Download Fundamentals in Nuclear Physics: From Nuclear Structure to by Jean-Louis Basdevant, James Rich, Michael Spiro PDF
By Jean-Louis Basdevant, James Rich, Michael Spiro
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Extra resources for Fundamentals in Nuclear Physics: From Nuclear Structure to Cosmology (Advanced Texts in Physics)
Sample text
The photon spectrum for the decays of the 6 lowest energy states is shown schematically on the lower right. J P = 0+ even − even nuclei (ground state) . 38) where l is the angular momentum quantum number of the unpaired nucleon. The ± is due to the fact that the unpaired spin can be either aligned or anti-aligned with the orbital angular momentum. We will go into more detail in Sect. 4 when we discuss the nuclear shell model. Spins and parities have important phenomenological consequences. They are important in the determination the rates of β-decays (Sect.
In fact the nucleon–nucleon force is attractive in both cases. For s = 1 it is sufficiently attractive to produce a bound state while for s = 0 it is not quite attractive enough. We can understand how this comes about by considering the 3-dimensional square well potential shown in Fig. 10: V (r) = −V0 r < R V (r) = 0 r > R . 43) While it is hardly a realistic representation of the nucleon–nucleon potential, its finite range, R, and its depth V0 can be chosen to correspond more or less to the range and depth of the real potential.
The use of particle exchange to describe potentials obviously has direct applications in bound states and elastic scattering. If one includes the possibility of the exchange of charged particles, we can also describe inelastic reactions, some of which are shown in Fig. 14. 42 GeV . 72) This particle mediates the so-called charged-current weak interactions. They play the essential cosmological role of changing neutrons into protons and vice versa. They thus play an essential role in the cosmological and astrophysical synthesis of heavy elements.