Abstract

The drive of low-energy nuclear astrophysics laboratories is to study the reactions of importance to stellar burning processes and elemental production through stellar nucleosynthesis, over the energy range of astrophysical interest. As laboratory measurements approach the stellar burning window, the rapid drop off of cross-sections is a significant barrier and drives the need to lower background interference. The natural background suppression of underground accelerator facilities enables the extension of current experimental data to lower energies. An example of such reactions of interest are those thought to be sources of neutrons for the s-process, the major production mechanism for elements above the iron peak. The reactions 13 C(α,n)16 O and 22 Ne(α,n)25 Mg are the proposed initial focus of the new nuclear astrophysics accelerator laboratory (CASPAR) currently under construction at the Sanford Underground Research Facility, Lead, South Dakota

Highlights

  • A new underground accelerator laboratory for studying low energy nuclear reaction cross sections of relevance for nuclear astrophysics, is currently under construction

  • The drive of low-energy nuclear astrophysics laboratories is to study the reactions of importance to stellar burning processes and elemental production through stellar nucleosynthesis, over the energy range of astrophysical interest

  • The Compact Accelerator System for Performing Astrophysical Research (CASPAR) laboratory is currently aligned towards the measurement of (α,n) reactions of relevance for the production of neutrons in core helium burning of massive Red Giant stars [4] and shell or inter-shell helium burning of low mass AGB stars [5]

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Summary

Introduction

A new underground accelerator laboratory for studying low energy nuclear reaction cross sections of relevance for nuclear astrophysics, is currently under construction. The main focus of this new system, is on the measurements of the stellar neutron sources that dictate the production of heavy elements through the weak and the main s-process in stars This is a long-standing, potentially transformational question of relevance for the understanding of the chemical evolution of our Universe in early stars and later star generations [1]. EPJ Web of Conferences approximately from 100 keV to 800 keV depending on the specific reaction Most significantly, this overlaps with the energy range of the University of Notre Dame, NSL facility (>500 keV) and the LUNA facility (500 keV) and the LUNA facility (

Experimental facility and equipment
Target station
Solid beam stop target
Extended gas target
Detection
Experimental interests
Summary

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