Simulations of a Supernova Imposter

Details Simulations of a Supernova Imposter Simulations of a Supernova Imposter

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..332...75a&link_type=abstract

The Fate of the Most Massive Stars, ASP Conference Series, Vol. 332, Proceedings of the conference held 23-28 May, 2004 in Grand

Physics

5

Scientific paper

We discuss possible non-supernova eruptions in massive stars like η Carina, using a combination of stellar evolution and radiation hydrodynamics, to ascertain the essential underlying physics of such phenomena. A summary of a combination of numerical hydrodynamical simulations, in one, two, and three dimensions, is used to explore various facets of the problem. We apply insight from multidimensional simulations to both stellar evolution and stellar hydrodynamics in the case of a 120 M&sun; star of solar abundances. We conclude that such stars should rapidly evolve to the redward of the Humphreys-Davidson limit, where they become vigorously unstable to density clumping and mass ejection, and predict CNO abundance differences in the clumpy and unclumped medium.

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