The formation of broad molecular line wings in turbulent boundary layers

Details The formation of broad molecular line wings in turbulent boundary layers The formation of broad molecular line wings in turbulent boundary layers

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992mnras.257..419h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 257, no. 3, Aug. 1, 1992, p. 419-422.

Astronomy and Astrophysics

Astronomy

26

Carbon Monoxide, Interstellar Matter, Molecular Clouds, Molecular Gases, Turbulent Boundary Layer, Carbon 12, Carbon 13, Interstellar Chemistry, Molecular Ions

Scientific paper

The broad (about 10 km/s) component seen in the CH(+) absorption feature toward Zeta Oph and the narrower (about 3 km/s) component are compatible with the CH(+) existing at the interface between a diffuse molecular cloud and a more tenuous medium flowing at about 300 km/s. The broad component arises in the turbulent boundary layer at the interface and the narrow component forms in underlying molecular gas which has approached the interface but has not entered the more turbulent parts of the boundary layer. The narrow-component gas is heated by the dissipation of waves generated in the turbulent boundary layer and propagating toward the cloud. A broad component in a CO emission feature, like those observed toward large dense molecular clouds even where no internal stellar sources exist, can arise in a turbulent boundary layer between a dense cloud and an external flowing medium. However, for a broad CO component to form in this way, flow from the cloud must be rapid enough (about 1 km/s for a hydrogen molecule number density of 100/cu cm) to drive the CO dissociating zone to and somewhat beyond the boundary layer.

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