Experimental Study of the ²²Ne(p,γ)²³Na Reaction and its Implications for Novae Scenarios

The ²²Ne(p,γ)²³Na reaction belongs to the catalytic neon-sodium cycle and has an important role in the explosive hydrogen burning. The neon-sodium cycle takes place at temperatures of T = 0:1 - 0:5GK and is assumed to occur in different astrophysical systems: e.g. in novae, in super novae of type Ia and during the shell-burning of red giant branch stars.

The implications of ²²Ne(p,γ)²³Na and the neon-sodium cycle in a nova scenario have been studied by using the nuclear network code libnucnet at GSI in Darmstadt. A nova is an outburst of matter in a binary system consisting of a white dwarf and a red giant star. It is therefore a representative phenomenon for explosive hydrogen burning. For the calculation of the nucleosynthesis during the nova outburst, the code libnucnet requires the initial mass composition of the novae partners, the temperature and density proles of the nova explosion and the thermonuclear reaction rates of the participating reactions. In the following, the code determined the ow and the nal atomic abundance in the neon-sodium cycle during the entire nova process. Additionally, the in uence of the temperature prole of the novae outburst as well as the thermonuclear reaction rate of the ²²Ne(p,γ)²³Na reaction on the nal atomic abundance in the outburst has been studied.

A characteristic measure for the reactions in astrophysical environments is the thermonuclear reaction rate. The reaction rate of ²²Ne(p,γ)²³Na has still strong uncertainties in the temperature range of T = 0:03-0:3 GK. These uncertainties are based on insucient upper limits of the resonance strengths as well as the possible existence of tentative states that are populated in the energy range of E^lab _p = 30 - 300 keV. The research presented in this thesis is dedicated to the experimental study of the ²²Ne(p,γ)²³Na reaction for an improved determination of the thermonuclear reaction rate. Furthermore, the implications of ²²Ne(p,γ)²³Na and the neon-sodium-cycle in novae scenarios are discussed. The data taking has been performed at the Laboratori Nazionali del Gran Sasso, Italy. This laboratory provides the LUNA facility (Laboratory for Underground Nuclear Astrophysics) for the measurement of small reaction cross sections. The LUNA facility includes a 400 kV ion accelerator, a windowless gas target system and a HPGe-detector. Based on the measurements of the ²²Ne(p,γ)²³Na reaction at LUNA, upper limits for the strengths of ve isolated resonances in the energy range of E^lab _p = 150 - 340 keV have been determined.

For the nuclear resonance at E^lab _res = 186 keV, a positive resonance strength has been measured for the rst time in literature.