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Abteilung für gespeicherte und gekühlte Ionen
Max-Planck-GesellschaftMax-Planck-Institut für KernphysikUniversität Heidelberg Abteilung für gespeicherte und gekühlte Ionen
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Tel.: +49 6221 516-851
Fax: +49 6221 516-852
Max-Planck-Institut für Kernphysik
Postfach 10 39 80
69029 Heidelberg
Max-Planck-Institut für Kernphysik
Saupfercheckweg 1
Gebäude: Gentnerlabor, Raum 134
69117 Heidelberg


Sonderseminare 2008

Zeit: Montag, 6. Oktober 2008, 16.00 h c.t.
Ort: Seminarraum Blaum
Redner: Dr. Yoshitaka Fujita, Department of Physics, Osaka University, Japan
Titel: Study of far-stability nuclei by combining mirror Gamow-Teller transitions


Gamow-Teller (GT) transition is one of the most popular nuclear weak processes of spinisospin (στ) type. It is of interest not only in the study of nuclear physics, but also in astrophysics; it plays important roles, for example, in supernova-explosion or nuclear synthesis. Relatively limited information can directly be obtained through the study of weak processes, such as β decay or neutrino induced reactions. However, it was found that (p, n) charge-exchange reactions at intermediate incoming energies (E > 100 MeV) and at 0° could selectively excite GT transitions, that extended the region of excitation energy of the study. With one-order-of-magnitude improvement of the energy resolution in (3He,t) measurements at 140 MeV/nucleon, fine structures of GT excitations, even those of GT giant resonances, can now be studied. Determination of GT transition strengths for pf-shell nuclei with astrophysical interest is discussed [1]. We show that quantum number "isospin" and accurate Q values (masses) of proton-rich nuclei play important roles in such studies.
[1] Y. Fujita et al., Phys. Rev. Lett. 95 (2005) 212501 external link


Zeit: Dienstag, 23. Sept. 2008, 16.00 h c.t.
Ort: Seminarraum Blaum
Redner: Dr. Joseph Formaggio, Massachussetts Institute of Technology, Cambridge/MA, USA
Titel: Twilight: Results from the third final phase of SNO


The Sudbury Neutrino Observatory (SNO) has the ability to measure the total flux of all active flavors of neutrinos using the neutral current reaction, whose signature is a neutron. By comparing the rates of the neutral current reaction to the charged current reaction, which only detects electron neutrinos, one can test the neutrino oscillation hypothesis independent of solar models. This talk will present results from the third and final phase of the SNO experiment.