Abstract
The 9C breakup was studied during the SAMURAI29R1 experiment through inclusive and exclusive measurements at energies around 160 AMeV for 9C, in order to evaluate the astrophysical S18 factor for the inverse process 8B(p,γ)9C at energies in the region of astrophysical interest. The radiative proton capture on 8B is important in the hot pp chains, in explosive Hydrogen burning (ppIV and rapI), at temperatures between 0.05 < T9 < 1 K, as possible alternative paths across the A = 8 mass gap. Another goal of this experiment was a detailed study of the breakup reaction mechanism. During the experiment the nuclear breakup process was studied using a natural C target with 425 µm thickness and the Coulomb dissociation by using a natural Pb target with 150 µm thickness. The reaction products were tracked simultaneously using a system of position sensitive Si detectors and in total 1024 output channels were read out by using new dual gain preamplifiers (DGP) specially designed for the experiments of the HI-p collaboration. The SAMURAI29R1 experiment was carried out during the SAMURAI 18Oxygen 2018 Spring campaign and it is part of the HI-p collaboration together with another three experiments. Performances of the setup used and first results of the analysis are presented.
Highlights
The main motivation for studying the proton breakup reaction of the 9 C nucleus is the astrophysical impact of its inverse reaction, the radiative proton capture on the 8 B nucleus
The method proposes to measure the inverse reaction of the radiative capture in a field of virtual photons created by the fast projectile moving in the strong Coulomb field of a target [8, 9] with high atomic number
In order to determine the radiative capture reaction cross-section, the Detailed Balance principle [8] will be used and it will be necessary to disentangle the contribution of different multipoles to the reaction cross-section
Summary
The main motivation for studying the proton breakup reaction of the 9 C nucleus is the astrophysical impact of its inverse reaction, the radiative proton capture on the 8 B nucleus. The thermonuclear energies relevant for nuclear astrophysics are below the Coulomb barrier, where the reaction cross-sections are very small. To measure such cross-sections is even more complicated when radioactive nuclides are involved. In order to bypass the experimental difficulties inherent to the direct measurements, different indirect methods were implemented in nuclear astrophysics for measuring the capture cross-sections [2]. Another fact that motivates to study the 9 C breakup is the large spread of the experimental results for the determined astrophysical S-factor, obtained in the previous experiments [3]
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