This is the third paper in a series performing the real-time CCD differential photometry of
Scuti variable stars in open clusters at the Seoul National University Observatory(SNUO).
In the first paper (Kim & Lee 1996, - Paper I), V650 Tau in the Pleiades cluster was studied.
The observational results of BT Cnc in the Praesepe cluster was presented in the second
one (Kim & Lee 1995, - Paper II). The main purposes of this long-term observational project are as follows.
First, we perform CCD photometry of Scuti variable stars showing complicated light curves.
They have multiple pulsation periods so as to be one of the most important observing targets
of asteroseismology (Brown & Gilliland 1994). For this work,
accurate data sets should be obtained over a sufficiently long-time baseline.
From the observed data, we detect precisely their pulsation periods as many as possible and
identify the pulsation mode for each period. Second, comparing our observational results
with the previous one, we investigate the variations
of pulsation period and its amplitude (for reviews, see Breger 1990a and Rodrıguez et al. 1995).
There are several advantages to observe variable stars in open clusters using a CCD camera. First, it allows more chances to find comparison stars near the variable stars. Second, we can get more accurate data because a number of objects are observed simultaneously in the same CCD frame. It is also possible to produce well-defined differential magnitudes even under non-photometric nights and at a less-photometric site like a university campus (Kreidl 1993). Finally, we are able to compare the physical properties (pulsation mode, mass, radius and age, etc.) derived from the pulsation model with ones obtained from the other methods such as the evolutionary model, because the physical properties of open clusters are known well.
In order to investigate the incidence of Scuti stars in the 
Persei cluster, Slovak (1978)
carried out the differential photometry for 24 A
F type stars in or near the Scuti
instability strip. He detected three variable stars as follows; V 459 Per (=BD +48
894, H 501),
V 461 Per (=BD +48905, H 606), V 465 Per (=BD +47842, H 906). Among these, V 465 Per is the bluest
and the largest-amplitude variable, displaying complicated light curves.
From the data obtained on two nights, he found a dominant pulsation period of 1.92 hours
and the secondary period of 43 minutes. Its membership was confirmed by the combined astrometric, photometric
and spectroscopic results (Prosser 1992).
The present paper provides observational results of V 465 Per (
,
A6Vn) obtained during the period
between November, 1994 and January, 1995. The observation and data reduction are reported in Sect. 2.
The frequency analysis and the identification of pulsation modes are presented in Sect. 3 and Sect. 4, respectively.