We use Spitzer data to infer that the small infrared excess of V819 Tau , a weak-lined T Tauri star in Taurus , is real and not attributable to a “ companion ” 10″ to the south .
We do not confirm the mid-infrared excess in HBC 427 and V410 X-ray 3 , which are also non-accreting T Tauri stars in the same region ; instead , for the former object , the excess arises from a red companion 9″ to the east .
A single-temperature blackbody fit to the continuum excess of V819 Tau implies a dust temperature of 143 K ; however , a better fit is achieved when the weak 10 and 20 \mu m silicate emission features are also included .
We infer a disk of sub- \mu m silicate grains between about 1 AU and several 100 AU with a constant surface density distribution .
The mid-infrared excess of V819 Tau can be successfully modeled with dust composed mostly of small amorphous olivine grains at a temperature of 85 K , and most of the excess emission is optically thin .
The disk could still be primordial , but gas-poor and therefore short-lived , or already at the debris disk stage , which would make it one of the youngest debris disk systems known .