One of the main problems concerning the interpretation of observed frequencies is to identify their pulsation modes. The most reliable method for pulsation mode identification is to analyze the profile variations of a high-resolution spectral line (for example, Kennelly et al. 1992). With the use of photometric data, the pulsation mode can be identified from the phase difference and amplitude ratio of color variations (Watson 1988; Garrido et al. 1990). In the case of small light variations such as V 465 Per, however, it would be difficult to obtain the color variations with sufficient accuracy. We used only the sizes and ratios of observed frequencies in order to identify the pulsation modes of V 465 Per.
The pulsation mode for each observed frequency can be identified from the comparison between the theoretical pulsation constant and observational one derived from the photometric parameters (Breger 1990b). The pulsation constant Q is expressed in terms of four observable parameters as follows (Breger et al. 1993);
For V 465 Per, we adopted the values of log 
and log g=4.312 (López de
Coca et al. 1990) which were
derived from the uvby, H
photometry. The absolute magnitude of
was calculated from the distance modulus of 
and
interstellar reddening of E (V-I)=0.16 for the 
Per cluster (Stauffer et al. 1989), and the
bolometric correction of -0.02. The 
(Garcıa et al. 1995) indicates the normal solar abundance.
The effective temperature and the absolute magnitude are similar to the
another values, log 
derived from the UBV photometry (B-V=0.276; Prosser 1992)
and MV=2.34 estimated from the uvby, H photometry (López de Coca et al. 1990).
The pulsation constants for the four frequencies are obtained by the above equation as follows;
, 
, 
and 
.
The uncertainties were estimated from the error of photometric parameters, following the method by Breger (1990b).
Comparing these Q-values with the theoretical ones, only the value of Q3 exists within
the range of p-mode oscillations (for example, 
; Dziembowski & Pamyatnykh 1991).
The other values fall within the range of g-mode oscillations which are not common among the 
Scuti variable stars;
Breger & Beichbuchner (1996) argued that the low-frequency variations reported in several Scuti variables
might be caused by variable comparison stars and/or instrumental/atmospheric effects.
So far, four candidates of BI CMi, 44 Tau, CE Oct and IK Peg (Breger & Beichbuchner 1996),
63 Her (Mangeney et al. 1991; Breger et al. 1994) and IFA star 9 in NGC 6134 (Frandsen et al. 1996)
may be known as Scuti variables with low-frequency (g-mode) oscillations.
In order to obtain the information on the pulsation mode, we investigate the frequency ratios of V 465 Per. The ratios of two frequencies, f1/f2=0.816 and f1/f3=0.517 are similar to those given by theoretical frequency ratios of two radial modes, P2/P1=0.810 and P3/P0=0.521 (Breger 1979), respectively. To match the results of frequency ratios with ones of pulsation constants, the observational parameters of V 465 Per should decrease to the value predicted at the theoretical p-mode oscillations, as the same case of HD 18878 (Mantegazza & Poretti 1993) and BI CMi (Mantegazza & Poretti 1994). If f1 is the first overtone radial mode (1H-mode; P1) or the fundamental radial mode (F-mode; P0), the value of log Q should be decreased by the amount of about -0.318 or -0.197, respectively. This difference of log Q may be too large to be interpreted as errors of photometric parameters.
In conclusion, we have detected four pulsation frequencies in V 465 Per. Among these, deduced from the high Q-values,
three frequencies (including two dominant frequencies of f1=14.040 c/d and f2=17.208 c/d)
may be associated with g-mode oscillations. This is very important
because g-mode oscillations are able to provide the information on the inner part of
stars such as the extent of the convective overshooting (Dziembowski & Pamyatnykh 1991).
However, it is noted that the Q-value might be affected by systematic error
related to rotational velocity (Breger 1990b; Pérez Hernández et al. 1995).
Therefore the pulsation mode identification on the basis of the Q value may involve some uncertainty for
a fast rotator such as V 465 Per which has a rotational velocity, 
(López de Coca et al. 1990).
For V 465 Per, extensive observations by a multisite campaign
would be required to detect more pulsation frequencies and to investigate the pulsational
characteristics such as g-mode oscillations.
Acknowledgements
One of us, S.-L. Kim thanks Dr. R. Garrido for his valuable advices, Dr. M. Breger and Dr. R.S. Stobie for their comments. We acknowledge ICNSRF (Inter-University Center for Natural Science Research Facilities) for using the CCD Camera. This work was supported by the Basic Research Institute Program, Ministry of Education, BSRI-95-5411 and also partly supported by MOST (Ministry Of Science and Technology) Research Fund.