Interstellar CH^+^ in southern OB associations.

Details Interstellar CH^+^ in southern OB associations. Interstellar CH^+^ in southern OB associations.

Apr 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997a%26a...320..929g&link_type=abstract

Astronomy and Astrophysics, v.320, p.929-944

Astronomy and Astrophysics

Astrophysics

47

Ism: Abundances, Ism: Clouds, Ism: Molecules, Open Clusters And Associations

Scientific paper

Optical absorption line observations of interstellar CH^+^ and CH are presented towards the southern OB associations CMa OB1, NGC 2439, Vela OB1, NGC 4755, and Cen OB1. A total of 5-11 stars per association were observed, with visual extinctions ranging from A_V_=0.5-4.5mag. The derived CH^+^ and CH velocities agree within the measurement errors. Towards a particular association, the CH^+^ column density N(CH^+^) is correlated to the visual extinction of the background star. These findings weaken the possibility that magnetic shocks are the general mechanism that is required to produce interstellar CH^+^. It is found that N(CH^+^) is correlated to N(CH), which indicates that N(CH^+^) is correlated to the optical depth of a cloud. The correlations are difficult to reconcile with scenarios where the sites of CH^+^ formation are constrained to the surface of molecular clouds. The observations support ideas which involve turbulence as a major CH^+^ production mechanism. In particular, the results are in agreement with expectations from a scenario where the CH^+^ formation proceeds in cool gas via a fraction of fast, non-Maxwellian H_2_ or C^+^, created by the dissipation of interstellar turbulence.

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