  We present infrared interferometric observations of the inner regions of two
A-star debris disks, beta Leo and zeta Lep, using the FLUOR instrument at the
CHARA interferometer on both short (30 m) and long (>200 m) baselines. For the
target stars, the short baseline visibilities are lower than expected for the
stellar photosphere alone, while those of a check star, delta Leo, are not. We
interpret this visibility offset of a few percent as a near-infrared excess
arising from dust grains which, due to the instrumental field of view, must be
located within several AU of the central star. For beta Leo, the near-infrared
excess producing grains are spatially distinct from the dust which produces the
previously known mid-infrared excess. For zeta Lep, the near-infrared excess
may be spatially associated with the mid-infrared excess producing material. We
present simple geometric models which are consistent with the near and
mid-infrared excess and show that for both objects, the near-infrared producing
material is most consistent with a thin ring of dust near the sublimation
radius with typical grain sizes smaller than the nominal radiation pressure
blowout radius. Finally, we discuss possible origins of the near-infrared
emitting dust in the context of debris disk evolution models.
