Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282..657o&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 2, p. 657-662
Astronomy and Astrophysics
Astrophysics
6
Comets, Infrared Spectra, Interplanetary Dust, Mass Ratios, Olivine, Silicon Carbides, Absorption Spectra, Chemical Composition, Emission Spectra, Silicates, Comets, Dust, Silicon Carbide, Composition, Emissions, Silicates, Idps, Wavelength, Infrared, Absorption, Spectra, Comparison, Analogs, Olivine, Grains, Laboratory Studies, Spectroscopy, Model, Parameters, Meteorites, Flux Density, Kohoutek, Wilson, Halley, Bradfield
Scientific paper
The 10 micrometer emission band observed in four different comets (Kohoutek, Wilson, Halley and Bradfield) has been generally attributed to silicates. In particular, the 11.3 micrometer substructure of the band has been fitted, up to now, using labortory data of crystalline olivine grains contained in interplanetary dust particles (IDPs). Also terrestrial olivine grains exhibit an 11.3 micrometer absorption feature when they are embedded in potassium bromide (KBr) matrices for infrared spectrosocpy. Therefore, since the grains are not in vacuum, a shift of about 0.3 micrometers of the peak position must be considered in order to take into account matrix effects. Such effects could also influence the spectrum of olivine-IDPs due to the experimental technique used to obtain the spectroscopic data In this case the attribution to olivine of the 11.3 micrometers, cometary substructure may be questioned. Another suitable candidate could be silicon carbon (SiC) which exhibits an absorption band in vacuum at 11.3 micrometers. To investigate such possiblity, we present here fits of the four cometary spectra obtained using a mixture of synthetic amorphous olivine and SiC particles. Using the results found for our best-fit parameters we estimate that the ratio between the mass of silicon locked in SiC grains and the total mass of this element in the cometary dust is of the order of 3 x 10-2.
Blanco Ariel
Fonti Sergio
Orofino Vincenzo
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