Some aspects of the physics of SNeII are discussed in a colloquium talk
by Ewald Müller
containing many color diagrams.
(part1, 0.5MB;
part2, 1.3MB;
part3, 2.2MB;
part4, 0.4MB;
all gzip'd postscript)
The role of neutrino heating and convective processes in the explosion mechanism of Type-II supernovae is investigated by one-, two- and three-dimensional hydrodynamical simulations of the long-time evolution of the collapsed stellar core after the bounce at nuclear matter density and after the associated formation of the supernova shock.
Our results are described in a letter (gzip'd postscript, 83kB) published in the Astrophysical Journal, 448 (1995), L109 and in a detailed paper (gzip'd postscript, 620kB) published in Astronomy & Astrophysics, 306 (1996), 167.
All colour figures of the A&A paper are listed below and can be viewed by clicking at the respective figure number.
Fig.7 (146 kB), Fig.10 (145 kB), Fig.11 (200 kB), Fig.12 (184 kB), Fig.15 (174 kB), Fig.16 (156 kB), Fig.17 (123 kB), Fig.19 (165 kB), Fig.20 (219 kB)
Convection Inside a Protoneutron Star
The left image shows the time evolution (159 kB) of the electron number fraction Y_e in a region between 15km and 155km. The panels are arranged in counter clockwise order, starting from the upper right panel, and show snapshots at 12ms, 14ms, 18ms and 21ms after the start of the 2D simulation. The colour levels correspond to Y_e values in the range [0.1, 0.5] increasing from blue, over green, yellow and orange to red.
The two images on the right show the surface Y_e = 0.160 at 13ms and 14ms obtained in a 3D simulation performed in a wedge of opening angle 60 degrees.
Ewald Müller / ewald _at_ mpa-garching.mpg.de /
12. June 2007
