Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apro10015r&link_type=abstract
American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As
Astronomy and Astrophysics
Astrophysics
Scientific paper
Although it seems strange to set T=0 two body matrix elements to zero in a nuclear structure calculation we find that we get results fairly close to what we would obtain using the full interaction for the \underlineexcitation energies of states of lowest isospin in even-even nuclei e.g. T=0 states in ^44Ti and T=1 states in ^50Cr. The realistic T=0 two body interactions are needed only for fine tuning the spectra. It should be noted that in a single j shell calculation the excitation energies are the same if the two body T=0 matrix elements are set to zero or to a constant. This is not true when more than one shell is involved. We thus examine three different such interactions A) T=0 matrix elements set equal to zero B) T=0 matrix elements set to a constant C) Full FPD6 interaction. While the excitation energies are not too sensitive to these changes we find transition strengths are. We find that the summed \underlineorbital B(M1) strength i.e. scissors mode excitations are quite sensitive to the T=0 two body matrix elements. We find the main change to come when going from interaction A to interaction B instead of from B to C. (For example in ^46Ti with 2 particles allowed outside the f_7/2 shell the values for T=1 arrow T=1 transitions went from 0.1850 to 0.6701 to 0.7095 μ_N^2.) Thus it appears that the orbital M1 strength depends on the presence of T=0 two body matrix elements but the main dependence is the presence of an average T=0 interaction and is not sensitive to the fluctuations. We find for Gamow-Teller transitions that the results depend more sensitively on the details (i.e. fluctuations) in the T=0 two body matrix elements.
Robinson Shadow
Zamick Larry
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