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--- abstract: 'We report on the analysis of the [[*Kepler *]{}]{}short-cadence (SC) light curve of V344 Lyr obtained during 2009 June 20 through 2010 Mar 19 (Q2–Q4). The system is an SU UMa star showing dwarf nova outbursts and superoutbursts, and promises to be a touchstone for CV studies for the foreseeable future. The system displays both positive and negative superhumps with periods of 2.20 and 2.06-hr, respectively, and we identify an orbital period of 2.11-hr. The positive superhumps have a maximum amplitude of $\sim$0.25-mag, the negative superhumps a maximum amplitude of $\sim$0.8 mag, and the orbital period at quiescence has an amplitude of $\sim$0.025 mag. The quality of the [[*Kepler *]{}]{}data is such that we can test vigorously the models for accretion disk dynamics that have been emerging in the past several years. The SC data for V344 Lyr are consistent with the model that two physical sources yield positive superhumps: early in the superoutburst, the superhump signal is generated by viscous dissipation within the periodically flexing disk, but late in the superoutburst, the signal is generated as the accretion stream bright spot sweeps around the rim of the non-axisymmetric disk. The disk superhumps are roughly anti-phased with the stream/late superhumps. The V344 Lyr data also reveal negative superhumps arising from accretion onto a tilted disk precessing in the retrograde direction, and suggest that negative superhumps may appear during the decline of DN outbursts. The period of negative superhumps has a positive $\dot P$ in between outbursts.' author: - 'Matt A. Wood, Martin D. Still, Steve B. Howell, John K. Cannizzo Alan P. Smale' title: 'V344 Lyrae: A Touchstone SU UMa Cataclysmic Variable in the Kepler Field' --- Introduction ============ Cataclysmic variable (CV) binary systems typically consist of low-mass main sequence stars that transfer mass though the L1 inner Lagrange point and onto a white dwarf primary via an accretion disk. Within the disk, viscosity acts to transport angular momentum outward in radius, allowing mass to move inward and accrete onto the primary white dwarf [e.g. @warner95; @fkr02; @hellier01]. In the case of steady-state accretion the disk is the brightest component of the system, with a disk luminosity $L_{\rm disk} \sim GM_1 \dot M_1/R_1$, where $\dot M_1$ is the mass accretion rate onto a white dwarf of mass $M_1$ and radius $R_1$. While members of the novalike (NL) CV subclass display a nearly constant mean system luminosity, members of the dwarf nova (DN) subclass display quasi-periodic outbursts of a few magnitudes thought to arise from a thermal instability in the disk. Specifically, models suggest a heating wave rapidly transitions the disk to a hot, high-viscosity state which significantly enhances $\dot M_1$ for a few days. Furthermore, within the DN subclass there are the SU UMa systems that in addition to normal DN outbursts display superoutbursts which are up to a magnitude brighter and last a few times longer than the DN outbursts. The SU UMa stars are characterized by the appearance at superoutburst of periodic large-amplitude photometric signals (termed