Abstract
We present Keck Interferometer observations of TW Hya that spatially resolve its emission at 2 μm wavelength. Analyzing these data together with existing K-band veiling and near-infrared photometric measurements, we conclude that the inner disk consists of optically thin, submicron-sized dust extending from ~4 AU to within 0.06 AU of the central star. The inner disk edge may be magnetospherically truncated. Even if we account for the presence of gas in the inner disk, these small dust grains have survival times against radiation blowout that are orders of magnitude shorter than the age of the system, suggesting continual replenishment through collisions of larger bodies.
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