Rubidium, zirconium, and lithium production in intermediate-mass asymptotic giant branch stars

Abstract

Context.A recent survey of a large sample of Galactic intermediate-mass (>3 M ) asymptotic giant branch (AGB) stars shows that they exhibit large overabundances of rubidium (Rb) up to 100-1000 times solar. In contrast, zirconium (Zr) is not enriched in these stars compared to its solar abundances. These observations set constraints on our theoretical notion of the slow neutron capture process (s process) that occurs inside intermediate-mass AGB stars. Lithium (Li) abundances are also reported for these stars. In intermediate-mass AGB stars, Li can be produced by proton captures occuring at the base of the convective envelope. For this reason the observations of Rb, Zr, and Li set complementary constraints on different processes occurring in the same stars. Aims. We present predictions for the abundances of Rb, Zr, and Li as computed for the first time simultaneously in intermediate-mass AGB star models and compare them to the current observational constraints. Methods. We calculate the Rb, Zr, and Li surface abundances for stellar models with masses between 3 and 6.5 M and metallicities between 0.02 and 0.004. Results. We find that the Rb abundance increases with increasing stellar mass, as is inferred from observations but we are unable to match the highest observed [Rb/Fe] abundances. Variations of the reaction rates of the neutron-capture cross sections involved with Rb production and the rate of the 22 Ne(α, n) 25 Mg reaction, responsible for neutron production inside these stars, yield only modest variations in the surface Rb content of ≈0.3 dex. Inclusion of a partial mixing zone (PMZ) to activate the 13 C(α, n) 16 O reaction as an additional neutron source yields significant enhancements in the Rb abundance. However this leads to Zr abundances that exceed the upper limits of the current observational constraints. If the third dredge-up (TDU) efficiency remains as high during the final stages of AGB evolution as during the earlier stages, we can match the lowest values of the observed Rb abundance range. We predict large variations in the Li abundance, which are observed. Finally, the predicted Rb production increases with decreasing metallicity, in qualitative agreement with observations of Magellanic Cloud AGB stars. However stellar models of Z = 0.008 and Z = 0.004 intermediate-mass AGB stars do not produce enough Rb to match the observed abundances.

CHEMISTRY OF THE SAGITTARIUS DWARF GALAXY: A TOP-LIGHT INITIAL MASS FUNCTION, OUTFLOWS, AND THER-PROCESS

“…Recent theoretical calculations by van Raai et al (2012) and Karakas et al (2012) produce Rb enhancements in intermediate-mass AGB stars near ∼1 dex, which is similar to the mean for Galactic Rb-rich stars. They also find larger Rb enhancements at lower metallicity, as observed, but the maximum predicted [Rb/Fe] ratio, thus far, is + 1.44 dex, significantly smaller than the most extreme observations.…”

s-process enrichment in the planetary nebula NGC 3918. Results from deep echelle spectrophotometry

“…Though only a lower limit, the modestly enhanced [Rb/O] value suggests that the reaction 13 C(α, n) 16 O was the neutron source in the AGB progenitor of NGC 3918, and not 22 Ne(α, n) 25 Mg which operates more efficiently in intermediate-mass AGB stars (van Raai et al 2012;Karakas et al 2012). In particular, the high neutron density of the 22 Ne source opens branchings in the sprocess path that lead to large enrichments of Rb relative to other n-capture elements, unlike the 13 C neutron source, which produces lower neutron densities.…”

Partial mixing and the formation of 13C pockets in AGB stars: effects on the s-process elements

“…Such neutron densities drive the activation of branching points on the s-process path, where unstable nuclei with half lives of the order of or larger than a day can capture a neutron instead of decaying, resulting in a branch on the path of neutron captures. However, the 22 Ne neutron source requires temperatures above 300 MK to be efficiently activated, which are only found in stellar models of mass above around 3 M⊙ (Iben & Truran 1978;Abia et al 2001;van Raai et al 2012;Karakas et al 2012). …”