On the CH(+) ion in diffuse interstellar clouds

Details On the CH(+) ion in diffuse interstellar clouds On the CH(+) ion in diffuse interstellar clouds

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...303..401l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 303, April 1, 1986, p. 401-415. Research supported by the Robert A. Welch F

Astronomy and Astrophysics

Astrophysics

81

Gas Density, Hydrocarbons, Interstellar Matter, Line Spectra, Molecular Clouds, Molecular Ions, Abundance, Interstellar Chemistry, Milky Way Galaxy, Reaction Kinetics, Southern Sky, Spectrum Analysis

Scientific paper

A survey of 65 lines of sight in the southern Milky Way for the interstellar line of CH(+) at 4232 A yielded 30 detections. The CH(+) column density N(CH+) is shown to be well correlated with the rotationally excited H2 detected by surveys with the Copernicus satellite: log N(CH+)/N(H2)ex inversely proportional to 2500/T(ex), where T(ex) is the excitation temperature of H2 provided by the observed populations in rotational levels J of about 3-5. This correlation is strong evidence that CH(+) is formed in warm gas where the reaction C(+) + H2 yields CH(+) + H is effective. Shocks probably provide the necessary heating.

Affiliated with

Also associated with

No associations

Rating

On the CH(+) ion in diffuse interstellar clouds does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with On the CH(+) ion in diffuse interstellar clouds, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On the CH(+) ion in diffuse interstellar clouds will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1101831