John Stauffer, Ann Marie Cody, Luisa Rebull, Lynne A. Hillenbrand, Neal J. Turner, John Carpenter, Sean Carey, Susan Terebey, Maria Morales-Calderon, Silvia H. P. Alencar, Pauline McGinnis, Alana Sousa, Jerome Bouvier, Laura Venuti, Lee Hartmann, Nuria Calvet, Giusi Micela, Ettore Flaccomio, Inseok Song, Rob Gutermuth, David Barrado, Frederick J. Vrba, Kevin Covey, William Herbst, Edward Gillen, Marcelo Medeiros Guimaraes, Herve Bouy, Fabio Favata. 2016. CSI 2264: Characterizing Young Stars in NGC 2264 with Stochastically Varying Light Curves. Astronomical Journal 151, 3, DOI: 10.3847/0004-6256/151/3/60
We provide CoRoT and Spitzer light curves and other supporting data for 17 classical T. Tauri stars in NGC. 2264 whose CoRoT light curves exemplify the “stochastic” light curve class as defined in 2014 by Cody et al. The most probable physical mechanism to explain the optical variability within this light curve class is time-dependent mass accretion onto the stellar photosphere, producing transient hot spots. Where we have appropriate spectral data, we show that the veiling variability in these stars is consistent in both amplitude and timescale with the optical light curve morphology. The veiling variability is also well-correlated with the strength of the He I 6678 angstrom emission line, predicted by models to arise in accretion shocks on or near the stellar photosphere. Stars with accretion burst light curve morphology also have variable mass accretion. The stochastic and accretion burst light curves can both be explained by a simple model of randomly occurring flux bursts, with the stochastic light curve class having a higher frequency of lower amplitude events. Members of the stochastic light curve class have only moderate mass accretion rates. Their Ha profiles usually have blueshifted absorption features, probably originating in a disk wind. The lack of periodic signatures in the light curves suggests that little of the variability is due to long-lived hot spots rotating into or out of our line of sight; instead, the primary driver of the observed photometric variability is likely to be instabilities in the inner disk that lead to variable mass accretion.
