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Molecular richness of the diffuse interstellar medium: a signpost of turbulent dissipation

Published online by Cambridge University Press:  21 March 2013

Edith Falgarone ,
Benjamin Godard ,
Guillaume Pineau des Forêts  and
Maryvonne Gerin
Edith Falgarone
Affiliation:
LERMA/LRA, Ecole Normale Supérieure & Observatoire de Paris, 24 rue Lhomond, 75005 Paris, France email: edith.falgarone@ens.fr
Benjamin Godard
Affiliation:
LUTh, Observatoire de Paris, 92195 Meudon, France email: benjamin.godard@obspm.fr
Guillaume Pineau des Forêts
Affiliation:
Institut d'Astrophysique Spatiale, 91405 Orsay, France
Maryvonne Gerin
Affiliation:
LERMA/LRA, Ecole Normale Supérieure & Observatoire de Paris, 24 rue Lhomond, 75005 Paris, France email: edith.falgarone@ens.fr
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Abstract

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The Herschel/HIFI absorption spectroscopy surveys reveal the unexpected molecular richness of the Galactic diffuse ISM, even in gas of very low average H2 molecular fraction. In particular, two hydrides, CH+ and SH+ with highly endoergic formation routes have abundances that challenge models of UV-driven chemistry. The intermittent dissipation of turbulence appears as a plausible additional source of energy for the diffuse ISM chemistry. We present recent results of the so-called models of Turbulent Dissipation Regions (TDR). The abundances of many of the molecules observed in the diffuse ISM, including CO that is used as a tracer of the molecular cloud mass, may be understood in the framework of the TDR models.

Keywords

astrochemistry — turbulence — magnetic fields — ISM: molecules — ISM: kinematics and dynamics — ISM: general — ISM: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 223 - 226
Copyright
Copyright © International Astronomical Union 2013

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