No description available.

Inaug.-diss.--Greifswald. / Lebenslauf.

Inaug.-diss.--Greifswald. / Lebenslauf.

Thesis (Ph. D.)--Columbia University, 1915. / Vita. "Reprinted from the Physical review, n.s., vol. VI, no. 6, December, 1915."

No abstract included. / Science, Faculty of / Mathematics, Department of / Graduate

A program of research has been undertaken to examine the interaction between vortex shedding and the galloping type oscillation which square cylinders are subject to when immersed in a water stream. It is possible that the fluctuating force from the vortex shedding could quench the galloping oscillation if it acts as a forced oscillation (independent of cylinder motion). An experiment was designed where a square cylinder with one degree of freedom could oscillate transversely to the water flow. The amplitude and frequency of the cylinder oscillation were measured. By using a hot film anemometer spectra of the fluctuating velocity in the wake were taken to determine what frequencies vortex shedding occurred at. The results show that for velocities greater than the resonant velocity the galloping oscillation is dominant and the cylinder motion controls the frequencies of the wake. For velocities less than the resonant velocity no galloping occurs and the vortex shedding seems to control any cylinder motion which occurs. To explain this type of response a mathematical model has been constructed. The model is a set of two coupled self excited oscillators} one with the characteristics of the galloping oscillation and the other with the characteristics of the fluctuating lift force from the vortex shedding. Using the model some aspects of the observed interaction are explained. / Applied Science, Faculty of / Mechanical Engineering, Department of / Unknown

A new technique for detecting solar oscillations in the visible to near infrared continuum has been developed and tested at the Santa Catalina Laboratory for Experimental Relativity by Astrometry (SCLERA). In 1985, measurements of the solar radiation intensity near disk center were made by Oglesby (1986, 1987). The results of these observations have been compared to the reported detections and classifications by Hill (1984, 1985) and Rabaey and Hill (1987) of the low-order, low-degree acoustic modes; the intermediate degree f-modes; and the low-order g-modes. For the low-order, low-degree, acoustic modes and the intermediate degree f-modes, a total of 40 multiplets were used in the analysis. The coincidence rates between the peaks in the power spectrum of the 1985 observations and the classified frequency spectrum for multiplets taken in subgroups of ≈5 (same n and contiguous in ℓ) are typically 4-5 σ above the accidental coincidence rate. The maximum coincidence rates for these same subgroups of multiplets were found to occur for frequency shifts of the classified spectrum ranging from -0.27 μHz for modes that are sensitive to the internal properties near the bottom of the convection zone to 0.06 μHz for modes that are sensitive to internal properties near the top of the convection zone. Also included in this work is a comparison of diameter measurements obtained at SCLERA in 1978 (Caudell 1980) with the classified modes mentioned above. Agreement in this case is at the 3.1 σ level for both the f-mode (n = 0) multiplets with 21 ≤ ℓ ≤ 36 and the n = 1, 6 ≤ ℓ ≤ 12 acoustic modes. The confirmation of the detection and classification of the low-order g-modes of oscillation was found to be at the 3.3 σ level. Additionally, the m dependence of the 1985 power spectrum was found to behave in the manner expected for the proper classifications in m for the g-modes.

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

Reproduction de : Thèse de doctorat : Physique nucléaire : Lyon 1 : 2004. / Titre provenant de l'écran titre. 131 réf. bibliogr.

Thesis (doctoral)--Königl. Technische Hochschule zu Berlin, 1912. / Includes bibliographical references.