  AM Canum Venaticorum (AM CVn) stars belong to a class of ultra-compact, short
period binaries with spectra dominated largely by helium. SDSS J0926+3624 is of
particular interest as it is the first observed eclipsing AM CVn system. We
observed SDSS J0926+3624 with the \textbf{Ar}ray \textbf{C}amera for
\textbf{O}ptical to \textbf{N}ear-IR \textbf{S}pectrophotometry (ARCONS) at the
Palomar 200" telescope. ARCONS uses a relatively new type of energy-resolved
photon counters called Microwave Kinetic Inductance Detectors (MKIDs). ARCONS,
sensitive to radiation from 350 to 1100 nm, has a time resolution of several
microseconds and can measure the energy of a photon to $\sim10%$. We present
the light curves for these observations and examine changes in orbital period
from prior observations. Using a quadratic ephemeris model, we measure a period
rate of change $\dot{P} = (3.07 \pm 0.56)\times 10^{-13}$. In addition, we use
the high timing resolution of ARCONS to examine the system's high frequency
variations and search for possible quasi-periodic oscillations (QPOs). Finally,
we use the instrument's spectral resolution to examine the light curves in
various wavelength bands. We do not find any high frequency QPOs or significant
spectral variability throughout an eclipse.
