  Since its discovery in 1995, V2400 Ophiuchi (V2400 Oph) has stood apart from
most known intermediate polar cataclysmic variables due to its proposed
magnetic field strength (9-27 MG) and disk-less accretion. To date, the exact
accretion mechanism of the system is still unknown, and standard accretion
models fail to accurately predict the peculiar behavior of its lightcurve. We
present the K2 Campaign~11 light curve of V2400 Oph recording 74.19 days of
photometric data cadenced at 1 minute. The light curve is dominated by
aperiodic flickering and quasi-periodic oscillations, which make the beat and
spin signals inconspicuous on short timescales. Notably, a log-log full power
spectrum shows a break frequency at $\sim10^2$ cycles~d$^{-1}$ similar to some
disk-fed systems. Through power spectral analysis, the beat and spin periods
are measured as $1003.4\pm0.2$ seconds and $ 927.7\pm 0.1$ seconds
respectively. A power spectrum of the entire K2 observation demonstrates beat
period dominance. However, time-resolved power spectra reveals a strong
dependence between observation length and the dominant frequency of the light
curve. For short observations (2-12 hrs) the beat, spin, or first beat harmonic
can be observed as the dominant periodic signal. Such incoherence and
variability indicate a dynamical accretion system more complex than current
intermediate polar theories can explain. We propose that a diamagnetic blob
accretion model may serve as a plausible explanation for the accretion
mechanism.
