Condensation and growth of hydrogenated carbon clusters in carbon-rich stars
G. Pascoli and
Received 22 September 1999 / Accepted 28 February 2000
Hydrogenated carbon cluster growth in carbon-rich stellar atmospheres is simulated by a model which takes into account the simultaneous formation of carbon compounds with carbon atoms under various states of hybridization. A grid of computations shows that a mixture of different species can appear (small hydrogenated carbon clusters, carbon chains or ring-shaped structures, aromatic-like entities, etc.) depending on both carbon to hydrogen relative abundance and temperature of the star. Dehydrogenation rate and sp2/sp and sp3/sp ratios are estimated.
Key words: molecular processes stars: circumstellar matter ISM: general ISM: molecules
This article contains no SIMBAD objects.
© European Southern Observatory (ESO) 2000
Online publication: July 7, 2000