Is HS 240 an interstellar bubble?

Details Is HS 240 an interstellar bubble? Is HS 240 an interstellar bubble?

Sep 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...221..311w&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 221, no. 2, Sept. 1989, p. 311-320.

Astronomy and Astrophysics

Astronomy

6

Astronomical Spectroscopy, H Ii Regions, Interstellar Matter, O Stars, Stellar Winds, Cosmic Dust, Electron Density (Concentration), Emission Spectra, Infrared Astronomy Satellite, Spectral Line Width

Scientific paper

Radio, optical, and infrared observations of the galactic H II region HS 240 = S 119 around the O 7.5 V star 68 Cyg are presented. No evidence is found that the extended nebular structure may have formed under the action of a strong stellar wind. The measured emission line strengths are typical for a low-excitation nebula. The electron temperature, derived from optical line widths, is (7500 + or - 1000) K. The large-scale emission measure distribution is rather uniform, with an average electron density of about 2/cu cm. There are indications that at least part of the gas is concentrated in small clumps of densities not higher than about 100/cu cm. The measured dust color temperature is 41 K averaged over the whole H II region. The infrared emission distribution - not ring-like but centered on the star - demonstrates that the inner region is not a wind-blown cavity.

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