Volume 432, Number 2, March III 2005
|Page(s)||547 - 557|
|Section||Interstellar and circumstellar matter|
|Published online||02 March 2005|
The 90–110 μm dust feature in low to intermediate mass protostars: Calcite?*
Laboratoire d'Astrophysique, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex 09, France e-mail: firstname.lastname@example.org
2 Kapteyn Astronomical Instute, BO Box 800, 9700 AV Groningen, The Netherlands
3 CESR CNRS - UPS, BP 4346, 31028, Toulouse Cedex 04, France
Accepted: 25 October 2004
We present ISO spectra between 60 and 180 μm of 32 protostars of low to intermediate mass. About half of the spectra present a dust feature between ~90 and ~110 μm. We describe the observational characteristics of this feature, which seems to be due to one single carrier. In Class 0 sources the feature peaks around 100 μm, while in AeBe stars it peaks around 95 μm. The feature peak position seems to mostly depend on the temperature of the dust of the source, suggesting reprocessing of the dust. We present arguments for the identification of the observed feature as due to calcite, and estimate that about 10% to 30% of elemental Ca is locked up in it. Therefore, calcite seems to be formed relatively easily around protostars despite the observation that on Earth it needs aqueous solutions. This rises the question of whether conditions simulating liquid water are common around forming stars and what creates them.
Key words: ISM: abundances / ISM: molecules / stars: formation / ISM: dust, extinction / ISM: lines and bands / infrared: ISM
© ESO, 2005
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