A stellar wind dynamic model for S 106

Details A stellar wind dynamic model for S 106 A stellar wind dynamic model for S 106

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990acasn..31..324j&link_type=abstract

(Acta Astronomica Sinica, vol. 31, no. 4, 1991, p. 324-335) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 15, June 1

Astronomy and Astrophysics

Astrophysics

Dynamic Models, H Ii Regions, Stellar Winds, Nebulae, Radio Emission, Stellar Envelopes, Thermodynamic Properties

Scientific paper

To explain the morphology of the bipolar nebula S 106, both a momentum-driven and an energy-driven shell model, are used in which time-independent mass loss, constant wind velocity and exponential decrease of circumstellar material are assumed. The results suggest that the structure of S 106 is due to the interaction of an anisotropic wind with the circumstellar gas. The optical- and radio-emission gap in the equatorial plane and the shell-like structure of the larger-scale southern lobe can be explained by the momentum-driven model.

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