TY - GEN
T1 - Element synthesis in stars
AU - Thielemann, Friedrich-Karl
AU - Brachwitz, F.
AU - Freiburghaus, C.
AU - Kolbe, E.
AU - Martinez-Pinedo, Gabriel
AU - Rauscher, T.
AU - Rembges, F.
AU - Hix, W. R.
AU - Liebendoerfer, M.
AU - Mezzacappa, A.
AU - Kratz, K.L.
AU - Pfeiffer, B.
AU - Langanke, K.
AU - Nomoto, K.
AU - Rosswog, S.
AU - Schatz, H.
AU - Wiescher, Michael
PY - 2001
Y1 - 2001
N2 - Except for H-1, H-2, He-3, He-4, and Li-7, originating from the Big Bang, all heavier elements are made in stellar evolution and stellar explosions. Nuclear physics, and in many cases nuclear structure far from stability, enters in a crucial way. Therefore, we examine in this review the role of nuclear physics in astrophysics in general and in particular how it affects stellar events and the resulting nucleosynthesis. Stellar modeling addresses four major aspects: 1. energy generation and nucleosynthesis, 2. energy transport via conduction, radiation or possibly convection, 3. hydrodynamics/hydrostatics, and finally 4. thermodynamic properties of the matter involved. Nuclear Physics enters via nuclear reaction cross sections and nuclear structure (affecting the composition changes and nuclear energy generation), neutrino-nucleon and neutrino-nucleus cross sections (affecting neutrino opacities and transport), and e.g. the equation of state at and beyond nuclear densities which creates a relation between the nuclear many body problem and and hydrodynamic response like pressure and entropy. In the following we review these four topics by highlighting the role and impact of nuclear physics in each of these aspects of stellar modeling. The main emphasis is put on the connection to element synthesis.
AB - Except for H-1, H-2, He-3, He-4, and Li-7, originating from the Big Bang, all heavier elements are made in stellar evolution and stellar explosions. Nuclear physics, and in many cases nuclear structure far from stability, enters in a crucial way. Therefore, we examine in this review the role of nuclear physics in astrophysics in general and in particular how it affects stellar events and the resulting nucleosynthesis. Stellar modeling addresses four major aspects: 1. energy generation and nucleosynthesis, 2. energy transport via conduction, radiation or possibly convection, 3. hydrodynamics/hydrostatics, and finally 4. thermodynamic properties of the matter involved. Nuclear Physics enters via nuclear reaction cross sections and nuclear structure (affecting the composition changes and nuclear energy generation), neutrino-nucleon and neutrino-nucleus cross sections (affecting neutrino opacities and transport), and e.g. the equation of state at and beyond nuclear densities which creates a relation between the nuclear many body problem and and hydrodynamic response like pressure and entropy. In the following we review these four topics by highlighting the role and impact of nuclear physics in each of these aspects of stellar modeling. The main emphasis is put on the connection to element synthesis.
KW - R-PROCESS NUCLEOSYNTHESIS
KW - IA SUPERNOVAE
KW - X-RAY-BURSTS
KW - CARBON DEFLAGRATION SUPERNOVAE
KW - II SUPERNOVAE
KW - METAL-POOR STARS
KW - NEUTRINO-DRIVEN WINDS
KW - CORE-COLLAPSE SUPERNOVAE
KW - REACTION-RATES
KW - ELECTRON-CAPTURE
U2 - 10.1016/S0146-6410(01)00103-X
DO - 10.1016/S0146-6410(01)00103-X
M3 - Conference contribution
T3 - Progress in Particle and Nuclear Physics
SP - 5
EP - 22
BT - Radioactive Beams in Nuclear Physics
A2 - Faessler, A.
PB - Elsevier
CY - Amsterdam
T2 - International School of Nuclear Physics on Radioactive Beams in Nuclear and Astrophysics
Y2 - 16 September 2000 through 24 September 2000
ER -