A Look Inside the Sun’s Fire

New Measurements Point at Slower Burn-In Phase of Hydrogen Burning.

Nuclear astrophysics studies the evolution of the elements in the universe since its creation. The astrophysical models rely on parameters that scientists deduce from laboratory measurements. Nuclear reactions play a crucial role inside of stars. A team from the Helmholtz-Zentrum Dresden-Rossendorf (HZDR), together with researchers from Italy, Hungary and Scotland, has now reinvestigated one of the central reactions at the Dresden Felsenkeller accelerator – with a surprising result, as reported in the journal Physical Review C (DOI: 10.1103/PhysRevC.107.L062801).

„We studied a long-known nuclear reaction, which is important for the creation of the elements in massive stars. It is also one of the earliest reactions to be studied at an ion accelerator laboratory: the collision of a carbon-12 nucleus with a hydrogen nucleus, which creates the isotope nitrogen-13 and gamma-radiation. The reaction is the first step in the so-called CNO cycle. We were interested in the reaction cross section, which tells us about the probability for this reaction to occur,“ says Prof. Daniel Bemmerer of the HZDR-Institute of Radiation Physics.

This parameter has been determined by a team of Italian, Hungarian, Scottish and German scientists at the Felsenkeller with unparalleled precision. The surprising result: the previously accepted value has to be corrected down by about 25 percent. The result suggests that the burn-in phase of the CNO cycle took longer, and that the emission of 13N neutrinos occurs closer to the center of the Sun than previously assumed. The new data also allows more precise theoretical predictions for the ratio of carbon isotopes 12C/13C in stars, which in turn help to benchmark and improve models for processes in the interior of stars.

A Miniature Sun in the Laboratory

Stars obtain their energy from the fusion of hydrogen to helium. Depending on the mass of the stellar object, different ways for this process to occur are known. In low-mass stars, such as our Sun, the so-called proton-proton chain is the dominant process. In more massive stars, much higher temperatures are reached inside, due to the gravitational pressure. This allows also for the reaction between hydrogen and carbon nuclei. Although less than two percent of the interstellar matter that forms stars is made of carbon, this concentration is sufficient to start and sustain the CNO cycle. The carbon acts as a catalyst that accelerates the reaction but does not get consumed in the process. The net reaction is the same as for the proton-proton chain: the fusion of hydrogen to helium. However, in massive stars this reaction proceeds much faster through the CNO cycle.

„We use tantalum discs with carbon evaporated on the surface as targets. They are hit by protons from our 5 MV Pelletron accelerator, which can cover a fairly large energy range. The gamma-rays which are created in the reaction can be detected with 20 high-purity germanium detectors,“ Bemmerer describes the experimental approach.

The Felsenkeller Underground Laboratory in the Plauenscher Grund near Dresden is jointly operated by HZDR and TU Dresden. Located in a tunnel formerly used to store ice for the Dresden Felsenkeller brewery, it is well-suited for such measurements, as a 45 meter thick layer of rock protects the detectors from cosmic radiation. Otherwise, this radiation could interfere with the sensitive measurements. The current work is also a good example for European collaboration in the astrophysics community: A PhD student from the University of Padua conducted research at the Felsenkeller for six months during the experiment. The participation of other measurement guests from Italy, Hungary and Scotland was financially supported by the EU as part of the “ChETEC-INFRA” project.

Wissenschaftliche Ansprechpartner:

Prof. Daniel Bemmerer I Institute of Radiation Physics
Phone: +49 351 260 3901 | Mobil: +49 179 4753139 I Email: d.bemmerer@hzdr.de

Dr. Axel Boeltzig I Institute of Radiation Physics
Phone: +49 351 260 3914 | Email: a.boeltzig@hzdr.de

Originalpublikation:

J. Skowronski, E. Masha, D. Piatti, M. Aliotta, H. Babu, D. Bemmerer, A. Boeltzig, R. Depalo, A. Caciolli, F. Cavanna, L. Csedreki, Z. Fülöp, G. Imbriani, D. Rapagnani, S. Rümmler, K. Schmidt, R. S. Sidhu, T. Szücs, S. Turkat, A. Yadav, Improved S factor of the 12C(p,γ)13N reaction at E=320–620 keV and the 422 keV resonance, Physical Review C 107, (2023), (DOI: 10.1103/PhysRevC.107.L062801)

https://www.hzdr.de/db/Cms?pOid=70512&pNid=99