Published November 12, 2012
| Version v1
Journal article
Physical conditions for the r-process
- 1. Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, C.P. 226, B-1050 Brussels (Belgium)
- 2. Senior High School of Waseda University, Nerima, Tokyo 177-0044 (Japan)
- 3. Technische Universität München, Excellence Cluster Universe, Boltzmannstr. 2, D-85748 Garching and Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching (Germany)
Description
Recent works show that the r-process can proceed by competition between neutron capture and β-decay in low temperature environments (< 5 × 108 K; cold r-process) where photo-disintegration plays no role. This is in contrast to the traditional picture of the r-process in high temperature environments (∼ 1 × 109 K; hot r-process) where the (n, γ)-(γ, n) equilibrium holds. In this study, we explore nucleosynthesis calculations based on a site-independent model to elucidate the physical conditions leading to cold and hot r-processes.
Additional details
Identifiers
- DOI
- 10.1063/1.4763398;
Publishing Information
- Journal Title
- AIP Conference Proceedings
- Journal Volume
- 1484
- Journal Issue
- 1
- Journal Page Range
- p. 217-224
- ISSN
- 0094-243X
- CODEN
- APCPCS
Conference
- Title
- Conference on origin of matter and evolution of galaxies 2011
- Dates
- 14-17 Nov 2011
- Place
- Wako (Japan)
INIS
- Country of Publication
- United States
- Country of Input or Organization
- International Atomic Energy Agency (IAEA)
- INIS RN
- 44034833
- Subject category
- S73: NUCLEAR PHYSICS AND RADIATION PHYSICS; S79: ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;
- Resource subtype / Literary indicator
- Conference
- Descriptors DEI
- ASTROPHYSICS; BETA DECAY; CAPTURE; EQUILIBRIUM; GAMMA RADIATION; NEUTRON REACTIONS; NUCLEOSYNTHESIS; PHOTONUCLEAR REACTIONS; R PROCESS
- Descriptors DEC
- BARYON REACTIONS; DECAY; ELECTROMAGNETIC RADIATION; EVOLUTION; HADRON REACTIONS; IONIZING RADIATIONS; NUCLEAR DECAY; NUCLEAR REACTIONS; NUCLEON REACTIONS; PHYSICS; RADIATIONS; STAR EVOLUTION; SYNTHESIS
Optional Information
- Notes
- (c) 2012 American Institute of Physics