The motion of wind-driven shells

Details The motion of wind-driven shells The motion of wind-driven shells

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006mnras.369..860c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 369, Issue 2, pp. 860-866.

Astronomy and Astrophysics

Astronomy

2

Stars: Mass-Loss: Stars: Pre-Main-Sequence: Ism: Jets And Outflows: Ism: Kinematics And Dynamics, Stars: Mass-Loss, Stars: Pre-Main-Sequence, Ism: Jets And Outflows, Ism: Kinematics And Dynamics

Scientific paper

We present a method for solving problems in which a stellar wind interacts with the surrounding environment through the production of a `double radiative shock' structure. This condition is generally met in problems involving winds ejected from young stars. We describe a method that can be applied to problems of winds with arbitrary time and angular dependence, interacting with a stationary environment with an arbitrary density distribution. We apply the method to the interaction of: a steady wind (with an instantaneous `turning-on') with a power-law environmental density stratification, a `wind plus jet' ejection with a toroidal environmental density stratification, and to the interaction of an isotropic wind with a clumpy environment. These three examples illustrate the wide range of possible applications of the proposed method. We also show a comparison between some of our thin-shell solutions and three-dimensional isothermal gasdynamic simulations of the flows. These comparisons are used as an evaluation of the applicability of our thin-shell solutions to the real flows.

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