Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a...103..358m&link_type=abstract
Astronomy and Astrophysics, vol. 103, no. 2, Nov. 1981, p. 358-366.
Astronomy and Astrophysics
Astrophysics
50
Gravitational Collapse, Hydrodynamics, Stellar Cores, Stellar Evolution, Stellar Mass, Stellar Models, Stellar Rotation, Isopycnic Processes, Rotating Matter, Stellar Structure, Supernovae
Scientific paper
The collapse of the rotating cores of massive stars (M greater than or equal to 15 solar masses) is considered. The dynamical evolution of the core is followed by an explicit two-dimensional hydrodynamic code. A realistic, finite-temperature equation of state is used in the calculations. Rigidly and differentially rotating initial models are both studied. It is found that in all cases considered the collapse proceeds up to nearly nuclear matter density before it is stopped. In none of the examined models is the core-bounce followed by an explosion. The dynamical behaviour of the slowly rotating models is very similar to that of nonrotating models. The rapidly rotating cores already show large nonspherical effects before core bounce. In these models, a high entropy blob is formed near the axis of rotation, which, while trying to rise and expand, is rapidly destroyed by the onset of circulation. A flattened, nearly hydrostatic central condensation builds up with relatively low central density on which the matter of the envelope is further accreted.
Hillebrandt Wolfgang
Mueller Ewald
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