INTEGRATED NUCLEOSYNTHESIS IN NEUTRINO-DRIVEN WINDS

Journal Article · Sun Oct 10 00:00:00 EDT 2010 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/722/1/954· OSTI ID:21464678

Roberts, L F; Woosley, S E ^[1]; Hoffman, R D ^[2]

---

1. Department of Astronomy and Astrophysics, University of California, Santa Cruz, CA 95064 (United States)
2. Computational Nuclear Physics Group, L-414, Lawrence Livermore National Laboratory, Livermore, CA 94550 (United States)

Although they are but a small fraction of the mass ejected in core-collapse supernovae, neutrino-driven winds (NDWs) from nascent proto-neutron stars (PNSs) have the potential to contribute significantly to supernova nucleosynthesis. In previous works, the NDW has been implicated as a possible source of r-process and light p-process isotopes. In this paper, we present time-dependent hydrodynamic calculations of nucleosynthesis in the NDW which include accurate weak interaction physics coupled to a full nuclear reaction network. Using two published models of PNS neutrino luminosities, we predict the contribution of the NDW to the integrated nucleosynthetic yield of the entire supernova. For the neutrino luminosity histories considered, no true r-process occurs in the most basic scenario. The wind driven from an older 1.4 M{sub sun} model for a PNS is moderately neutron-rich at late times however, and produces {sup 87}Rb, {sup 88}Sr, {sup 89}Y, and {sup 90}Zr in near solar proportions relative to oxygen. The wind from a more recently studied 1.27 M{sub sun} PNS is proton-rich throughout its entire evolution and does not contribute significantly to the abundance of any element. It thus seems very unlikely that the simplest model of the NDW can produce the r-process. At most, it contributes to the production of the N = 50 closed shell elements and some light p-nuclei. In doing so, it may have left a distinctive signature on the abundances in metal-poor stars, but the results are sensitive to both uncertain models for the explosion and the masses of the neutron stars involved.

• OSTI ID: 21464678
• Journal Information: Astrophysical Journal, Vol. 722, Issue 1; Other Information: DOI: 10.1088/0004-637X/722/1/954; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ABUNDANCE
COSMIC NEUTRINOS
LUMINOSITY
NEUTRON STARS
NUCLEAR REACTIONS
NUCLEOSYNTHESIS
R PROCESS
RUBIDIUM 87
STRONTIUM 88
SUPERNOVAE
TIME DEPENDENCE
WEAK INTERACTIONS
YTTRIUM 89
ZIRCONIUM 90
ALKALINE EARTH ISOTOPES
BASIC INTERACTIONS
BETA DECAY RADIOISOTOPES
BETA-MINUS DECAY RADIOISOTOPES
BINARY STARS
COSMIC RADIATION
ELEMENTARY PARTICLES
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
EVOLUTION
FERMIONS
INTERACTIONS
INTERMEDIATE MASS NUCLEI
IONIZING RADIATIONS
ISOMERIC TRANSITION ISOTOPES
ISOTOPES
LEPTONS
MASSLESS PARTICLES
MILLISECONDS LIVING RADIOISOTOPES
NEUTRINOS
NUCLEI
ODD-EVEN NUCLEI
OPTICAL PROPERTIES
PHYSICAL PROPERTIES
RADIATIONS
RADIOISOTOPES
RUBIDIUM ISOTOPES
SECONDS LIVING RADIOISOTOPES
STABLE ISOTOPES
STAR EVOLUTION
STARS
STRONTIUM ISOTOPES
SYNTHESIS
VARIABLE STARS
YEARS LIVING RADIOISOTOPES
YTTRIUM ISOTOPES
ZIRCONIUM ISOTOPES