In the analysis of GK Per, a strange phenomenon can be observed¡Xquasi-periodic oscillations (QPO). ¡§QPOs are defined as low-coherence brightness oscillations thought to be associated with material within the inner accretion flows of CVs (Morales-Rueda, Still & Roche, hereafter MSR, 1999). Though the source can be considered periodic, its period has a certain variance. The state of the GK Per system affects the observed QPO period (PQPO) (Yi & Kenyon 1997). Various people have analyzed the optical periodicity, but their results vary greatly. For example, Patterson (1981) observed the source during quiescence in 1978, finding PQPO to be about 380 seconds. During the decline phase of GK Per in 1983, Mazeh et al. (1985) found PQPO ~360 sec, and also determined PQPO ~400 s during two nights of GK Per¡s outburst phase (Yi & Kenyon 1997). Watson, King & Osborne (1985) also observed a ~5000 s QPO through the analysis of X-ray data.
             No consensus has been reached as to a single model for the QPO phenomenon. Theoretical models suggest dense blobs in orbit within the inner disk (Bath 1973), pulsations on the surface of the white dwarf (Papaloizou & Pringle 1978), or oscillating acoustic waves in the inner regions of the accretion disk (Okuda et al. 1992; Godon 1995). However, these models can only account for QPOs of a few hundred seconds. GK Per, on the other hand, has a QPO of several thousand seconds (MSR 1999). To explain this problem, several new models were developed.
             MSR (1999) apply the magnetospheric¡Xor beat-frequency¡Xmodel suggested by Watson, King & Osbourne (1985). Since GK Per has a relatively weak magnetic field, the accretion disk will come very close to the star, completely surrounding the magnetic field. At the inner edge, clumps of plasma will be present. The magnetosphere will keep the clumps from coming closer to the star¡Xunless the clump moves directly above the poles. When this occurs, t...