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Based on more than four weeks of continuous high cadence photometricmonitoring of several hundred members of the young cluster NGC 2264 with twospace telescopes, NASA's Spitzer and the CNES CoRoT (Convection, Rotation, andplanetary Transits), we provide high quality, multi-wavelength light curves foryoung stellar objects (YSOs) whose optical variability is dominated by shortduration flux bursts, which we infer are due to enhanced mass accretion rates.These light curves show many brief -- several hour to one day -- brighteningsat optical and near-infrared (IR) wavelengths with amplitudes generally in therange 5-50% of the quiescent value. Typically, a dozen or more of these burstsoccur in a thirty day period. We demonstrate that stars exhibiting this type ofvariability have large ultraviolet (UV) excesses and dominate the portion ofthe u-g vs. g-r color-color diagram with the largest UV excesses. These starsalso have large Halpha equivalent widths, and either centrally peaked, lumpyHalpha emission profiles or profiles with blue-shifted absorption dipsassociated with disk or stellar winds. Light curves of this type have beenpredicted for stars whose accretion is dominated by Rayleigh-Taylorinstabilities at the boundary between their magnetosphere and innercircumstellar disk, or where magneto-rotational instabilities modulate theaccretion rate from the inner disk. Amongst the stars with the largest UVexcesses or largest Halpha equivalent widths, light curves with this type ofvariability greatly outnumber light curves with relatively smooth sinusoidalvariations associated with long-lived hot spots. We provide quantitativestatistics for the average duration and strength of the accretion bursts andfor the fraction of the accretion luminosity associated with these bursts.

CSI 2264: Characterizing Accretion-Burst Dominated Light Curves for Young Stars in NGC 2264