

	Nova Her 1963 showed gradual brightening before its 
maximum (1). The light curve during decline was observed in many 
observatories, however rapid fluctuations, in few hours observation, 
were not observed.
	The nova showed random changements in brightness of 0.02,
0.05 magnitudes during the summer 1965 when it was observed by
Chincarini in blue and ultraviolet light with the 24" of the Lick 
Observatory. The maximum amplitude of light variations was of 0.13
magnitudes in one hour. Such fluctuations were also observed the year
before by Almar at the Konkoly Observatory and a short periodicity,
about 1 hour, was suspected (2). Observations by Almar and Chincarini
at the Astrophysical Observatory of Asiago (March 16, 1966) and by
Almar (March 28, 1966) showed after a period of constant brightness
a decrease in luminosity. Following these observations Rosino 
announced the presence of a minimum of 40 minutes duration and 0.1 mag
depth similar to the partial eclipse of the Algol-type binaries (3).
	Observations of the nova were carried out at Lick Observatory
on the nights April 20, 21, 22 and 27 (U. T.). The 1P21 cell without
any filter has been used. The light curve of the nova is now 
characterized by:

	a/ fluctuations of amplitude between 0.2 and 0.1 magnitudes
	and lasting from 5 to 50 minutes

	b/ overimposed a few minima with amplitude of 0.1-0.2
	magnitudes and lasting only 15 minutes were observed.

	A preliminary analysis of the observations did not show 
evidence of eclipse. However a piece of the light curve observed on April
22 is almost exactly (within 0.02 magnitudes) repeated  on the light
curve of the night April 27. During this period, lasting about 90 minutes,
the nova increased in brightness of about 0.2 magnitudes with fluctuations 
of 0.06-0.10 magnitudes. The same features lasting 90 minutes
seem to be present on the night April 20, in this case the agreement is
poorer. A period P = 359.5 minutes could agree with all our observations. 
More observations are needed in order to understand the nature
of the periodicity. A spectrum obtained at the Crossley during 1965
showed very strong hydrogen and nebular emissions on a faint 
continuum. Most of the light should, therefore, be coming from the 
expanding gaseous shell.

Lick Observatory
May 29, 1966
						 G. CHINCARINI
						 V. S. HOWARD

References:
(1) W. Gotz	Sky and Telescope (April 1966)
(2) I. Almar	Private communication (March 1966)
(3) L. Rosino   I.A.U. Circular No. 1953.