THE FU ORIONIS OUTBURST AS A THERMAL ACCRETION EVENT - OBSERVATIONAL CONSTRAINTS FOR PROTOSTELLAR DISK MODELS

The results of the time-dependent disk models developed in Bell and Lin are compared with observed properties of FU Orionis variables. Specific models are fit to the light curves of FU Ori, V1515 Cyg, and V1057 Cyg. The slow risetime of V1515 Cyg can be matched by a self-regulated outburst model. The rapid risetimes of FU Ori and V1057 Cyg can be fitted with the application of modest perturbations to the disk surface density. Model disks display spectral features characteristic of observed objects. The color evolution of V1057 Cyg is naturally explained if mass flux drops in the inner disk (tau < 1/4 AU) while remaining steady in the outer disk. The decrease in optical line width (rotational velocity) observed during the decay of V1057 Cyg may be accounted for by an outward-propagating ionization front. We predict that before final decay to the quiescent phase, short-wavelength line widths (lambda < 1.5 mu m) will again increase. It is suggested that FU Orionis outbursts primarily occur to systems during the embedded phase with ages less than several times 10(5) yr.