Heavy Elements in Stars

  title={Heavy Elements in Stars},
  author={Arnold I. Boothroyd},
  pages={1690 - 1691}
Abundances of elements produced in stars four to eight times the mass of the Sun indicate a different dominant nuclear reaction mechanism than in lower-mass stars. 
Origin of the Chemical Elements
This review provides the necessary background from astrophysics, nuclear, and particle physics to understand the cosmic origin of the chemical elements. It reflects the year 2009 state of the art in
Challenges in nucleosynthesis of trans-iron elements
Nucleosynthesis beyond Fe poses additional challenges not encountered when studying astrophysical processes involving light nuclei. Astrophysical sites and conditions are not well known for some of
Photodisintegration studies ofastrophysically relevant p-nuclei
The majority of the light elements up to iron (Fe) are formed by successive rounds of thermonuclear fusion burning in the stellar interiors. The nuclei heavier than iron (Z>26) are being synthesized
Alpha-induced reaction cross section measurements on $^{151}$Eu for the astrophysical $\gamma$-process
In order to extend the experimental database relevant for the astrophysical -process towards the unexplored heavier mass region, the cross sections of the 151 Eu(�,) 155 Tb and 151 Eu(�,n) 154 Tb


Nucleosynthesis in asymptotic giant branch stars: Relevance for galactic enrichment and solar system formation
▪ Abstract We present a review of nucleosynthesis in AGB stars outlining the development of theoretical models and their relationship to observations. We focus on the new high resolution codes with...
Rubidium-Rich Asymptotic Giant Branch Stars
A long-debated issue concerning the nucleosynthesis of neutron-rich elements in asymptotic giant branch (AGB) stars is the identification of the neutron source. We report intermediate-mass (4 to 8
The 85Kr s-Process Branching and the Mass of Carbon Stars
We present new spectroscopic observations for a sample of C(N)-type red giants. These objects belong to the class of asymptotic giant branch stars, experiencing thermal instabilities in the
Nucleosynthesis and Mixing on the Asymptotic Giant Branch. III. Predicted and Observed s-Process Abundances
We present the results of s-process nucleosynthesis calculations for asymptotic giant branch (AGB) stars of different metallicities and different initial stellar masses (1.5 and 3 M☉), and we present
Evolution of Asymptotic Giant Branch Stars
▪ Abstract The current status of modeling the evolution and nucleosynthesis of asymptotic giant branch (AGB) stars is reviewed. The principles of AGB evolution have been investigated in recent years