An infrared shell in the CYG X - CYG OB 1 region

Details An infrared shell in the CYG X - CYG OB 1 region An infrared shell in the CYG X - CYG OB 1 region

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990azh....67.1152l&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 67, Nov.-Dec. 1990, p. 1152-1164. In Russian.

Astronomy and Astrophysics

Astronomy

9

Infrared Astronomy, Interstellar Matter, Star Clusters, Brightness Distribution, Cygnus Constellation, Infrared Astronomy Satellite, Molecular Clouds, Star Formation, Stellar Winds, Wolf-Rayet Stars

Scientific paper

IRAS data were processed to look for evidence of physical interaction of the young stellar groups Cyg OB 1 - Be 86 - Be 87 - NGC 6913 - IC 4996 with the molecular cloud complex. The infrared brightness distribution reveals a shell-like structure: a half-ring of about 3 deg with center at about l = 77 deg, b = 0.5 deg, is most visible at 60 and 100 microns. The IR shell is shown to be most probably associated with Be 87, which includes the star WR 142 (spectral class WO 2), with the star-forming region ON 2, and with the giant molecular cloud at the distance d = 950 pc, but a physical connection of the dust shell with Cyg OB 1 (d = 1.8 kpc) cannot be ruled out. The measured dust color temperature is T(60/100) = 29-30 K and the mass of the gas in the shell is M = 1000 x (d/1kpc)-squared solar masses. It is shown that the IR shell might result from the action of the stellar wind of the Wolf-Rayet and Of stars in it. The "superwind" of WR 142 is probably not the prevailing factor, in view of its short duration.

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