Ponente
Sr.
Adrià Casanovas
(UPC)
Descripción
About half of the elemental abundances between Fe and Bi are produced by the so-called s (slow) process of neutron capture reactions in AGB stars. Of particular importance are some nuclides produced during the s-process which are radioactive, with half-lives from years to Gy, so its decay process competes with the neutron capture chain: these nuclides are known as branching points. The measurement of the neutron capture cross section of these elements is crucial to determine the local abundance pattern around the branching point, which yields information of the s-process stellar environment, such as temperature, neutron density or pressure. 204Tl (T1/2=2.78 y) is a very interesting branching point. In the recurrent He-flashes of AGB stars, 204Tl can either β-decay to the s-only nuclide 204Pb or capture another neutron, thus producing 205Tl. which in some stellar environments can decay to 205Pb. On the other hand, neutron capture on 204Pb also yields 205Pb (T1/2=1.5×107 y). Therefore, the value of the 204Tl capture cross section is necessary to determine precisely the primordial 205Pb/204Pb abundances ratio, which would allow one to estimate the time span since the last s-process events that contributed to the elemental composition of the Solar System.
In the year 2015, the cross section of the 204Tl(n,γ) reaction was measured for the first time ever employing four C6D6 scintillation detectors in the neutron time-of-flight facility n_TOF at CERN. The sample was a 203Tl oxide pellet enriched to 4% in 204Tl. The 204Tl total mass was 9 mg, with a total activity of 160 MBq.
In this talk several aspects of this capture cross section measurement will be covered, from the experimental methods and the extraction of the cross section and other important capture reaction parameters, to the final application of the results on s-process nucleosynthesis.
Autor primario
Sr.
Adrià Casanovas
(UPC)
