The structure and evolution of the dark cloud B 164 under the influence of a bright star, π^1^ Cyg.

Details The structure and evolution of the dark cloud B 164 under the influence of a bright star, π^1^ Cyg. The structure and evolution of the dark cloud B 164 under the influence of a bright star, π^1^ Cyg.

Aug 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...312..989p&link_type=abstract

Astronomy and Astrophysics, v.312, p.989-999

Astronomy and Astrophysics

Astrophysics

6

Hydrodynamics, Ism: Individual Objects: B 164, Ism: Kinematics And Dynamics, Ism: Clouds, Stars: {Pi}^1^ Cyg, Radio Lines: Ism

Scientific paper

We present ^12^CO, ^13^CO and C^18^O (J: 1->0) and (J: 2->1) observations of B 164. This large Bok globule (Bok & Cordwell 1973) is interesting because it is isolated, has a peculiar velocity profile and seems to have been recently compressed on its western side. Assuming that this globule was originally spherical and in rotation, we try to interpret the ^13^CO and C^18^O data with a Berne's (1978, 1979) type Monte-Carlo radiative transfer model in which we have introduced rotation. The best solution indicates a large envelope of outwards-decreasing density from 1000cm^-3^ to 100cm^-3^ and a relatively small core with central density of the order of 5000cm^-3^. CO isotopomers have a very low abundance in this model with the ^13^CO abundance in the range 10^-7^-3x10^-6^ and C^18^O=~1-2x10^-8^. Next, we show that if π^1^ Cyg (Azelfafage, HD 206672), a Be3-III star is at the same distance as B 164 from us, it could be the progenitor of the observed compression. Using a chemico-hydro-dynamical (CHD) model (Breart de Boisanger et al. 1992) we show that the most probable explanation is that the star has just arrived close enough to the cloud to efficiently compress it via the heating of the diffuse interstellar medium and/or the increase in radiation pressure.

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