Hostname: page-component-586b7cd67f-vdxz6 Total loading time: 0 Render date: 2024-11-25T13:39:45.387Z Has data issue: false hasContentIssue false
  • English
  • Français

Abundance of CH+ in Translucent Molecular Clouds: Problems for Shock Models?

Published online by Cambridge University Press:  07 August 2017

R. Gredel ,
E.F. Van Dishoeck  and
J.H. Black
R. Gredel
Affiliation:
European Southern Observatory, Casilla 19001, Santiago 19, Chile
E.F. Van Dishoeck
Affiliation:
Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands
J.H. Black
Affiliation:
Steward Observatory, Univ. of Arizona, Tucson, AZ 85721, USA

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The large abundance of CH+ in diffuse clouds has been a mystery for more than 50 years (Dalgarno 1976). Many different explanations have been proposed, but only (shock) models with a substantial column of warm gas appear capable of approaching the observed column densities (Elitzur and Watson 1978). In these models, CH+ is formed in the warm postshock gas through the reaction C+ + H2 → CH+ + H, which is endoergic by 4650 K. Although the most sophisticated MHD shock models are consistent with various observational aspects of CH+, they require substantial “fine-tuning” of the parameters (Draine and Katz 1986; Hartquist et al. 1990). In addition, they predict a shift in velocity between CH+ and other molecules found in the cold quiescent gas, which is not observed in recent data (e.g. Crawford 1989). In order to test further the shock models, we have searched for CH+ in a number of translucent clouds (AV ≍ 1-5 mag), which have H2 column densities that are up to an order of magnitude larger than the clouds studied so far (cf. Souza 1979). Observations of the chemically related molecules CH, C2, CN and CO have been obtained as well.

Type
Diffuse, Translucent and High-Latitude Clouds
Information
Symposium - International Astronomical Union , Volume 150: Astrochemistry of Cosmic Phenomena , 1992 , pp. 153 - 154
Copyright
Copyright © Kluwer 1992 

References

Crawford, I.A. 1989, MNRAS 241, 575.CrossRefGoogle Scholar
Dalgarno, A. 1976, in Atomic Processes and Applications , eds. Burke, P.G. and Moiseiwitsch, B.L. (North–Holland), p. 110.Google Scholar
Draine, B.T. and Katz, N. 1986, ApJ 310, 392.CrossRefGoogle Scholar
Duley, W.W., Hartquist, T.W., Sternberg, A., Wagenblast, R., and Williams, D.A. 1991, this conference.Google Scholar
Elitzur, M. and Watson, W.D. 1978, ApJ 222, L141.CrossRefGoogle Scholar
Gredel, R., van Dishoeck, E.F., and Black, J.H. 1991, A&A in press.Google Scholar
Hartquist, T.W., Flower, D.R., and Pineau des Forets, G. 1990, in Molecular Astrophysics—a volume honoring A. Dalgarno , ed. Hartquist, T.W. (Cambridge University), p. 99.CrossRefGoogle Scholar
Souza, S.P. 1979, PhD Thesis, State University of New York at Stony Brook.Google Scholar