Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...184..284m&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 184, no. 1-2, Oct. 1987, p. 284-290.
Astronomy and Astrophysics
Astrophysics
19
Hydrogen Clouds, Masers, Molecular Clouds, Stellar Evolution, Absorption Spectra, Ammonia, Carbon Monoxide
Scientific paper
The molecular cloud surrounding the H II region G 34.3+0.2 has been extensively mapped in the J = 1→0, J = 2→1 transitions of 12CO and 13CO and in the J = 1→0, J = 3→2 transitions of HCO+. Interpretation of the emission is complicated by a deep self absorption feature observed in all spectra and attributed to a tenuous foreground cloud which is moving towards the core of the cloud. The mass of the cloud is estimated from 13CO observations to be greater than 103M_sun;. A comparison of the J = 1→0 and J = 3→2 HCO+ line intensities, together with the observed similarity of the HCO+ and 13CO maps, indicate the existence of dense condensations (molecular hydrogen density ≡106cm-3) in the core. A blue shifted high velocity molecular outflow is observed in 13CO and 12CO to the NW of the H II region. It is suggested that the driving force for the outflow is a stellar wind which is also responsible for the bipolar appearance of the H II region.
Andersson Mauritz
Davies Steven R.
Dent William R. F.
Little Leslie T.
Macdonald G. H.
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