Nucleosynthesis in Early Supernova Winds. II. The Role of Neutrinos

By J. Pruet, R. Hoffman, Stan Woosley, Hans-Thomas Janka, R. Buras. 2005

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One of the outstanding unsolved riddles of nuclear astrophysics is the origin of the so-called p-process nuclei from A = 92 to 126. Both the lighter and heavier p-process nuclei are adequately produced in the neon and oxygen shells of ordinary Type II supernovae, but the origin of these intermediate isotopes, especially 92,94Mo and 96,98Ru, has long been mysterious. Here we explore the production of these nuclei in the neutrino-driven wind from a young neutron star. We consider such early times that the wind still contains a proton excess because the rates for νe and positron captures on neutrons are faster than those for the inverse captures on protons. Following a suggestion by Fröhlich and coworkers, we also include the possibility that—in addition to the protons, α-particles, and heavy seed—a small flux of neutrons is maintained by the reaction p(e, e+)n. This flux of neutrons is critical in bridging the long waiting points along the path of the rp-process by (n, p) reactions. Using the unmodified ejecta histories from a recent two-dimensional supernova model by Janka and coworkers, we find synthesis of p-rich nuclei up to 102Pd, although our calculations do not show efficient production of 92Mo. If the entropy of these ejecta is increased by a factor of 2, the synthesis extends to 120Te. Still larger increases in entropy, which might reflect the role of magnetic fields or vibrational energy input neglected in the hydrodynamical model, result in the production of nuclei up to A ≈ 170. Elements synthesized in these more extreme outflows include numerous s- and p-process nuclei, and even some r-process nuclei can be synthesized in these proton-rich conditions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/34c4242339272e830b1c0a92ee8b4ca396410380

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A NEW MULTI-DIMENSIONAL GENERAL RELATIVISTIC NEUTRINO HYDRODYNAMICS CODE FOR CORE-COLLAPSE SUPERNOVAE. II. RELATIVISTIC EXPLOSION MODELS OF CORE-COLLAPSE SUPERNOVAE (2012, background): “Depending on the neutrino luminosities there may also be potential for νp-process nucleosynthesis (Fröhlich et al. 2006a; Pruet et al. 2006).”
NUCLEOSYNTHESIS AND EVOLUTION OF MASSIVE METAL-FREE STARS (2008, unknown): “This probably means the production of the r-process (Woosley et al. 1994), some light p-process nuclei by the rp-process (Pruet et al. 2006; Fröhlich et al. 2006), and the production of significant quantities of rare nuclei lighter than molybdenum (Hoffman et al. 1996; Pruet et al. 2005).”
Europium production: neutron star mergers versus core-collapse supernovae (2013, background): “Proton-rich winds were first found by Liebendoerfer et al. (2003) and discussed in detail also by Froelich et al. c© 2013 RAS (2006a,b) as well as Pruet et al. (2005, 2006).”
The rp-Process in Neutrino-driven Winds (2006, methodology): “The other is the two dimensional simulation of a collapsing 15M⊙ progenitor by Buras et al. (2006), which is also taken in Pruet et al. (2005, 2006).”
Features of the Acoustic Mechanism of Core-Collapse Supernova Explosions (2006, background): “Since Ye was not allowed to exceed 0.5, the potential effects of νe and ν̄e absorption for Yes above 0.5 and/or in enabling the ν-p and rp processes (Frölich et al. 2005ab,2006; Pruet et al. 2005,2006) were not properly incorporated.”
Three-dimensional simulations of neutrino-driven core-collapse supernovae from low-mass single and binary star progenitors (2018, background): “Models with more sophisticated neutrino transport tend to predict predominantly proton-rich outflows with Ye > 0.5 (Pruet et al. 2006; Fröhlich et al. 2006; Müller et al. 2012; Wanajo et al. 2018; Vartanyan et al. 2018), although significant amounts of neutron-rich material can be produced in…”
THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS (2010, background): “…1973) and many more have been discovered since (see Clayton 1968; Wallace & Woosley 1981; Rolfs & Rodney 1988; Woosley et al. 1990; Woosley & Hoffman 1992; Pagel 1997; Wallerstein et al. 1997; Schatz et al. 1998; Iliadis 2007; Boyd 2008; Fröhlich et al. 2006; Pruet et al. 2006 for recent reviews).”
Nucleosynthesis and remnants in massive stars of solar metallicity (2007, background): “These9 include not only the r-process (Woosley et al., 1994), but some important p-process nuclei (Pruet et al., 2006; Fröhlich et al., 2006), and even abundant elements like Zn (Hoffman et al., 1996) and Sc (Pruet et al., 2005).”
A successful 3D core-collapse supernova explosion model (2018, background): “…site of the p- and νp-processes (Pruet et al. 2006; Fröhlich et al. 2006; Wanajo et al. 2011) and might be the context for the production of some of the first peak of the r-process (Hoffman et al. 1996; Pruet et al. 2006; Fröhlich et al. 2006; Wanajo et al. 2011; Frebel 2018; Bliss et al. 2018).”
Three-dimensional neutrino-driven supernovae: neutron star kicks, spins, and asymmetric ejection of nucleosynthesis products (2012, background): “…Ye in the neutrino-heated ejecta, while more sophisticated energy-dependent neutrino transport yields (slightly) proton-rich conditions in the neutrino-processed material expelled during the early explosion (e.g., Pruet et al. 2006; Fröhlich et al. 2006; Fischer et al. 2010; Müller et al. 2012).”
NUCLEOSYNTHESIS IN ELECTRON CAPTURE SUPERNOVAE OF ASYMPTOTIC GIANT BRANCH STARS (2008, background): “3.6. νp-process The νp-process (or neutrino-induced rp-process) is now believed to be a promising nuclear process that synthesizes light p-nuclei up to A ∼ 110 (Fröhlich et al. 2006; Pruet et al. 2006; Wanajo 2006).”
CHARGED-PARTICLE AND NEUTRON-CAPTURE PROCESSES IN THE HIGH-ENTROPY WIND OF CORE-COLLAPSE SUPERNOVAE (2010, background): “While in the early phase of core-collapse supernovae a Ye larger than 0.5 is expected (see, e.g., Fröhlich et al. 2006a, 2006b; Pruet et al. 2006), the late phases are expected to experience Ye < 0.5 and enable the onset of an r-process.”
MAGNETOROTATIONALLY DRIVEN SUPERNOVAE AS THE ORIGIN OF EARLY GALAXY r-PROCESS ELEMENTS? (2012, background): “…et al. 2001; Wanajo 2006; Arcones et al. 2007), and (b) in addition, the innermost ejecta turned out to be proton-rich instead of neutron-rich (Pruet et al. 2006; Fröhlich et al. 2006), a situation which has now also been shown in long-term simulations (Fischer et al. 2010; Hüdepohl et al.…”