2008/10/23 by Vikram V Dwarkadas, V V Dwarkadas
Physics and Astronomy · #Astrophysics and Star Formation Studies #Solar and Space Plasma Dynamics #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1088/0031-8949/2008/t132/014024
12 pages, 5 Figs, in proceedings of "Turbulent Mixing and Beyond". This is an author-created, un-copyedited version accepted for publication to Physica Scripta T. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The definitive publisher authenticated version will be available online
arxiv created 2008/10/23 · openalex publication_date 2008/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
Winds from massive stars (> 8 solar masses) result in the formation of wind-blown 'bubbles' around these stars. In this paper we study, via two-dimensional (2D) numerical hydrodynamic simulations, the onset and growth of turbulence during the formation and evolution of these wind-blown 'bubbles'. Our simulations reveal the formation of vortex rolls during the main-sequence stage of the evolution, and Rayleigh–Taylor instabilities in the subsequent stages due to accelerating and/or decelerating wind-blown shells. The bubble shows a very turbulent interior just prior to the death of the star, with a significant percentage of the internal energy expended in non-radial motions. This would affect the subsequent evolution of the resultant supernova shock wave. We discuss the implications of these results, show how the ratio of kinetic energy in radial versus non-radial motions varies throughout the evolution, and discuss how these results would carry over to 3D.