A Self Similar Model for a Core Collapse Supernova Shock Wave


Almog Yalinewich(CITA, Toronto, Canada)

Sepy 14, 2020

Despite their importance for many astrophysical phenomena and decades of research, both observational and computational, core collapse supernovae are not fully understood. When a massive star exhausts the available fuel, the core collapses to form a proto neutron star, releasing a large amount of energy. As a result, a shock wave emerges and, initially, travels outward. This shock wave propagates through the stellar interoir, which collapses under the effect of gravity. In spherically symmetric, one dimensional simulations, the shock stalls and recedes resulting in a failed supernova, while in 2 and 3-D simulations the shock survives and expands, resulting in a successful supernova. The main difference between one and multi dimensional simulations is turbulence, but it is not clear how turbulence helps the shock resist gravity. In this talk I'll describe an extension to the classical Sedov Taylor explosion that includes point source gravity. One of the insights from this model is that there is an energy threshold below which the shock cannot propagate outward, and that this critical energy depends on the structure of the shocked region. I therefore suggest that turbulence helps sustain the shock wave by distributing the material inside the shocked region in a more energy efficient way.

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