The double differential cross sections at lab between 0.0°and 12.3°and the polarization transfer D NN at 0°for the 90 Zr(p,n) reaction are measured at a bombarding energy of 295 MeV. A multipole decomposition technique is applied to the cross sections to extract Lϭ0, Lϭ1, Lϭ2, and Lϭ3 contributions. The Gamow-Teller ͑GT͒ strength B(GT) in the continuum deduced from the Lϭ0 cross section is compared both with the perturbative calculation by Bertsch and Hamamoto and with the second-order random phase approximation calculation by DroSdS et al. The sum of B(GT) values up to 50 MeV excitation becomes S  Ϫϭ28.0Ϯ1.6 after subtracting the contribution of the isovector spin-monopole strength. This S  Ϫ value of 28.0Ϯ1.6 corresponds to about ͑93 Ϯ 5͒% of the minimum value of the sum rule 3(NϪZ)ϭ30. The usefulness of the polarization transfer observable in the distorted wave impulse approximation is presented. ͓S0556-2813͑97͒02006-2͔
The cross section, the deuteron vector A(d)(y) and tensor analyzing powers A(ij), the polarization transfer coefficients K(y('))(ij), and the induced polarization P(y(')) were measured for the dp elastic scattering at 270 MeV. The cross section and A(d)(y) are well reproduced by Faddeev calculations with modern data-equivalent nucleon-nucleon forces plus the Tucson-Melbourne three-nucleon force. In contrast, A(ij), K(y('))(ij), or P(y(')) are not described by such calculations. These facts indicate the deficiencies in the spin dependence of the Tucson-Melbourne force and call for extended three-nucleon force models.
We have detected sub-TeV gamma-ray emission from the direction of the Galactic center (GC) using the CANGAROO-II Imaging Atmospheric Cerenkov Telescope. We detected a statistically significant excess at energies greater than 250 GeV. The flux was 1 order of magnitude lower than that of the Crab Nebula at 1 TeV with a soft spectrum proportional to . The signal centroid is consistent with the GC direction, and the
Ϫ4.65.0עE observed profile is consistent with a pointlike source. Our data suggest that the GeV source 3EG J1746Ϫ2851 is identical to this TeV source, and we study the combined spectra to determine the possible origin of the gammaray emission. We also obtain an upper limit on the cold dark matter density in the Galactic halo.
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