Nucleosynthesis in neutrino-driven, aspherical supernova explosion of a massive star

Journal Article · Fri Oct 28 00:00:00 EDT 2011 · AIP Conference Proceedings

DOI:https://doi.org/10.1063/1.3628410· OSTI ID:21612084

Fujimoto, S ^[1]; Hashimoto, M ^[2]; Ono, M ^[3]; Kotake, K ^[4]; Ohnishi, N ^[5]

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1. Kumamoto National College of Technology, 2659-2 Suya, Goshi 861-1102 (Japan)
2. Department of Physics, School of Sciences, Kyushu University, Fukuoka 810-8560 (Japan)
3. Department of Physics, School of Sciences, Kyushu University (Japan)
4. Division of Theoretical Astronomy, National Astronomical Observatory (Japan)
5. Department of Aerospace Engineering, Tohoku University (Japan)

We examine explosive nucleosynthesis of p-nuclei during a delayed neutrino-driven, aspherical supernova explosion aided by standing accretion shock instability, based on two-dimensional hydrodynamic simulations of the explosion of a 15M{sub {center_dot}} star. We find that p-nuclei are mainly produced through {gamma}-processes, and that the nuclei lighter than {sup 92}Mo are abundantly synthesized in slightly neutron-rich bubbles with electron fractions of Y{sub e}{<=}0.48. {sup 94}Mo, {sup 96}Ru, and {sup 98}Ru, are underproduced compared with the solar system, as in the spherical model.

• OSTI ID: 21612084
• Journal Information: AIP Conference Proceedings, Vol. 1377, Issue 1; Conference: FINUSTAR 3 Conference on frontiers in nuclear structure, astrophysics, and reactions, Rhodes (Greece), 23-27 Aug 2010; Other Information: DOI: 10.1063/1.3628410; (c) 2011 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
• Country of Publication: United States
• Language: English

Related Subjects

73 NUCLEAR PHYSICS AND RADIATION PHYSICS
79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ASTROPHYSICS
COMPUTERIZED SIMULATION
ELECTRONS
HYDRODYNAMICS
MOLYBDENUM 92
MOLYBDENUM 94
NEUTRINOS
NEUTRONS
NUCLEOSYNTHESIS
RUTHENIUM 96
RUTHENIUM 98
SOLAR SYSTEM
SPHERICAL MODEL
STAR EVOLUTION
TWO-DIMENSIONAL CALCULATIONS
BARYONS
ELEMENTARY PARTICLES
EVEN-EVEN NUCLEI
EVOLUTION
FERMIONS
FLUID MECHANICS
HADRONS
INTERMEDIATE MASS NUCLEI
ISOMERIC TRANSITION ISOTOPES
ISOTOPES
LEPTONS
MASSLESS PARTICLES
MATHEMATICAL MODELS
MECHANICS
MOLYBDENUM ISOTOPES
NANOSECONDS LIVING RADIOISOTOPES
NUCLEAR MODELS
NUCLEI
NUCLEONS
PHYSICS
RADIOISOTOPES
RUTHENIUM ISOTOPES
SIMULATION
STABLE ISOTOPES
SYNTHESIS