English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

A small number of naturally occurring, proton-rich nuclides (the p-nuclei)cannot be made in the s- and r-process. Their origin is not well understood.Massive stars can produce p-nuclei through photodisintegration of pre-existingintermediate and heavy nuclei. This so-called gamma-process requires highstellar plasma temperatures and occurs mainly in explosive O/Ne burning duringa core-collapse supernova. Although the gamma-process in massive stars has beensuccessful in producing a large range of p-nuclei, significant deficiencesremain. An increasing number of processes and sites has been studied in recentyears in search of viable alternatives replacing or supplementing the massivestar models. A large number of unstable nuclei, however, with onlytheoretically predicted reaction rates are included in the reaction network andthus the nuclear input may also bear considerable uncertainties. The currentstatus of astrophysical models, nuclear input, and observational constraints isreviewed. After an overview of currently discussed models, the focus is on thepossibility to better constrain those models through different means.Meteoritic data not only provide the actual isotopic abundances of the p-nucleibut can also put constraints on the possible contribution of proton-richnucleosynthesis. The main part of the review focusses on the nuclearuncertainties involved in the determination of the astrophysical reaction ratesrequired for the extended reaction networks used in nucleosynthesis studies.Experimental approaches are discussed together with their necessary connectionto theory, which is especially pronounced for reactions with intermediate andheavy nuclei in explosive nuclear burning, even close to stability.

Constraining the astrophysical origin of the p-nuclei through nuclear physics and meteoritic data