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In this paper we examine the effectiveness of reducing the second order radial equation, of the hyperspherical coordinate solution to the two-electron Schrodinger equation, into a set of coupled first order linear equations as suggested by Klar. All results have been obtained in a completely nonadiabatic formalism thereby ensuring accuracy. We arrive at the conclusion that our application of the reduction process is in some way inconsistent and suggest a possible resolution to this anomaly.

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Thesis (Ph. D.)--University of Texas at Austin, 2002. / Vita. Includes bibliographical references. Available also from UMI Company.

Thesis (Ph. D.)--University of Texas at Austin, 1998. / Vita. Includes bibliographical references (leaves 77-80). Available also in a digital version from Dissertation Abstracts.

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Call number: LD2668 .T4 1985 T36 / Master of Science

Ho, Tak Ngai = 中子星在絶熱冷卻下的不穩定性 : 數值模擬和簡單類比 / 何德藝. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2011. / Includes bibliographical references (leaves 101-102). / Abstracts in English and Chinese. / Ho, Tak Ngai = Zhong zi xing zai jue re leng que xia de bu wen ding xing : shu zhi mo ni he jian dan lei bi / He Deyi. / Chapter 1 --- Introduction --- p.1 / Chapter 2 --- The astrophysical problem --- p.2 / Chapter 2.1 --- Neutron stars --- p.2 / Chapter 2.2 --- Equations --- p.4 / Chapter 2.3 --- EOS --- p.6 / Chapter 2.4 --- Equilibrium configurations --- p.8 / Chapter 2.5 --- Stability --- p.9 / Chapter 2.6 --- The key equilibrium properties --- p.10 / Chapter 2.7 --- Adiabatic cooling --- p.11 / Chapter 2.8 --- Modeling adiabatic cooling by varying T --- p.13 / Chapter 3 --- Numerical Simulations in GR --- p.17 / Chapter 3.1 --- Introduction --- p.17 / Chapter 3.2 --- The equations and the EOS --- p.17 / Chapter 3.3 --- Evolution of a stellar system in GR --- p.20 / Chapter 3.4 --- Results --- p.22 / Chapter 4 --- Newtonian model --- p.27 / Chapter 4.1 --- Introduction --- p.27 / Chapter 4.2 --- Newtonian fluid equations --- p.28 / Chapter 4.3 --- Polytropes --- p.28 / Chapter 4.4 --- Model EOS --- p.31 / Chapter 4.5 --- Equilibrium solutions --- p.33 / Chapter 4.6 --- Stability --- p.35 / Chapter 4.7 --- Dynamics --- p.38 / Chapter 4.8 --- Adiabatic changes --- p.42 / Chapter 4.9 --- Results --- p.46 / Chapter 5 --- Model of instability --- p.52 / Chapter 5.1 --- Introduction . --- p.52 / Chapter 5.2 --- Analytical study of the model --- p.54 / Chapter 5.3 --- Numerical verification --- p.55 / Chapter 5.4 --- Summary --- p.59 / Chapter 6 --- Model of criticality --- p.62 / Chapter 6.1 --- Introduction --- p.62 / Chapter 6.2 --- General discussion of equilibrium properties --- p.63 / Chapter 6.3 --- Construction of model --- p.67 / Chapter 6.4 --- Study of the model --- p.75 / Chapter 6.5 --- Conclusion --- p.82 / Chapter 7 --- Conclusion --- p.85 / Appendix --- p.87 / Chapter A --- Neutron stars cooling due to neutrinos emission --- p.87 / Chapter B --- Determining how r change --- p.89 / Chapter C --- Basic equations in the GR context --- p.91 / Chapter C.1 --- ADM formulation of the field equations --- p.91 / Chapter C.2 --- Explicit form of the hyperbolic equation --- p.93 / Chapter D --- One-zone model --- p.95 / Chapter E --- Numerical scheme of getting the EOS --- p.98 / Bibliography --- p.101