  In order to link infrared observations of dust formed during planet formation
in debris disks to mid-infrared spectroscopic data of planetary materials from
differentiated terrestrial and asteroidal bodies, we obtained absorption
spectra of a representative suite of terrestrial crustal and mantle materials,
and of typical Martian meteorites. A series of debris disk spectra
characterized by a strong feature in the 9.0-9.5 micron range (HD23514,
HD15407a, HD172555 and HD165014), is comparable to materials that underwent
shock, collision or high temperature events. These are amorphous materials such
as tektites, SiO2-glass, obsidian, and highly shocked shergottites as well as
inclusions from mesosiderites (Group A). A second group (BD+20307, Beta
Pictoris, HD145263, ID8, HD113766, HD69830, P1121, and Eta Corvi) have strong
pyroxene and olivine bands in the 9-12 micron range and is very similar to
ultramafic rocks (e.g. harzburgite, dunite)(Group B). This could indicate the
occurrence of differentiated materials similar to those in our Solar System in
these other systems. However, mixing of projectile and target material, as well
as that of crustal and mantle material has to be taken into account in large
scale events like hit-and-run and giant collisions or even large-scale
planetary impacts. This could explain the olivine-dominated dust of group B.
The crustal-type material of group A would possibly require the stripping of
upper layers by grazing-style hit-and run encounters or high energy events like
evaporation/condensation in giant collisions. In tidal disruptions or the
involvement of predominantly icy/water bodies the resulting mineral dust would
originate mainly in one of the involved planetesimals. This could allow
attributing the observed composition to a specific body (such as e.g. Eta
Corvi).
