A historical split in the way convection is treated in a stellar ... condition can be written two ways one ... Goldreich-Schubert-Fricke. Solberg Hoiland ...
With help from many, including Andrzej Baran, Staszek Zola, ... Teff=29635 K (29,500 /-500) log g = 5.518 (5.50 /-0.05) Near core He exhaustion (0.74% by mass) ...
NUCLEOSYNTHESIS IN STELLAR EVOLUTION AND EXPLOSIONS: ABUNDANCE YIELDS FOR CHEMICAL EVOLUTION. ... Jaeger et al. (2001): 22Ne(a,n)25Mg. Kunz et al. (2001): 12C(a,g)16O ...
from H to Si and eventually explodes as a core collapse supernova. Mup' MPISN Massive stars ... Mass Loss (determine which stars explode as RSG and which as BSG) ...
Depending on T the different branchings become active. In all cases the result is ... Balance between forward and reverse reactions for increasing number of processes ...
Code developed on the basis of hydrodynamic stellar structure equations for ... Goldreich-Schubert-Fricke instability: oscilatory instability due to temperature ...
10. The Interiors of Stars Goals: 1. Develop the basic equations describing equilibrium conditions applying in stellar interiors. 2. Estimate the physical conditions ...
compact blue giants depending ... Eta Car. 136-155 M. Massey & Hunter (1998) R136a1. Bonanos et al. (2004) ... Eta Car. Calculations suggested that strong ...
B star seismology. W.A. Dziembowski, Warsaw University Obsevatory ... the most important task for B star seismology. B-type pulsators: progenitors of Cepheids, ...