by Yip Ching Wa. / Thesis (M.Phil.)--Chinese University of Hong Kong, 1998. / Includes bibliographical references (leaves 142-147). / Text in English; abstract also in Chinese. / by Yip Ching Wa. / Acknowledgement --- p.i / Contents --- p.ii / List of Figures --- p.vii / List of Tables --- p.xi / Abstract --- p.xiii / Chapter Chapter 1. --- Introduction to stellar oscillations --- p.1 / Chapter 1.1 --- Motivations of study --- p.1 / Chapter 1.2 --- Historical background of stellar oscillation --- p.2 / Chapter 1.3 --- Compact stars --- p.4 / Chapter 1.4 --- The observational aspects --- p.5 / Chapter 1.5 --- Outline of the thesis --- p.6 / Chapter Chapter 2. --- Static Stars --- p.8 / Chapter 2.1 --- Newtonian stars --- p.8 / Chapter 2.2 --- Relativistic stars --- p.10 / Chapter Chapter 3. --- Mode classifications --- p.14 / Chapter 3.1 --- Newtonian vs relativistic oscillations --- p.14 / Chapter 3.2 --- Radial oscillations --- p.15 / Chapter 3.3 --- Nonradial oscillations --- p.16 / Chapter 3.3.1 --- Spheroidal mode --- p.17 / Chapter 3.3.1.1 --- f-mode (yundamental mode) --- p.17 / Chapter 3.3.1.2 --- p-mode (pressure mode) --- p.18 / Chapter 3.3.1.3 --- g-mode (gravity mode) --- p.18 / Chapter 3.3.1.4 --- w-mode (gravitational-wave mode) --- p.19 / Chapter 3.3.2 --- Toroidal mode --- p.20 / Chapter 3.3.2.1 --- t-mode : (torsional mode) --- p.21 / Chapter 3.3.3 --- Characteristic frequencies of local vibrations --- p.22 / Chapter 3.3.4 --- Stability --- p.23 / Chapter 3.3.4.1 --- Dynamical stability --- p.24 / Chapter 3.3.4.2 --- Secular stability --- p.24 / Chapter 3.3.4.3 --- Pulsational stability --- p.24 / Chapter 3.4 --- Summary --- p.24 / Chapter Chapter 4. --- Adiabatic radial oscillations of stars --- p.26 / Chapter 4.0.1 --- Newtonian case --- p.26 / Chapter 4.0.2 --- Relativistic case --- p.29 / Chapter 4.1 --- Results --- p.30 / Chapter 4.2 --- The stability criteria --- p.31 / Chapter 4.3 --- Summary --- p.39 / Chapter Chapter 5. --- Quasinormal modes of stars --- p.40 / Chapter 5.1 --- Introduction --- p.40 / Chapter 5.2 --- The Scattering Method --- p.42 / Chapter 5.3 --- WKB approximation --- p.43 / Chapter 5.4 --- Chandrasekhar and Detweiler's series --- p.44 / Chapter 5.4.1 --- Application of the series --- p.45 / Chapter 5.5 --- Leaver's series --- p.46 / Chapter 5.5.1 --- Application of the series --- p.48 / Chapter 5.6 --- Summary --- p.52 / Chapter Chapter 6. --- Relativistic nonradial oscillations --- p.53 / Chapter 6.1 --- Axial perturbation --- p.55 / Chapter 6.1.1 --- Perturbation equations --- p.55 / Chapter 6.1.2 --- Boundary conditions --- p.58 / Chapter 6.2 --- Polar perturbations --- p.58 / Chapter 6.2.1 --- Perturbation equations for r≤R --- p.58 / Chapter 6.2.2 --- Boundary condition at r→ 0 --- p.60 / Chapter 6.2.3 --- Perturbation equation for r ≥R --- p.63 / Chapter 6.2.4 --- Boundary condition at r→ ∞ --- p.64 / Chapter 6.3 --- Numerical integration of the perturbation equations --- p.64 / Chapter 6.4 --- The stability problem --- p.66 / Chapter 6.5 --- Summary --- p.66 / Chapter Chapter 7. --- Oscillations of simple model stars --- p.67 / Chapter 7.1 --- Motivations of study --- p.67 / Chapter 7.2 --- Equation of states --- p.68 / Chapter 7.2.1 --- Homogeneous stars --- p.68 / Chapter 7.2.2 --- Relativistic polytropic stars --- p.69 / Chapter 7.3 --- Static stars --- p.69 / Chapter 7.4 --- Oscillation spectra --- p.71 / Chapter 7.4.1 --- Homogeneous star --- p.72 / Chapter 7.4.1.1 --- Axial QNM --- p.72 / Chapter 7.4.1.2 --- Polar QNM --- p.76 / Chapter 7.4.2 --- Polytropic star --- p.78 / Chapter 7.4.2.1 --- Axial QNM --- p.78 / Chapter 7.4.2.2 --- Polar QNM --- p.80 / Chapter 7.4.3 --- Effects of specific ingredients of EOS --- p.82 / Chapter 7.5 --- A comparison of methods for evaluating outgoing-wave solutions --- p.85 / Chapter 7.6 --- Summary --- p.88 / Chapter Chapter 8. --- Oscillations of realistic neutron stars --- p.89 / Chapter 8.1 --- Motivations of study --- p.89 / Chapter 8.2 --- Equations of states --- p.90 / Chapter 8.3 --- Static stars --- p.94 / Chapter 8.4 --- Axial QNM --- p.96 / Chapter 8.5 --- Polar QNM --- p.97 / Chapter 8.6 --- Effects of specific ingredients of EOS --- p.99 / Chapter 8.6.1 --- Effects of neutral pion condensate --- p.100 / Chapter 8.7 --- Summary --- p.101 / Chapter Chapter 9. --- Oscillations of quark stars --- p.105 / Chapter 9.1 --- Motivations of study --- p.105 / Chapter 9.2 --- The equations of states --- p.106 / Chapter 9.2.1 --- Light-quark stars (LQS) --- p.106 / Chapter 9.2.2 --- Hybrid neutron stars with quark cores (HLQS) --- p.107 / Chapter 9.2.3 --- Hybrid neutron stars with strange quark cores (HSSI and HSSII) --- p.107 / Chapter 9.3 --- Axial QNM --- p.111 / Chapter 9.4 --- Polar QNM --- p.114 / Chapter 9.5 --- Effects of specific ingredients of EOS --- p.117 / Chapter 9.6 --- Properties of wII modes --- p.118 / Chapter 9.7 --- Summary --- p.121 / Chapter Chapter 10. --- Conclusion --- p.123 / Chapter 10.1 --- Summary of results --- p.123 / Chapter 10.2 --- Outlook of the problem --- p.124 / Appendix A. Unit conventions --- p.126 / Appendix B. Proof of the regularity of the singular point Vrw(r = 0) --- p.127 / Appendix C. Derivation of transformation between Ψrwand Ψz --- p.129 / Appendix D. Newtonian Cowling Approximation --- p.132 / Chapter D.1 --- Cowling Approximation --- p.132 / Chapter D.2 --- Local Analysis --- p.134 / Chapter D.3 --- Existence of p and g-modes --- p.135 / Appendix E. Relativistic Cowling Approximation --- p.138 / Bibliography --- p.143

Time series of high resolution CFHT spectra of four δ Scuti stars are examined for consistency with the presence of nonradial pulsations (nrp). Each series exhibits a progression of subfeatures moving from blue to red through the absorption lines. We have reproduced the profile variations using a geometrical model which imposes sectorial modes on the surface of the star. Modeling of the low-degree modes is guided by radial-velocity variations and the known photometric variations. Synthetic spectra generated with the appropriate Teff and log g for each star are used as input for the model. In this way, the entire wavelength region covered by the observations can be reproduced and the effects of blending on the nrp profiles are included explicitly. The extension from a single-line model to one generated over a wide spectral region provides a much more sensitive comparison with the observations. In general, we find that the data can be reproduced by the combination of a high-degree mode (ℓ > 8) and a low-degree mode [ℓ < 2). The intrinsic line widths and υ sinί together set a limit on the resolution of the stellar surface and by including this resolution in our treatment we can estimate the velocity amplitude of the oscillations (~ 5 km/s). We find that low values of k (≤ 0.1) expected for p-mode oscillations are consistent with the observations. A possible relationship between the periods of the high- and low-degree modes is noted, the question of uniqueness is addressed and comparisons are made with models invoking starspots. For at least one of the stars (қ² Boo), it is impossible to fit the observations by a starspot model without assuming unrealistic values of radius or equatorial velocity. / Science, Faculty of / Physics and Astronomy, Department of / Graduate

Wu Jun = 中子星的極性w-模振盪 / 吳俊. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2005. / Includes bibliographical references (leaves 100-102). / Text in English; abstracts in English and Chinese. / Wu Jun = Zhong zi xing de ji xing w-mo zhen dang / Wu Jun. / Abstract --- p.i / Acknowledgement --- p.iii / Chapter 1 --- Introduction --- p.1 / Chapter 1.1 --- Background introduction and historical review --- p.1 / Chapter 1.2 --- Outline of the thesis --- p.3 / Chapter 1.3 --- Notations and conventions --- p.4 / Chapter 2 --- Equilibrium and oscillations of Relativistic stars --- p.5 / Chapter 2.1 --- Relativistic stars --- p.5 / Chapter 2.1.1 --- Equilibrium configuration --- p.6 / Chapter 2.1.2 --- Equation of state --- p.7 / Chapter 2.2 --- Oscillations of relativistic stars --- p.9 / Chapter 2.2.1 --- Families of fluid modes --- p.10 / Chapter 2.2.2 --- Families of spacetime modes (w-mode) --- p.11 / Chapter 3 --- Polar oscillations of neutron stars --- p.14 / Chapter 3.1 --- Axial oscillations of neutron stars --- p.14 / Chapter 3.2 --- LD formulation --- p.16 / Chapter 3.2.1 --- Equations inside star --- p.17 / Chapter 3.2.2 --- Boundary conditions at r = 0 and r = R --- p.19 / Chapter 3.2.3 --- Perturbations outside star --- p.21 / Chapter 3.3 --- AAKS formulation --- p.22 / Chapter 3.3.1 --- Equations inside the star --- p.23 / Chapter 3.3.2 --- Behavior at the center and the stellar surface --- p.25 / Chapter 3.3.3 --- Evolution outside star --- p.28 / Chapter 3.3.4 --- Connection formula --- p.29 / Chapter 4 --- QNMs of polar oscillations --- p.31 / Chapter 4.1 --- Solution outside star --- p.31 / Chapter 4.2 --- LD approach --- p.32 / Chapter 4.3 --- Hamiltonian constraint --- p.33 / Chapter 4.4 --- Boundary conditions a.t r = R --- p.37 / Chapter 4.5 --- Direct integration scheme (DIS) --- p.42 / Chapter 4.6 --- Two-way integration scheme (TIS) --- p.43 / Chapter 4.7 --- Connect the interior and exterior solutions --- p.45 / Chapter 4.8 --- Numerical results --- p.46 / Chapter 5 --- Polar oscillations without fluid motions --- p.50 / Chapter 5.1 --- Zero pressure variation approximation (ZPVA) --- p.51 / Chapter 5.1.1 --- Evolution formulas --- p.51 / Chapter 5.1.2 --- Boundary conditions --- p.53 / Chapter 5.1.3 --- Approximate QNMs --- p.55 / Chapter 5.2 --- Zero density variation approximation (ZDVA) --- p.55 / Chapter 5.2.1 --- Single equation formulas --- p.58 / Chapter 5.2.2 --- Numerical results --- p.61 / Chapter 5.2.3 --- Summary --- p.62 / Chapter 5.3 --- Application of ZDVA --- p.65 / Chapter 5.3.1 --- Relation between axial and polar w-modes --- p.65 / Chapter 5.3.2 --- Analysis --- p.66 / Chapter 6 --- Universal behavior of polar QNMs --- p.69 / Chapter 6.1 --- Universal behavior of polar w-modes --- p.70 / Chapter 6.2 --- Ordinary CQM of neutron stars --- p.71 / Chapter 6.2.1 --- TOV parameters of a CQM star --- p.71 / Chapter 6.2.2 --- Stability problem of CQM --- p.73 / Chapter 6.2.3 --- EOS near the surface --- p.75 / Chapter 6.3 --- Scaling behavior of polar oscillations --- p.78 / Chapter 6.3.1 --- Scaling behavior of fluid motions --- p.79 / Chapter 6.3.2 --- Scaled wave equations --- p.80 / Chapter 6.4 --- Scaled Cubic-Quintic Model (SCQM) --- p.82 / Chapter 7 --- Conclusion --- p.85 / Chapter 7.1 --- Summary of Our Work --- p.85 / Chapter 7.2 --- Outlook --- p.86 / Chapter A --- Expansion of Hamiltonian constraint around the center --- p.88 / Chapter B --- Factorization integration scheme (FIS) --- p.92 / Chapter C --- Equivalence of two definitions of the Zerilli function --- p.96

Thesis--Harvard University. / Bibliography: leaves 167-176.

The absorption line profiles of Spica (α Virginis, HD116658, B1.5IV, m=0.97) show features, at about the 1% level, moving from the blue wavelengths towards the red wavelengths. A series of spectra were taken, at the 1.22 m telescope at the Dominion Astrophysical Observatory on three nights in April, 1982 and two nights in April, 1984, to study these moving features. As Spica is a member of a binary system, the effect of the secondary had to be removed from the observations. This was done by subtracting a template spectrum which had been scaled, broadened and shifted to match the secondary, from each observation. The required shifts were determined using the orbital elements on blended nights and using the Fahlman-Glaspy small-shifts technique on unblended nights. An average of all the spectra was then subtracted from each observation. The resulting series of residuals clearly show the motion of the features seen in the line profiles. The acceleration of the features was estimated to be between 0.0055 and 0.0068 kms⁻². Assuming the features are due to nonradial oscillations, this acceleration corresponds to waves moving slowly, about 5 to 20 kms⁻¹, in a prograde direction. The angular frequency of the oscillations, after accounting for the effects of rotation, would be about 3.4X10⁻⁵ rads⁻¹. A computer model that produces line profiles, under the assumption of a single nonradial oscillation, was used to produce profiles for comparison with observations. Using an [formula omitted]=8 and m=-8 mode, an intrinsic frequency of 3.4X10⁻⁵ rads⁻¹ and a stellar rotation rate of 190 kms⁻¹, the model produced profiles similar to those observed. The change in the model profiles with time was also similar to that observed. / Science, Faculty of / Physics and Astronomy, Department of / Graduate

by Lin Lap-Ming. / Thesis (M.Phil.)--Chinese University of Hong Kong, 1999. / Includes bibliographical references (leaves [105]-109). / Text in English; abstracts in English and Chinese. / by Lin Lap-Ming. / Abstract --- p.i / Acknowledgement --- p.ii / Contents --- p.iii / List of Figures --- p.vi / List of Tables --- p.ix / Chapter Chapter 1. --- Introduction --- p.1 / Chapter 1.1 --- Physical Motivation --- p.1 / Chapter 1.2 --- Quasi-Normal Modes --- p.3 / Chapter 1.3 --- Superfluidity in Neutron Stars --- p.7 / Chapter 1.4 --- Outline of this Thesis --- p.9 / Chapter Chapter 2. --- The Ordinary Perfect Fluid Neutron Stars --- p.11 / Chapter 2.1 --- The Equilibrium Neutron Star Models --- p.11 / Chapter 2.2 --- Non-Radial Oscillations of Neutron Stars --- p.14 / Chapter 2.3 --- The Quasi-Normal Modes of Stars --- p.17 / Chapter 2.3.1 --- The Fluid Modes --- p.17 / Chapter 2.3.2 --- The Spacetime Modes --- p.18 / Chapter Chapter 3. --- The General Relativistic Superfluid Formalism --- p.22 / Chapter 3.1 --- The Carter Formalism --- p.22 / Chapter 3.2 --- The Master Function --- p.25 / Chapter Chapter 4. --- The Equilibrium Superfluid Neutron Stars --- p.27 / Chapter 4.1 --- The Equilibrium Configurations --- p.27 / Chapter 4.2 --- Initial and Boundary Conditions --- p.34 / Chapter 4.3 --- Polytropic Models --- p.36 / Chapter Chapter 5. --- Non-Radial Oscillations of Superfluid Neutron Stars --- p.40 / Chapter 5.1 --- The Linearized Field Equations Inside the Star --- p.40 / Chapter 5.1.1 --- Equations for Even-Parity Perturbations --- p.45 / Chapter 5.1.2 --- Equations for Odd-Parity Perturbations --- p.48 / Chapter 5.2 --- Initial and Boundary Conditions --- p.49 / Chapter 5.2.1 --- Radial Integration Initial Conditions --- p.49 / Chapter 5.2.2 --- Boundary conditions at the Surface --- p.55 / Chapter 5.3 --- The Linearized Field Equations Outside the Star --- p.57 / Chapter 5.4 --- Numerical Technique --- p.60 / Chapter Chapter 6. --- Quasi-Normal Modes Extraction --- p.62 / Chapter 6.1 --- Numerical Techniques for Quasi-Normal Modes Extraction --- p.62 / Chapter 6.2 --- The Leaver Series --- p.64 / Chapter 6.3 --- The Graphical Method --- p.67 / Chapter Chapter 7. --- The Quasi-Normal Modes of Superfluid Neutron Stars --- p.69 / Chapter 7.1 --- Polytropic Models --- p.69 / Chapter 7.1.1 --- The w-modes --- p.70 / Chapter 7.1.2 --- The f- and p-modes --- p.74 / Chapter 7.2 --- Ideal Neutron-Proton-Electron Gas --- p.82 / Chapter 7.3 --- Convergence Tests and Accuracy --- p.92 / Chapter Chapter 8. --- Conclusion --- p.95 / Appendix A. Speeds of Sound --- p.97 / Appendix B. Equations for Radial Oscillations --- p.99 / Appendix C. Numerical Technique for Solving Leaver's Series --- p.101 / Appendix D. Scaling in Numerical Calculations --- p.103 / Bibliography --- p.105

Wong, Ka Sin Jamie = 超流性對中子星振盪的影響 / 黃家倩. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2009. / Includes bibliographical references (p. 212-215). / Abstract also in Chinese. / Wong, Ka Sin Jamie = Chao liu xing dui zhong zi xing zhen dang de ying xiang / Huang Jiaqian. / Chapter 1 --- Introduction --- p.1 / Chapter 1.1 --- Motivations --- p.1 / Chapter 1.2 --- Outline of Thesis --- p.3 / Chapter 1.3 --- Notation and Conventions --- p.4 / Chapter 2 --- The Relativistic Superfluid Star --- p.7 / Chapter 2.1 --- The Carter Formalism --- p.7 / Chapter 2.2 --- The Equilibrium Superfluid Star Models --- p.9 / Chapter 2.3 --- Non-Radial Oscillations of Superfluid Neutron Star --- p.13 / Chapter 2.3.1 --- Equations for Even-Parity Perturbations --- p.16 / Chapter 2.3.2 --- Equations for Odd-Parity Perturbations --- p.18 / Chapter 2.3.3 --- Linearised Equations Outside the Star --- p.19 / Chapter 2.3.4 --- Boundary Conditions for Quasinormal Modes --- p.21 / Chapter 2.3.5 --- Quasinormal Mode Spectrum of Superfluid Stars --- p.22 / Chapter 3 --- Universality in Superfluidf-mode --- p.25 / Chapter 3.1 --- What is an f-mode? --- p.25 / Chapter 3.2 --- Uncoupled Polytropic Master Function for Superfluid Stars --- p.27 / Chapter 3.3 --- Reparametrising the Uncoupled Polytropic Master Function --- p.29 / Chapter 3.4 --- f-mode Frequency of Uncoupled Polytropic Superfluid Stars --- p.30 / Chapter 3.5 --- "Derivation of Superfluid Mode Frequency for a Newtonian Sphere of Two Homogeneous, Incompressible, Uncoupled Fluids" --- p.40 / Chapter 4 --- Effects of Entrainment on Superfluid Mode Frequencies --- p.45 / Chapter 4.1 --- What is entrainment? --- p.45 / Chapter 4.2 --- Numerical Results --- p.48 / Chapter 4.3 --- Newtonian Variational Formalism --- p.51 / Chapter 4.4 --- Deriving the Approximate First Order Shift --- p.54 / Chapter 5 --- Variational Principle for Polar Modes --- p.60 / Chapter 5.1 --- Alternative Set of Perturbed Equations for Superfluid Neutron Star --- p.60 / Chapter 5.2 --- Boundary Conditions for Polar Quasinormal Modes --- p.64 / Chapter 5.3 --- Deriving the Variational Principle --- p.65 / Chapter 5.4 --- Recasting the Principle in Abstract Notation --- p.67 / Chapter 5.5 --- Doing Away with the Constraint Equations --- p.70 / Chapter 5.6 --- Regarding the Purely Real Nature of the First Order Term --- p.71 / Chapter 5.7 --- First Order Shift in Mode Frequency due to Entrainment --- p.74 / Chapter 6 --- Excitation of Quasinormal Modes --- p.77 / Chapter 6.1 --- Perturbed Equations Inside the Star --- p.77 / Chapter 6.2 --- Perturbed Equations Outside the Star --- p.78 / Chapter 6.3 --- Circular Orbits in Schwarzschild Spacetime --- p.80 / Chapter 6.4 --- Calculation of Source Term --- p.82 / Chapter 6.5 --- Determination of Amplitude --- p.85 / Chapter 6.6 --- Numerical Procedures --- p.86 / Chapter 6.7 --- Numerical Results --- p.89 / Chapter 7 --- Stability of Non-rotating Newtonian Superfluid Stars to Non-radial Oscillations --- p.91 / Chapter 7.1 --- Introduction --- p.91 / Chapter 7.2 --- Two-fluid Systems --- p.93 / Chapter 7.3 --- A Review of Basic Thermodynamics --- p.96 / Chapter 7.4 --- Perturbed System of Equations --- p.100 / Chapter 7.5 --- Schwarzschild Discriminant --- p.102 / Chapter 7.6 --- Variational Principle for Mode Frequency --- p.105 / Chapter 7.7 --- Stability of Polar Oscillations --- p.108 / Chapter 7.7.1 --- A Sufficient Condition for Stability --- p.109 / Chapter 7.7.2 --- A Necessary and Sufficient Condition for the Occurrence of Zero-frequency Modes --- p.112 / Chapter 7.7.3 --- Conditions for Instability --- p.119 / Chapter 7.8 --- A Little Application to Zero-temperature Superfluid Star --- p.121 / Chapter 7.9 --- Inclusion of Non-dissipative Magnus-typed Force --- p.122 / Chapter 7.10 --- Conclusion --- p.123 / Chapter 8 --- A Single Scalar Governing Stability of Newtonian Superfluid Neutron Stars to Non-radial Oscillations --- p.125 / Chapter 8.1 --- Introduction --- p.125 / Chapter 8.2 --- Summary of Results of the Last Chapter --- p.126 / Chapter 8.3 --- Motivation --- p.129 / Chapter 8.4 --- Occurrence of Neutral Modes --- p.131 / Chapter 8.5 --- S> 0 Implies Stability to Non-radial Oscillations --- p.133 / Chapter 8.6 --- S < 0 On a Finite Interval of r Implies Instability --- p.135 / Chapter 8.7 --- Conclusion --- p.137 / Chapter 9 --- Lagrangian Perturbation Theory for Rotating Non-relativistic Superfluid Stars --- p.138 / Chapter 9.1 --- Perturbation Operators --- p.139 / Chapter 9.2 --- Perturbing the Dynamical Equations --- p.143 / Chapter 9.3 --- Variational Principle and Symplectic Structure --- p.147 / Chapter 9.4 --- Showing Antisymmetry of B --- p.149 / Chapter 9.5 --- Showing Symmetry of C --- p.154 / Chapter 9.6 --- Canonical Displacement --- p.157 / Chapter 9.7 --- Using Canonical Energy in Stability Calculation --- p.163 / Chapter 9.8 --- Instability of r-mode for a Superfluid Star --- p.164 / Chapter 9.9 --- CFS Instability of Normal Modes --- p.169 / Chapter 10 --- Conclusion --- p.172 / Chapter A --- Some Useful Relations --- p.174 / Chapter B --- Derivation of Equations Given in Section 5.1 --- p.176 / Chapter C --- Order Analysis of Quantities at Stellar Radius --- p.179 / Chapter D --- Condition for the Occurrence of Non-radiating Modes --- p.182 / Chapter E --- Perturbed Equations for Polar Oscillations and Boundary Conditions --- p.186 / Chapter F --- Deriving the Variational Principle --- p.191 / Chapter G --- Discerning Similarity with Ordinary-fluid Variational Expression --- p.195 / Chapter G.l --- T'=0 --- p.195 / Chapter G.2 --- T'=0 --- p.199 / Chapter H --- A Condition for Instability of a Dynamical System --- p.202 / Chapter I --- Derivation of Zeroth-order r-mode Frequency --- p.205 / Chapter J --- Spin-s Spherical Harmonics --- p.207 / Chapter J.1 --- Spin-s Quantities --- p.207 / Chapter J.2 --- Motivation of Spin-s Spherical Harmonics --- p.208 / Chapter J.3 --- Proof of a Relation --- p.210 / Bibliography --- p.212

Chan, Pak On = 星體震動的分析方法 / 陳柏安. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2011. / Includes bibliographical references (p. 117-119). / Abstracts in English and Chinese. / Chan, Pak On = Xing ti zhen dong de fen xi fang fa / Chen Boan. / Chapter 1 --- Introduction --- p.1 / Chapter 1.1 --- Background --- p.1 / Chapter 1.2 --- Outline of the Content --- p.3 / Chapter 2 --- Preliminaries --- p.5 / Chapter 2.1 --- Einstein Equation --- p.5 / Chapter 2.1.1 --- Hydrostatic Equilibrium --- p.6 / Chapter 2.1.2 --- Linearized Stellar Pulsation --- p.7 / Chapter 2.1.3 --- Gravitational Radiation --- p.11 / Chapter 2.2 --- Classification of Modes --- p.13 / Chapter 2.2.1 --- Fundamental Mode --- p.14 / Chapter 2.2.2 --- Pressure Modes --- p.14 / Chapter 2.2.3 --- Gravity Modes --- p.14 / Chapter 2.3 --- Relativistic Cowling Approximation --- p.15 / Chapter 3 --- Stellar Structure of Quark Stars --- p.19 / Chapter 3.1 --- Ordinary Quark Stars --- p.19 / Chapter 3.1.1 --- Stellar Profile --- p.20 / Chapter 3.1.2 --- Radius and Mass --- p.27 / Chapter 3.1.3 --- Moment of Inertia --- p.30 / Chapter 3.2 --- Effects of Finite Strange Quark Mass and Finite Temperature --- p.32 / Chapter 3.2.1 --- Sommerfeld's Expansions --- p.33 / Chapter 3.2.2 --- Static EOS for Quark Matter --- p.35 / Chapter 3.2.3 --- Corrections to Ordinary Quark Stars --- p.37 / Chapter 3.2.4 --- Induced Buoyancy under Adiabaticity --- p.40 / Chapter 3.2.5 --- Induced Buoyancy under Fixed Composition --- p.45 / Chapter 3.3 --- Addition of Nuclear Crust --- p.47 / Chapter 4 --- Pressure Modes --- p.52 / Chapter 4.1 --- Sturm-Liouville Equation for p-modes --- p.52 / Chapter 4.2 --- Asymptotic Expansion --- p.54 / Chapter 4.3 --- "P""modes for Quark Stars" --- p.57 / Chapter 4.4 --- p-modes for Neutron Stars --- p.62 / Chapter 4.5 --- p-modes for Hybrid Stars --- p.65 / Chapter 5 --- Gravity Modes --- p.74 / Chapter 5.1 --- Sturm-Liouville Equation for modes --- p.74 / Chapter 5.2 --- Asymptotic Expansion --- p.76 / Chapter 5.3 --- g-modes for Quark Stars --- p.78 / Chapter 5.4 --- modes for Hybrid Stars --- p.83 / Chapter 5.5 --- Conditions on the modes --- p.88 / Chapter 6 --- Fundamental Mode --- p.93 / Chapter 6.1 --- Overview of the f-mode Universalities --- p.93 / Chapter 6.2 --- Relation between Real Part and Imaginary Part of Mwf --- p.95 / Chapter 6.3 --- New Universalities of f-mode --- p.96 / Chapter 7 --- Conclusions and Remarks --- p.104 / Chapter A --- Scattering Approximation --- p.106 / Chapter B --- Series Solution to Stellar Profile of Quark Stars --- p.108 / Chapter C --- AAKAS Formalism under Cowling Approximation --- p.113 / Chapter D --- Series Solutions to the Spectra of p-modes and g-modes --- p.114 / Bibliography --- p.117

With recent advances in CCD technology, it has become possible to detect low-amplitude variability in stars. Thus, the number of low-amplitude variables has increased at an exceptional rate over the past decade. Many of these low-amplitude variables are pulsating stars such as Delta Scuti or Gamma Doradus stars, whose periods are on the orders of hours and days, respectively. One particular place where these variables are being found is in close binary systems. A close binary system has two components separated on the order of tens of solar radii and whose periods are on the order of days. Eclipsing binary systems occur when the orbital plane of the system is aligned such that the stars eclipse each other with respect to Earth’s line of sight. Soydugan et al. (2006) presented a paper in which a small number of eclipsing systems with a Delta Scuti-type pulsating component were analyzed. The group derived an observational relationship between the pulsation and orbital periods, thus indicating a physical phenomenon. The proposed project herein will seek to further determine whether there is a statistically significant relationship between the pulsation period and orbital parameters of close binary systems with a Delta Scuti-type pulsating component by searching for such pulsations in close binary systems using the method of high-precision CCD photometry. / Stellar dynamics -- Observations -- [Delta] Scuti stars in close binary systems. / Department of Physics and Astronomy

Yeung Yuk Ming. / Thesis (M.Phil.)--Chinese University of Hong Kong, 2002. / Includes bibliographical references (leaves 82-85). / Abstracts in English and Chinese. / Chapter 1 --- Introduction --- p.1 / Chapter 1.1 --- Motivations --- p.1 / Chapter 1.2 --- Historical background --- p.2 / Chapter 1.3 --- Outline of this thesis --- p.3 / Chapter 2 --- Mode classifications --- p.5 / Chapter 2.1 --- Fluid modes --- p.6 / Chapter 2.1.1 --- f mode (fundamental mode) --- p.6 / Chapter 2.1.2 --- p mode (pressure mode) --- p.7 / Chapter 2.1.3 --- g mode (gravity mode) --- p.7 / Chapter 2.2 --- w mode (spacetime mode) --- p.8 / Chapter 3 --- Oscillations of neutron stars --- p.10 / Chapter 3.1 --- The equilibrium configurations of neutron star models --- p.10 / Chapter 3.1.1 --- Newtonian stars --- p.10 / Chapter 3.1.2 --- Relativistic stars --- p.11 / Chapter 3.2 --- Perturbation of the star's equilibrium --- p.14 / Chapter 3.2.1 --- Axial perturbation equation --- p.15 / Chapter 3.2.2 --- Boundary conditions --- p.16 / Chapter 3.2.3 --- Numerical techniques --- p.16 / Chapter 3.2.4 --- The Quasinormal modes of stars --- p.18 / Chapter 4 --- Excitation and detection of QNMs --- p.20 / Chapter 4.1 --- Studies of excitation of stellar QNMs --- p.20 / Chapter 4.2 --- Detection of QNM ringing --- p.21 / Chapter 4.3 --- Parameter estimation --- p.23 / Chapter 5 --- Oscillations of realistic neutron stars --- p.28 / Chapter 5.1 --- Motivations of study --- p.28 / Chapter 5.2 --- Realistic equations of state --- p.29 / Chapter 5.3 --- Axial QNM --- p.36 / Chapter 6 --- Logarithmic perturbation method --- p.38 / Chapter 6.1 --- Introduction --- p.38 / Chapter 6.2 --- Logarithmic perturbation theory --- p.39 / Chapter 6.3 --- Evaluation of perturbation formulae --- p.42 / Chapter 6.3.1 --- The first-order perturbation --- p.42 / Chapter 6.3.2 --- The second-order perturbation --- p.47 / Chapter 6.4 --- Comparison of LPT calculations with exact results --- p.47 / Chapter 6.5 --- Discussion --- p.51 / Chapter 7 --- Scaled coordinate logarithmic perturbation method --- p.53 / Chapter 7.1 --- Rescaling of the axial perturbation equations --- p.54 / Chapter 7.1.1 --- The original axial perturbation equations --- p.55 / Chapter 7.1.2 --- The rescaled axial perturbation equations --- p.56 / Chapter 7.2 --- The formalism of SCLPT --- p.57 / Chapter 7.2.1 --- Logarithmic perturbation theory --- p.59 / Chapter 7.2.2 --- First-order perturbation --- p.63 / Chapter 7.2.3 --- Second-order perturbation --- p.65 / Chapter 7.3 --- Comparison of the perturbation calculation with the exact result --- p.67 / Chapter 7.4 --- Discussion --- p.70 / Chapter 8 --- Conclusion --- p.73 / Chapter 8.1 --- Summary --- p.73 / Chapter 8.2 --- Outlook --- p.74 / Chapter A --- Units conventions --- p.76 / Chapter B --- Numerical technique in Leaver's series --- p.77 / Chapter C --- Method of numerical derivatives --- p.80 / Bibliography --- p.82