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Giant Resonances (GR) are the broad resonances that occur at excitation energies between 10 and 30 MeV. They correspond to the collective motion of nucleons within the nucleus. The GR modes can be classified according to their multipolarity L, spin S and isospin T quantum numbers. In the microscopic description, the GR modes can be understood as the collective particle-hole excitations characterized by certain values of the angular momentum and parity (Jπ), orbital momentum, spin, and isospin. The Giant Monopole Resonance (GMR) is interesting because its excitation energy is directly related to the incompressibility of the nucleus KA. KA can be used to derive the incompressibility of nuclear matter KNM, but this extrapolation from the data for real nuclei is not straightforward due to contributions from surface, Coulomb and asymmetry effects. Thus, improvements to the extrapolated KNM can be made by measuring the GMR for increasing (N-Z)/A. The incompressibility of nuclear matter is of importance in the nuclear equation of state (EOS) which describes a number of phenomena: collective excitations of nuclei, supernova explosions and radii of neutron stars. In order to study the Isoscalar Giant Monopole Resonance in unstable nuclei, a ΔE-ΔE-E decay detector composed of plastic scintillator arrays has been built and tested. The measurement of the ISGMR in unstable nuclei will be done using inverse kinematics, with a 40 MeV per nucleon beam of the unstable nucleus incident on a 6Li target. Xinfeng Chen studied the viability of this approach, taking data for elastic scattering and inelastic scattering to low-lying states and giant resonances of 240 MeV 6Li ions on 24Mg, 28Si, and 116Sn. Nuclei excited to the GMR region are particle unstable, and will decay by p, α or n decay shortly after excitation. To reconstruct the event it is necessary to measure the energy and angle of the decay particle and of the residual heavy ion. In many lighter nuclei a few nucleons off stability, and in light proton rich nuclei, the neutron threshold is above the region of interest.

Typescript. / Thesis (Ph. D.)--University of Hawaii, 1968. / Bibliography: Leaves 82-86. / ix, 86 leaves illus., tables

Thesis (M.S.)--University of Michigan, 1970.

Thesis (M.S.)--University of Michigan, 1970.

Theses (M.S.)--Marshall University, 2007. / Title from document title page. Includes abstract. Document formatted into pages: contains vi, 66 pages including color illustrations and maps. Includes vitae. Bibliography: p. 58-64.

According to both spectroscopic measurements and interior models, Jupiter, Saturn, Uranus and Neptune possess gaseous envelopes that are enriched in heavy elements compared to the Sun. Straightforward application of the dominant theories of gas giant formation - core accretion and gravitational instability - fail to provide the observed enrichment, suggesting that the surplus heavy elements were somehow dumped onto the planets after the envelopes were already in existence. Previous work has shown that if giant planets rapidly reached their cur rent configuration and radii, they do not accrete the remaining planetesimals efficiently enough to explain their observed heavy-element surplus. We ex plore the likely scenario that the effective accretion cross-sections of the giants were enhanced by the presence of the massive circumplanetary disks out of which their regular satellite systems formed. Perhaps surprisingly, we find that a simple model with protosatellite disks around Jupiter and Saturn can meet known constraints without tuning any parameters. Fur thermore, we show that the heavy-element budgets in Jupiter and Saturn can be matched slightly better if Saturn’s envelope (and disk) are formed roughly 0.1 — 10 Myr after that of Jupiter. We also show that giant planets forming in an initially-compact con figuration can acquire the observed enrichments if they are surrounded by similar protosatellite disks. Protosatellite disks efficiently increase the capture cross-section, and thus the metallicity, of the giant planets. Detailed models of planet formation must therefore account for the presence of such disks during the early stages of solar system formation. / Science, Faculty of / Physics and Astronomy, Department of / Graduate

Thesis (M.S.)--Oregon State University, 2005. / Printout. Includes bibliographical references (leaves 64-72). Also available on the World Wide Web.

Thesis (M.S. in Psych.)--School of Psychology, Georgia Institute of Technology, 2004. Directed by Terry Maple. / Includes bibliographical references (leaves 58-69).

Thesis (Ph.D.)--Murdoch University, 2005. / Thesis submitted to the Division of Health Sciences. CD-ROM contains appendix. Bibliography: leaves 104-120.