Presolar grain isotopic ratios as constraints to nuclear and stellar parameters of AGB nucleosynthesis

TL;DR

This paper uses isotopic ratios in presolar grains to refine models of AGB star nucleosynthesis, highlighting the importance of magnetic flux tubes, primary isotope production, and nuclear physics uncertainties.

Contribution

It introduces a new AGB nucleosynthesis model incorporating magnetic flux-tube buoyancy and compares it with presolar grain data to constrain nuclear reaction rates.

Findings

Models reproduce presolar SiC grain isotopic ratios with unprecedented accuracy.

Magnetic flux tubes influence the formation of C-rich subcomponents in AGB winds.

Constraints suggest the need for new measurements of weak interaction rates and neutron-capture cross sections.

Abstract

Recent models for evolved Low Mass Stars (with $M \lesssim 3M_\odot$), undergoing the AGB phase assume that magnetic flux-tube buoyancy drives the formation of $^{13}$C reservoirs in He-rich layers. We illustrate their crucial properties, showing how the low abundance of $^{13}$C generated below the convective envelope hampers the formation of primary $^{14}$N and the ensuing synthesis of intermediate-mass nuclei, like $^{19}$F and $^{22}$Ne. In the mentioned models, their production is therefore of a purely secondary nature. Shortage of primary $^{22}$Ne has also important effects in reducing the neutron density. Another property concerns AGB winds, which are likely to preserve C-rich subcomponents, isolated by magnetic tension, even when the envelope composition is O-rich. Conditions for the formation of C-rich compounds are therefore found in stages earlier than previously envisaged. These issues, together with the uncertainties related to several nuclear physics quantities, are discussed in the light of the isotopic admixtures of s-process elements in presolar SiC grains of stellar origin, which provide important and precise constraints to the otherwise uncertain parameters. By comparing nucleosynthesis results with measured SiC data, it is argued that such a detailed series of constraints indicates the need for new measurements of weak interaction rates in ionized plasmas, as well as of neutron-capture cross sections, especially near the N = 50 and N = 82 neutron magic numbers. Nontheless, the peculiarity of our models allows us to achieve fits to the presolar grain data of a quality so far never obtained in previously published attempts.