The structure of inner region of protoplanetary disks around young
pre-main-sequence stars is still poorly understood. This part of the
disk is shaped by various forces influencing dust and gas dynamics and
by dust sublimation, which creates abrupt drops in the dust density.
This region also emits a strong near-infrared flux that cannot be
explained by classical accretion disk models, which suggests the
existence of some unusual dust distribution or disk shape. In this
talk I will show why we still lack a convincing description of this
part of the disk and why it presents unusually difficult problem for
radiative transfer methods.
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