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The 14N(p,γ)15O reaction studied at low and high beam energy

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Kurzfassung in Englisch

The CNO cycle consists of a set of nuclear reactions that convert hydrogen into helium and releases energy in stars. The cycle contributes less than 1% to our Sun's luminosity, but it is responsible for detectable neutrino fluxes that can bring direct information of the physical conditions in the solar core, provided that the nuclear reaction rate is known with sufficient precision.
The 14N(p,γ)15O is the slowest reaction in the CNO cycle and estabilishes its rate. The experimental study has been performed both at the LUNA 400 kV accelerator deep underground in the Gran Sasso mountain in Italy and at a 3 MV Tandetron in the Helmholtz-Zentrum Dresden-Rossendorf. A proton beam was sent on solid TiN targets and the prompt photons were collected by a composite HPGe detector (at LUNA) or by up to four HPGe detectors (Dresden).
The obtained results improve the fit of the excitation function in the R-matrix framework, that is used to extrapolate the S-factor at the very low astrophysical energies. In addition, the strength of two resonances at Ep = 430 and 897 keV of the 15N(p,αγ)12C reaction were measured, improving the precision for hydrogen depth profiling.

weitere Metadaten

Kernastrophysik, CNO, solare Neutrino, LUNA, 14N, 15N, HPGe, Tiefenprofilanalyse von Wasserstoff
nuclear astrophysics, CNO, solar neutrinos, LUNA, 14N, 15N, HPGe, hydrogen depth profiling
DDC Klassifikation530
RVK KlassifikationUS 1000, UN 2500
HochschuleTechnische Universität Dresden
FakultätFakultät Mathematik und Naturwissenschaften
BetreuerProf. Dr. Eckart Grosse
Dr. Daniel Bemmerer
GutachterProf. Dr. Eckart Grosse
Dr. Zsölt Fülöp
Tag d. Einreichung (bei der Fakultät)28.01.2011
Tag d. Verteidigung / Kolloquiums / Prüfung01.11.2011
Veröffentlichungsdatum (online)04.06.2012
persistente URNurn:nbn:de:bsz:14-qucosa-87464

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