TYPE Ia SUPERNOVAE AS SITES OF THE p-PROCESS: TWO-DIMENSIONAL MODELS COUPLED TO NUCLEOSYNTHESIS

Journal Article · Sat Oct 01 00:00:00 EDT 2011 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/739/2/93; COUNTRY OF INPUT: INTERNATIONAL ATOMIC ENERGY AGENCY (IAEA)· OSTI ID:21587464

Travaglio, C; Gallino, R ^[1]; Roepke, F K ^[2]; Hillebrandt, W ^[3]

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1. INAF-Astronomical Observatory Teramo, Via Mentore Maggini snc, Loc. Collurania, 64100 Teramo (Italy)
2. Universitaet Wuerzburg, Am Hubland, D-97074 Wuerzburg (Germany)
3. Max-Planck-Institut fuer Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching bei Muenchen (Germany)

Beyond Fe, there is a class of 35 proton-rich nuclides, between {sup 74}Se and {sup 196}Hg, called p-nuclei. They are bypassed by the s and r neutron capture processes and are typically 10-1000 times less abundant than the s- and/or r-isotopes in the solar system. The bulk of p-isotopes is created in the 'gamma processes' by sequences of photodisintegrations and beta decays in explosive conditions in both core collapse supernovae (SNe II) and in Type Ia supernovae (SNe Ia). SNe II contribute to the production of p-nuclei through explosive neon and oxygen burning. However, the major problem in SN II ejecta is a general underproduction of the light p-nuclei for A < 120. We explore SNe Ia as p-process sites in the framework of a two-dimensional SN Ia delayed detonation model as well as pure deflagration models. The white dwarf precursor is assumed to have reached the Chandrasekhar mass in a binary system by mass accretion from a giant/main-sequence companion. We use enhanced s-seed distributions, with seeds directly obtained from a sequence of thermal pulse instabilities both in the asymptotic giant branch phase and in the accreted material. We apply the tracer-particle method to reconstruct the nucleosynthesis by the thermal histories of Lagrangian particles, passively advected in the hydrodynamic calculations. For each particle, we follow the explosive nucleosynthesis with a detailed nuclear reaction network for all isotopes up to {sup 209}Bi. We select tracers within the typical temperature range for p-process production, (1.5-3.7) x 10{sup 9} K, and analyze in detail their behavior, exploring the influence of different s-process distributions on the p-process nucleosynthesis. In addition, we discuss the sensitivity of p-process production to parameters of the explosion mechanism, taking into account the consequences on Fe and alpha elements. We find that SNe Ia can produce a large amount of p-nuclei, both the light p-nuclei below A = 120 and the heavy-p nuclei, at quite flat average production factors, tightly related to the s-process seed distribution. For the first time, we find a stellar source able to produce both light and heavy p-nuclei almost at the same level as {sup 56}Fe, including the debated neutron magic {sup 92,} {sup 94}Mo and {sup 96,} {sup 98}Ru. We also find that there is an important contribution from the p-process nucleosynthesis to the s-only nuclei {sup 80}Kr, {sup 86}Sr, to the neutron magic {sup 90}Zr, and to the neutron-rich {sup 96}Zr. Finally, we investigate the metallicity effect on p-process production in our models. Starting with different s-process seed distributions for two metallicities Z = 0.02 and Z = 0.001, running two-dimensional SN Ia models with different initial composition, we estimate that SNe Ia can contribute to at least 50% of the solar p-process composition. A more detailed analysis of the role of SNe Ia in Galactic chemical evolution of p-nuclei is in preparation.

• OSTI ID: 21587464
• Journal Information: Astrophysical Journal, Vol. 739, Issue 2; Other Information: DOI: 10.1088/0004-637X/739/2/93; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

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73 NUCLEAR PHYSICS AND RADIATION PHYSICS
BISMUTH 209
HYDRODYNAMICS
IRON 56
KRYPTON 80
MERCURY 196
MOLYBDENUM 94
MOLYBDENUM 96
NEUTRON REACTIONS
NUCLEOSYNTHESIS
PHOTONUCLEAR REACTIONS
RUTHENIUM 98
S PROCESS
SELENIUM 74
STRONTIUM 86
SUPERNOVAE
TWO-DIMENSIONAL CALCULATIONS
ZIRCONIUM 90
ZIRCONIUM 96
ALKALINE EARTH ISOTOPES
BARYON REACTIONS
BINARY STARS
BISMUTH ISOTOPES
ERUPTIVE VARIABLE STARS
EVEN-EVEN NUCLEI
EVOLUTION
FLUID MECHANICS
HADRON REACTIONS
HEAVY NUCLEI
INTERMEDIATE MASS NUCLEI
IRON ISOTOPES
ISOMERIC TRANSITION ISOTOPES
ISOTOPES
KRYPTON ISOTOPES
MECHANICS
MERCURY ISOTOPES
MILLISECONDS LIVING RADIOISOTOPES
MOLYBDENUM ISOTOPES
NANOSECONDS LIVING RADIOISOTOPES
NUCLEAR REACTIONS
NUCLEI
NUCLEON REACTIONS
ODD-EVEN NUCLEI
RADIOISOTOPES
RUTHENIUM ISOTOPES
SELENIUM ISOTOPES
STABLE ISOTOPES
STAR EVOLUTION
STARS
STRONTIUM ISOTOPES
SYNTHESIS
VARIABLE STARS
ZIRCONIUM ISOTOPES