Winds in collision. III - Modeling the interaction nebulae of eruptive symbiotics

Details Winds in collision. III - Modeling the interaction nebulae of eruptive symbiotics Winds in collision. III - Modeling the interaction nebulae of eruptive symbiotics

Sep 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...183..247g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 183, no. 2, Sept. 1987, p. 247-256.

Astronomy and Astrophysics

Astrophysics

107

Collisions, Nebulae, Stellar Mass Ejection, Stellar Models, Stellar Winds, Symbiotic Stars, Conservation Equations, Mass Distribution, Momentum Theory, Stellar Envelopes, Stellar Structure, Velocity Distribution

Scientific paper

Observations of HM Sge and V1016 Cyg have been interpreted (Wallerstein et al., 1984; Wilson et al., 1984) in terms of two colliding stellar winds in an interacting binary. Here, a simplified model for the structure of the nebula which forms at the interface of the colliding winds is developed, based on momentum conservation. From this model, the geometry, mass distribution, and velocity distribution of the nebula can be found as a function of the parameters of the colliding stellar winds which sustain it. Under the assumption of negligible orbital motion, the nebular shell reaches a steady-state configuration. Its shape is roughly conical, with the cone apex angle determined by a single parameter. The time development of a cross-section of the nebula which forms in a system with nonnegligible orbital motion is also calculated, under the assumption that the nebular shell is thin relative to its overall dimensions.

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