The infrared continuum spectrum of VY Canis Majoris

We combine spectra of VY CMa obtained with the short- and long-wavelength s pectrometers, SWS and LWS, on the Infrared Space Observatory(3) to provide a first detailed continuum spectrum of this highly luminous star. The circu mstellar dust cloud through which the star is observed is partially self-ab sorbing, which makes for complex computational modeling. We review previous work and comment on them range of uncertainties about the physical traits and mineralogical composition of the modeled disk. We show that these uncer tainties significantly affect the modeling of the outflow and the estimated mass loss. In particular, we demonstrate that a variety of quite diverse m odels can produce good fits to the observed spectrum. If the outflow is ste ady, and the radiative repulsion on the dust cloud dominates the star's gra vitational attraction, we show that the total dust mass loss rate is simila r to4 x 10(-6) M-circle dot yr(-1), assuming that the star is at. a distanc e of 1.5 kpc. Several indications, however, suggest that the outflow from t he star may be spasmodic. We discuss this and other problems facing the con struction of a physically coherent model of the dust cloud and a realistic mass-loss analysis.