EDP Sciences
Free Access
Volume 468, Number 1, June II 2007
Page(s) 171 - 188
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361:20065771
Published online 19 March 2007

A&A 468, 171-188 (2007)
DOI: 10.1051/0004-6361:20065771

Far-infrared to millimeter astrophysical dust emission

I. A model based on physical properties of amorphous solids
C. Meny1, V. Gromov1, 0, 2, N. Boudet1, J.-Ph. Bernard1, D. Paradis1, and C. Nayral1

1  Centre d'Étude Spatiale des Rayonnements, CNRS, 9 avenue du Colonel Roche, 31028 Toulouse, France
    e-mail: meny@cesr.fr; vgromov@iki.rssi.ru
2  Space Research Institute, RAS, 84/32 Profsoyuznaya, 117810 Moscow, Russia

(Received 7 June 2006 / Accepted 11 December 2006 )

Aims.We propose a new description of astronomical dust emission in the spectral region from the far-infrared to millimeter wavelengths.
Methods.Unlike previous classical models, this description explicitly incorporates the effect of the disordered internal structure of amorphous dust grains. Our model is based on results from solid state physics used to interpret laboratory data. The model takes into account the effect of absorption by disordered charge distribution, as well as the effect of absorption by localized two level systems.
Results.We review constraints on the various free parameters of the model from theory and laboratory experimental data. We show that, for realistic values of the free parameters, the shape of the emission spectrum will exhibit very broad structures whose shape will change in a non trivial way with the temperature of dust grains. The spectral shape also depends upon the parameters describing the internal structure of the grains. This opens new perspectives for identifying the nature of astronomical dust from the observed shape of the FIR/mm emission spectrum. A companion paper will provide an explicit comparison of the model with astronomical data.

Key words: dust, extinction -- diffuse radiation -- infrared: ISM -- radio continuum: ISM -- scattering -- radiation mechanisms: thermal

© ESO 2007

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