Speaker
Description
The results of one-dimensional stellar evolution models depend on recipes for convection, mixing, and diffusion deep inside the stars. Three-dimensional simulations are required to make more reliable models that are independent of the choice of these recipes. In addition, the three-dimensional models show asymmetries which may aid the subsequent neutrino driven explosion. We have simulated seven minutes of oxygen burning phase of a massive star (18.88 $\rm M_{\odot}$) prior to collapse. The initial model is unstable against convection and with time we observe the development of large scale modes in the flow. The behavior of convection is quite different in such a system. Convective eddies bring lighter elements into the inner burning zone where they can be burnt episodically at a much faster rate which further powers convection leading to large scale flows. This is an example of a “reactive-convective” hydrodynamic system. In this talk, I will describe the results of our simulations, and the physical picture of convective-reactive flows which may develop during the last burning stages of a star.
| Abstract type | RU or CN Highlight Talk (please discuss with Coordinators before) |
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