Spectroscopic diagnostic for the mineralogy of large dust grains

Details Spectroscopic diagnostic for the mineralogy of large dust grains Spectroscopic diagnostic for the mineralogy of large dust grains

2003-10-30

arxiv.org/abs/astro-ph/0310863v1

Astron.Astrophys. 413 (2004) L35-L38

Astronomy and Astrophysics

Astrophysics

Submitted to A&A Letters

Scientific paper

10.1051/0004-6361:20031699

We examine the thermal infrared spectra of large dust grains of different chemical composition and mineralogy. Strong resonances in the optical properties result in detectable spectral structure even when the grain is much larger than the wavelength at which it radiates. We apply this to the thermal infrared spectra of compact amorphous and crystalline silicates. The weak resonances of amorphous silicates at 9.7 and 18 micron virtually disappear for grains larger than about 10 micron. In contrast, the strong resonances of crystalline silicates produce emission dips in the infrared spectra of large grains; these emission dips are shifted in wavelength compared to the emission peaks commonly seen in small crystalline silicate grains. We discuss the effect of a fluffy or compact grain structure on the infrared emission spectra of large grains, and apply our theory to the dust shell surrounding Vega.

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