The p-process of stellar nucleosynthesis: astrophysics and nuclear physics status

By M. Arnould, S. Goriely. 2003

419 citations recorded by the source corpus.

Subfields: Atomic and Molecular Physics, and Optics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/2a2ff211f069c6d9b36930ff9617ba561cc9992c

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Citations in the corpus

The rp-Process in Neutrino-driven Winds (2006, background): “As soon as the α-process ceases, the proton capture plays an important role for the production of the p-isotope 92Mo as suggested by Hoffman et al. (1996), whose origin has been a long-standing mystery (see Arnould & Goriely 2003, for a recent review).”
The impact of individual nuclear properties on $r$-process nucleosynthesis (2015, methodology): “ton-rich side of stability [3, 4]. Since that time much progress has been made, e.g. [5], and the basic mechanisms of and astrophysical sites for the creation of the s-process [6] and heavy p-process [7, 8] nuclei are on a rm footing. The site or sites of the rprocess still evade denitive determinat”
NUGRID STELLAR DATA SET. I. STELLAR YIELDS FROM H TO BI FOR STARS WITH METALLICITIES Z = 0.02 and Z = 0.01 (2013, background): “One example is the classical p process (also known as the γ process) which forms proton-rich nuclei due to the photo-disintegration of s-process products in deep s-process-rich layers (Arnould & Goriely 2003).”
Origin of the heaviest elements: The rapid neutron-capture process (2019, background): “Aside from the so-called p-process (Arnould and Goriely, 2003; Rauscher et al., 2013; Nishimura et al., 2018) that accounts for the minor heavy element isotopes on the proton-rich side of the val-”
The s process: Nuclear physics, stellar models, and observations (2010, background): “The subset of stable isotopes on the proton-rich side are ascribed to the p process, which is likely to occur also in supernova explosions (Arnould and Goriely, 2003).”
THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS (2010, background): “…theoretical rate calculations based on shell model (Herndl & Brown 1997; Fisker et al. 2001) or Hauser–Feshbach models (Hauser & Feshbach 1952; Holmes et al. 1976; Woosley et al. 1978; Woosley & Hoffman 1992; Rauscher & Thielemann 1998, 2000; Rauscher 2008a; Goriely 1998; Arnould & Goriely 2003).”
Neutron-Capture Elements in the Early Galaxy (2008, methodology): “Detailed discussions of p-nuclei have been given in the reviews of, e.g., Lambert (1992) and Arnould & Goriely (2003) and these isotopes will not be considered further here.”
Origin of the Chemical Elements (2010, background): “The bulk of p-nuclides can be explained in such a model but some problems remain (Rauscher et al. 2002, Arnould and Goriely 2003, Boyd 2008).”