  We obtained mid-infrared spectra of chondrules, matrix, CAIs and bulk
material from primitive type 1-4 chondrites in order to compare them with the
dust material in young, forming solar systems and around comets. Our aim is to
investigate whether there are similarities between the first processed
materials in our early Solar System and protoplanetary disks currently forming
around other stars. Chondrule spectra can be divided into two groups. 1)
Chondrules dominated by olivine features at 11.3 micron and 10.0 micron. 2)
mesostasis rich chondrules that show main features at 10 micron. Bulk ordinary
chondrites show similar features to both groups. Fine-grained matrix is divided
into three groups. 1) phyllosilicate-rich with a main band at 10 micron, 2)
olivine-rich with bands at 11.3 micron and 10 micron, 3) pyroxene rich. Impact
shock processed matrix from Murchison (CM2) shows features from
phyllosilicate-rich, amorphous and olivine rich material. Astronomical spectra
are divided into four groups based on their spectral characteristics, amorphous
(group 1), pyroxene rich (group 2), olivine rich (group 3) and complex (group
4). Group 2 is similar to enstatite-rich fine grained material like e.g.
Kakangari (K3) matrix. Group 3 and 4 can be explained by a combination of
varying concentrations of olivine and mesostasis rich chondrules and fine
grained matrix, but also show very good agreement with shock processed
material. Comparison of band ratios confirms the similarity with chondritic
material e.g. for HD100546, while the inner disk of HD142527 show no sign of
chondrule material. Comparison between spectra indicate a general similarity
between primitive solar system materials and circumstellar dust and comets.
