The internal stellar evolution of massive stars from from hydrogen
burning till core collapse is shown using "Kippenhahn" diagrams.
We show the stellar evolution as a function of stellar mass and
also demonstrate the influence of one key nuclear reaction rate,
C12(a,g).
Michael Kuhlen's Movies and Images
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The code (written by Prof. Gary Glatzmeier, Earth &
Marine Sciences UCSC) is 3D, fully spectral, and employs the anelastic
hydrodynamic approximation. I have been using it to model convection in various
astrophysical circumstances:
Core Convection during Carbon burning in a Carbon White Dwarf - pre-SNIa
Follow these links for various snapshots and some movies of these simulations.
Tami Rogers' Movies
Convection_Ra9.mpg
(6.5 MB)This is a movie of the entropy in 2d convection with
periodic side boundaries and isentropic top and bottom
boundaries. The Rayleigh number in this calculation is 1.d9 and
the prandtl number is 0.1, clearly in the turbulent regime. As
expected in 2d the small scale structure cascades to the large
scale "roll".
Convection_Ra10.mpg
(Warning 32 MB)This is a movie of the entropy in 2d
convection with periodic side boundaris and isentropic top and bottom
boundaries. The Rayleigh number in this calculation is 1.d10 and the
prandtl number is 0.1, clearly in the turbulent regime. In this
calculation the small scale structure cascades to the large scale
"roll" as expected in 2d.
Core Convection in a 15 Solar Mass Main Sequence Star
Oxygen Shell Convection in a 25 Solar Mass Star