A dynamic model for the outer nebula of R Aquarii
W. J. Henney & J. E. Dyson, University of Manchester, UK
Astronomy & Astrophysics 261, 301-313
Abstract:
The symbiotic star R Aquarii is surrounded by a
complex extended emission nebulosity. We model the lenticular outer
nebula as the interaction of a fast wind from an accretion disk with
inhomogeneously distributed ambient gas. The ambient gas is swept up
into a thin shell which becomes elongated in the direction of the
steepest density gradient. We investigate a variety of ambient density
distributions and we show that the gross morphology, kinematics and
optical appearance of the nebula can be reproduced by such a model
under the assumption that the emission is produced by optically thin
shock-heated gas. In the best-fit model, the ambient gas has a number
density of 10 cm-3 in the orbital plane of the system and falls off
exponentially above and below this plane. We deduce the mass loss rate
of the fast wind to be of order 10-10 solar mass/yr for an
assumed fast wind velocity of 1000 km/s, and we show this to be
broadly consistent with observations.
Available as.............
Will Henney <will@astroscu.unam.mx>
Last modified: Tue Dec 19 16:17:35 CST 1995