Vega-like systems or dust debris disks are characterized by a small
amount of circumstellar gas, the presence of planetary objects and
dust. The small solar system objects (trans-Neptunian objects,
asteroids, comets, and meteoroids) and the interplanetary dust cloud
also form a planetary debris disk, although the solar system dust
density is much lower than for the debris disks that are observed
around other stars. A large amount of observational data, though of
different kind, exist for the solar system and the Beta Pictoris
system. After discussing our basic knowledge of planetary disk
evolution, this presentation will address the existence of a
second-generation gas component and the existence of amorphous and
crystalline silicates in the solar system and around Beta Pictoris.