Two-dimensional models of stellar wind bubbles. I - Numerical methods and their application to the investigation of outer shell instabilities

Details Two-dimensional models of stellar wind bubbles. I - Numerical methods and their application to the investigation of outer shell instabilities Two-dimensional models of stellar wind bubbles. I - Numerical methods and their application to the investigation of outer shell instabilities

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...143...59r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 143, no. 1, Feb. 1985, p. 59-71.

Statistics

Computation

109

Computational Fluid Dynamics, Interstellar Matter, Magnetohydrodynamic Stability, Plasma Bubbles, Stellar Envelopes, Stellar Winds, Two Dimensional Models, Herbig-Haro Objects, Molecular Flow, Nebulae, Nonadiabatic Theory, Perturbation, Radiative Heat Transfer, Stellar Models, Thin Walled Shells

Scientific paper

This paper is the first of a series on the evolution and stability of stellar wind bubbles. Interactions between winds and the interstellar medium are dealt with, but processes leading to wind generation and acceleration are not studied. In the present paper a second order two-dimensional hydrodynamical code is developed and shown to have clear advantages over widely used first-order schemes. Its application range is discussed and research perspectives are outlined. The code is tested on existing analytical solutions for the internal structure of wind bubbles. Models of spherically symmetric adiabatic bubbles are shown to be quantitatively correct. A good qualitative agreement with one-dimensional numerical models is also achieved when radiative energy losses are taken into account. Outer shells of radiative models are tested for stability against density and velocity perturbations. It is shown that contrary to common belief they cannot fragment as soon as they cool. The instability of the shell is not a pure thermal one and its growth time is much longer than the cooling time.

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