Volume 369, Number 2, April II 2001
|Page(s)||589 - 593|
|Published online||15 April 2001|
Cassiopeia A dust composition and heating*
DSM/DAPNIA/Service d'Astrophysique, CEA/Saclay, 91191 Gif-sur-Yvette, France
2 Supélec, Service des Mesures, 91192 Gif-sur-Yvette, France
Corresponding author: T. Douvion, Thomas.Douvion@supelec.fr or email@example.com
Accepted: 9 January 2001
Material ejected by a supernova is directly observed in the form of Fast Moving Knots (FMK's) in the Cassiopeia A supernova remnant. Part of this material has condensed into dust. In this paper, by fitting the ISO mid-infrared emission of the dust, we derive the dust composition and discuss the dust heating. The dust is found to be made mainly of three components: pyroxene, quartz and aluminium oxide. These components have to be heated at two different temperatures, a "hot" temperature around 350 K and a cold temperature around 90 K. The physical conditions in the knot-shocked region are such that the dust can be collisionally heated to a temperature of 350 K. The cold dust temperature can also be well accounted for by the knot model discussed in the paper. The dust formation efficiency is tentatively estimated to be of the order of 10% in this supernova.
Key words: supernova remnant / supernovae individual: Cas A dust / infrared: general
© ESO, 2001
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