Halo Nuclei

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the nuclear chart for light nuclei d PAN, July 2005
Binding energies of nuclei Stable Light nuclei: need a lot of energy to break it (example 4 He=2p+2n E=20 MeV) neutron dripline: 11 Li E=0.3 MeV proton dripline: 8 B E=0.1 MeV Binding energies ~ 100 times smaller PAN, July 2005 (1 MeV=1.000.000 eV=1.6x10 -13 J)
Page 1 and 2: Halo Nuclei F. M. Nunes PAN, July 2
Page 3: Lifetimes of nuclei Stable Light nu
Page 7 and 8: Halo nuclei: sizes Very large spati
Page 9 and 10: Halo nuclei: simplified spectra 3p+
Page 11 and 12: Structure (example for 8 B) Microsc
Page 13 and 14: Deuteron: the first halo nucleus D=
Page 15 and 16: Halo nuclei and Quantum Mechanics H
Page 17 and 18: Borromean Halo nuclei Some halo nuc
Page 19 and 20: Halo nuclei: what are the present i
Page 21 and 22: Halo nuclei: elastic scattering PAN
Page 29 and 30: Halo nuclei: breakup PAN, July 2005
Page 35 and 36: Halo nuclei: transfer PAN, July 200
Page 41 and 42: Halo nuclei: fusion PAN, July 2005
Page 43 and 44: Halo nuclei: fusion PAN, July 2005
Page 45 and 46: Halo nuclei: what are our tools? Re
Page 47 and 48: The end Questions? PAN, July 2005
Page 49: Dripline nuclei and Astrophysics PA

Halo Nuclei

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