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Title:
Carbonaceous Dust in Planetary Systems: Origin and Astrobiological Significance
Authors:
Caro, G. M. Munoz; Martinez-Frias, J.
Publication:
Workshop on Dust in Planetary Systems (ESA SP-643). September 26-30 2005, Kauai, Hawaii. Editors: Krueger, H. and Graps, A., p.133-138
Publication Date:
01/2007
Origin:
ADS
Bibliographic Code:
2007ESASP.643..133C

Abstract

A brief overview of astrobiologically relevant organic species detected in small solar system bodies, in particular meteorites, is provided. Such organic molecules, however, are only a minor component of the carbon in these objects. Many of them, like amino acids, probably the most interesting family of molecules for astrobiology, have not yet been detected in the interstellar medium. Most of the carbon is present as the so-called macromolecular organic material, both in meteorites and interplanetary dust particles. We show that material is analogous to hydrogenated amorphous carbon, a hydrocarbon widely studied by chemists. A form of hydrogenated amorphous carbon is also observed in grains toward the diffuse interstellar medium, and even in Seyfert 2 galaxies, although with different chemical properties. Therefore, in our attempt to trace the evolution of carbonaceous matter as the local interstellar cloud collapsed leading to the formation of the solar nebula, we focus on the study of an ubiquitous form of carbon, namely hydrogenated amorphous carbon.
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