Abstract
The residual amount of light elements lithium, beryllium and boron (LiBeB) abundances in stellar atmospheres has been largely accepted as one of the most powerful probes for understanding stellar structure and mixing phenomena. They are in fact gradually destroyed at different depths of stellar interior mainly by (p,α), thus their fate in stars is an incomparable tool for studying mixing processes. In order to avoid extrapolation procedures on the available direct S(E)-factor measurements, the Trojan Horse Method (THM) has been developed, allowing one to measure the bare nucleus S(E)-factor for astrophysically relevant reactions without experiencing Coulomb penetrability effects. Here, a summary on the recent 6,7Li and 11B TH investigations will be given and the corresponding results discussed.
Highlights
Stellar structure and mixing mechanisms for low-mass Main-Sequence stars have been a matter of study for a long time, with particular regard to the understanding of surface abundances
Standard Stellar Models do not take into account the possibility of “communication” between the convective zone and the nuclear destruction zone where the burning of such elements occurs mainly via (p,α) reactions induced at temperatures of about T6∼10
The energy region of interest for astrophysics is usually explored by means of extrapolation procedures on the bare-nucleus S(E)b-factor because it smoothly varies with the energy, removing the exponential drop of the cross section ([4])
Summary
Stellar structure and mixing mechanisms for low-mass Main-Sequence stars have been a matter of study for a long time, with particular regard to the understanding of surface abundances. Standard Stellar Models do not take into account the possibility of “communication” between the convective zone and the nuclear destruction zone where the burning of such elements occurs mainly via (p,α) reactions induced at temperatures of about T6∼10.
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