NUCLEOSYNTHESIS IN CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK-HADRON PHASE TRANSITION

Journal Article · Wed Oct 10 00:00:00 EDT 2012 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/758/1/9· OSTI ID:22092126

Nishimura, Nobuya; Thielemann, Friedrich-Karl; Hempel, Matthias; Kaeppeli, Roger; Rauscher, Thomas; Winteler, Christian ^[1]; Fischer, Tobias; Martinez-Pinedo, Gabriel ^[2]; Froehlich, Carla ^[3]; Sagert, Irina ^[4]

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1. Department of Physics, University of Basel, CH-4056 Basel (Switzerland)
2. GSI, Helmholtzzentrum fuer Schwerionenforschung GmbH, D-64291 Darmstadt (Germany)
3. Department of Physics, North Carolina State University, NC 27695 (United States)
4. Department of Physics and Astronomy, Michigan State University, MI 48824 (United States)

We explore heavy-element nucleosynthesis in the explosion of massive stars that are triggered by a quark-hadron phase transition during the early post-bounce phase of core-collapse supernovae. The present study is based on general-relativistic radiation hydrodynamics simulations with three-flavor Boltzmann neutrino transport in spherical symmetry, which utilize a quark-hadron hybrid equation of state based on the MIT bag model for strange quark matter. The quark-hadron phase transition inside the stellar core forms a shock wave propagating toward the surface of the proto-neutron star. This shock wave results in an explosion and ejects neutron-rich matter from the outer accreted layers of the proto-neutron star. Later, during the cooling phase, the proto-neutron star develops a proton-rich neutrino-driven wind. We present a detailed analysis of the nucleosynthesis outcome in both neutron-rich and proton-rich ejecta and compare our integrated nucleosynthesis with observations of the solar system and metal-poor stars. For our standard scenario, we find that a 'weak' r-process occurs and elements up to the second peak (A {approx} 130) are successfully synthesized. Furthermore, uncertainties in the explosion dynamics could barely allow us to obtain the strong r-process which produces heavier isotopes, including the third peak (A {approx} 195) and actinide elements.

• OSTI ID: 22092126
• Journal Information: Astrophysical Journal, Vol. 758, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTROPHYSICS
BAG MODEL
COMPARATIVE EVALUATIONS
COSMOLOGY
ELEMENT ABUNDANCE
EQUATIONS OF STATE
FLAVOR MODEL
HYDRODYNAMICS
NEUTRINOS
NEUTRON STARS
NEUTRONS
NUCLEOSYNTHESIS
PHASE TRANSFORMATIONS
PROTONS
PROTOSTARS
QUARK MATTER
R PROCESS
RELATIVISTIC RANGE
S QUARKS
SUPERNOVAE