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We present a high angular resolution millimeter-wave dust continuum imagingsurvey of circumstellar material associated with individual components of 23multiple star systems in the Taurus-Auriga young cluster. Combined withprevious measurements, these new data permit a comprehensive look at howmillimeter luminosity (a tracer of disk mass) relates to the separation andmass of a stellar companion. Approximately one third (28-37%) of individualstars in multiples have detectable millimeter emission, a rate half that forsingle stars (~62%). There is a strong correlation between the luminosity andprojected separation (a_p) of a stellar pair. Wide pairs (a_p > 300 AU) have asimilar luminosity distribution as single stars, medium pairs (a_p ~ 30-300 AU)are a factor of 5 fainter, and close pairs (a_p < 30 AU) are ~ 5 times fainteryet (aside from a small population of bright circumbinary disks). In mostcases, the emission is dominated by a disk around the primary (or a widetertiary in triples), but there is no clear relationship between luminosity andstellar mass ratio. A direct comparison of resolved disk sizes with predictionsfrom tidal truncation models yields mixed results; some disks are larger thanexpected given their companion separations. We suggest that the presence of astellar companion impacts disk properties at a level comparable to the internalevolution mechanisms operating in isolated systems, with both the multiple starformation process itself and star-disk tidal interactions likely playingimportant roles in the evolution of disk material. From the perspective of themass content of the disk, we expect that (giant) planet formation is inhibitedaround the components of close pairs or secondaries, but should be as likely asfor single stars around the primaries (or wide tertiaries in hierarchicaltriples) in more widely-separated multiple star systems.

A Resolved Census of Millimeter Emission from Taurus Multiple Star Systems