Iron-aromatics coordination in molecular clouds

Details Iron-aromatics coordination in molecular clouds Iron-aromatics coordination in molecular clouds

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282..916m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 3, p. 916-923

Astronomy and Astrophysics

Astrophysics

21

Astronomical Models, Cosmic Dust, Interstellar Chemistry, Interstellar Matter, Iron, Molecular Clouds, Organometallic Compounds, Polycyclic Aromatic Hydrocarbons, Abundance, Chemical Bonds, Interstellar Extinction, Mathematical Models, Photodissociation

Scientific paper

Aromatic molecules (generally supposed to be PAHs, i.e. polycyclic aromatic hydrocarbons) are assumed to be present in the interstellar medium (ISM). Serra et al. (1992) proposed that efficient organmetallic reactions should occur in the ISM between the PAHs and the iron atoms or ions, leading to the formation of organmetallic complexes, the organmetallic bonding being of the same order of stability as an aromatic C-H bond. We present in this paper a model taking into account the formation and the photodissociation reactions inside typical cloud configurations. The results show that organmetallic complexes are stable inside interstellar clumps protected by an extinction Av c.a. 4-5 mag against the local star light or the interstellar radiation field (ISRF). The equilibrium between formation/photodissociation reactions is reached for a time scale of about 104-105 yr. A consequence of organmetallic complexation which would occur in a very short time scale (2000 yr), is that Fe would be depleted in the dense cores of molecular clouds (R7 in the rho Oph molecular complex for example)and could participate to the dust grains formation by PAH accretion.

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