The vicinity of Omicron Per

Details The vicinity of Omicron Per The vicinity of Omicron Per

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...185..297b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 185, no. 1-2, Oct. 1987, p. 297-305.

Astronomy and Astrophysics

Astrophysics

11

Astronomical Maps, B Stars, Dark Matter, Emission Spectra, Line Spectra, Molecular Clouds, Abundance, Infrared Spectra, O Stars, Spectral Resolution, Ultraviolet Spectra, Visible Spectrum

Scientific paper

The authors have mapped the region around the B1 III star ο Per (HD 23180) in the emission of the J = 1-0 and J = 2-1 lines of 12CO and 13CO with ≈1 arcmin resolution. The molecular cloud morphology suggests the presence of a warm hole near the position of the star. It is tempting to think that ο Per is the cause of this molecular gap. However, the observed heating of the cloud edge, as well as optical, infrared (IRAS) and carbon recombination line data, all suggest that the local ultraviolet field is enhanced only by a factor 10 - 100. Therefore ο Per must be located at least a few parsecs away from the cloud, and the precise alignment of the observed hole with the star is probably mainly due to chance. Furthermore, other neighbouring OB stars (mainly BD +31°643, ζ Per and X Per) could contribute appreciably (even more than ο Per) to the ultraviolet enhancement which seems extend over several degrees on the north-east edge of the Perseus local molecular cloud.

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