Infrared and Millimeter Observations of Inner and Outer Disks around
disk material surrounding young stars determine the early environmental
conditions that influence the development of planetary systems and
provide constraints on theoretical models of star and planet formation.
At infrared wavelengths, we are exploiting the exceptional angular
resolution of the Keck interferometer to resolve the hot inner disks of
classical and weak-lined T Tauri stars at sub-AU scales. With the Owens
Valley Millimeter Array (OVRO) we are targeting Class I and Class II
young binaries in Taurus and Ophiuchus to determine the distribution
and evolution of cool dust in the outer disks.
The K-band Keck interferometry measurements of several pre-Main
Sequence stars show calibrated squared visibilities significantly less
than unity, indicating spatially resolved sources. By modeling the
visibility as arising from an unresolved star and a resolved disk the
size of the inner disk can be estimated. The inferred sizes are more
consistent with disk models incorporating a puffed-up inner edge at the
dust destruction radius than standard flared disk models.
The OVRO 3mm continuum maps of the Ophiuchus binaries reveal that the
dust emission is dominated by the primary, even at the Class I stage.
The circumprimary disks have masses that are comparable to the Minimum
Mass Solar Nebula and show evidence for grain growth. The nondetection
of massive secondary disks suggests a dissipation timescale that may
negatively impact planet formation. One Ophiuchus secondary is detected
in line emission with the unique combination of a CO gas disk without a
corresponding dust disk detection