Thesis (M.A.)--香港中文大學. / Includes bibliographical references (leaves 405-407). / Thesis (M.A.)--Xianggang Zhong wen da xue. / Chapter 第一章 --- 生平 / Chapter 第一節 --- 詩人的時代 --- p.1-26 / Chapter 第二節 --- 詩人的里籍和生年 --- p.27-49 / Chapter 第三節 --- 詩人的仕履 --- p.50-78 / Chapter 第四節 --- 詩人的家境 --- p.79-101 / Chapter 第一章 --- 附錄 鮑照年譜簡編 --- p.102-153 / Chapter 第二章 --- 成就 --- p.154-156 / Chapter 第一節 --- 取法前人 --- p.157-186 / Chapter 第二節 --- 取法時人 --- p.187-216 / Chapter 第三節 --- 詩人的藝術成果及影響 --- p.217-291 / Chapter 第三章 --- 詩人重要作品專論 / Chapter 第一節 --- 擬行路難的有關問題 --- p.292-315 / Chapter 第二節 --- 蕪城賦及辭賦述要 --- p.316-357 / Chapter 第四章 --- 研究詩人作品著錄 / Chapter 第一節 --- 歷代集評 --- p.358-394 / Chapter 第二節 --- 研究詩人及其作品書刊文章著錄 --- p.395-404 / 附錄 / 主要參考書目 --- p.405-407

Based on a Ph.D. thesis in the Dept. of Electrical Engineering, 1968. / Bibliography: p.125-126.

This thesis is an analytical study of various cadenzas written for the first movement of Mozart’s Piano Concerto No.20 in D minor, K.466. As one of the six of his own concertos for which Mozart did not provide an original cadenza, the D minor concerto poses an important challenge to the performer: should she compose or improvise her own cadenza, or should she select one written by someone else? Many composer/pianists active during the nineteenth and twentieth centuries penned cadenzas to this concerto for their own use, and this thesis explores those by August Eberhard Müller, Emanuel Aloys Förster, Ludwig van Beethoven, Johann Nepomuk Hummel, Charles-Valentin Alkan, Clara Schumann, Johannes Brahms, Ferruccio Busoni, Bedrich Smetana and Paul Badura-Skoda. In addition to these written-out cadenzas, it also discusses improvised cadenzas in the recordings by Robert Levin and Chick Corea. Each composer/pianist’s unique compositional style is illuminated through the study of each cadenza, and consideration of these styles allows multiple views on a single concerto. A discussion of the meaning and history of cadenzas precedes the analytical study, and in conclusion, the author contributes her own cadenza.

In this work, the effect of rotation on the oscillation frequencies of some radially and nonradially oscillating Delta-Scuti stars have been explored. Rotation has been considered as a perturbation and treated up to the second order. Series of evolutionary models have been calculated for the oscillating stars in question and compared with the observational parameters. Three stars are considered: V350 Peg with no rotation, CC And with a rotational velocity Vsini=20 km/s, and BS Tuc with Vsini=130 km/s. We find that splitting in the oscillation frequencies are conspicuous especially in fast rotating stars, with a considerable contribution from the related terms due to second order effect.

In this work, the CHANDRA ACIS-S3 data of the old classical nova RR Pic (1925) is presented. The source is detected with a count rate of 0.067 (+-0.002) c/s in the 0.3-5.0 keV energy range. The orbital period of the binary system in X-ray wavelengths is detected. X-ray spectrum of RR Pic can be represented by a composite model of bremsstrahlung with a photoelectric absorption, two absorption lines centered around 1.1-1.4 keV and 5 Gaussian emission lines centered at around 0.3-1.1 keV . The best t bremsstrahlung temperature derived from the model ranges from 0.99 to 1.60 keV and the unabsorbed X-ray flux is found to be 2.51 (+0.39 -1.21) erg/cm2/s in the 0.3-5.0 keV range.The absorption lines correspond to several transitions of Fe, Ne and Na. The emission lines correspond to various transitions of S, N, O, C, Ne and Fe / and observations with better spectral resolution are needed to determine the exact transitions. The source spectrum is better explained with photoionized plasma model rather than the cooling flow model. It has also been found that the neutral Hydrogen column density differs for orbital minimum and orbital maximum spectra with values 0.25 (+0.23 -0:18)*10^22 atoms/cm2 and 0.64 (+0.13 -0.14)*10^22 atoms/cm2 respectively at 3 sigma confidence level. The difference of neutral Hydrogen column density between the maximum and minimum phase spectra indicates existence of a warm absorbing region on the disc at the location of the impact zone.

In this study spectral and photometric data of the SAX J2103.5+4545 Be/X-ray system are given. The spectral data were taken from June 2007 to September 2008 with the 1.5 m Russian-Turkish telescope, whereas the photometric data were obtained using ROTSE-IIId archive from June 2004 to November 2008. The photometric data up to April 2007 shows that the system was in quiescence in the optical region. But, in the 23rd of April 2007, the system&#039 / s luminosity underwent a large increase, which is in agreement with X-ray data. This increase was approximately 1 mag. Also, the Halpha line was displaying an emission with increased equivalent width proportional to the outburst. Afterwards, the Halpha line profile changed from a double peaked emission into a single peaked absorption, which is in agreement with the system&#039 / s structure. This means that the Be star threw away its disc and its light curve fell back to its old luminosity.

In this thesis we analyse X-ray data of accretion powered low mass and high mass X-ray binaries to understand the nature of their accretion mechanisms by searching for some clues of viscous time-scales of their accretion discs, if they have, in their low frequency power density spectra created from their long-term X-ray observations, or by doing pulse timing analysis with much shorter X-ray data to detect the effects of torque fluctuations caused by the accreting material on the pulsar. The low mass and high mass X-ray binaries we analysed have breaks in their power density spectra, which are attributed to the role of viscosity in the formation of accretion discs. Although, the time-scales corresponding to these break frequencies are smaller than the predictions of the Standard theory of accretion discs, the sources give consistent results among themselves by displaying the expected correlation between their break and orbital frequencies. The correlation curve of LMXBs implies thicker appearing accretion discs than those assumed by the theory. The dichotomy of the HMXBs on this curve points out the different origins of accretion that these sources may have, and offers a way to distinguish the stellar-wind fed systems from the Roche-lobe overflow systems. The timing and spectral analysis of Swift J1626.6-5156 reveal a correlation between the spin-up rate and the luminosity of the source implying that the pulsar is accretion-powered. This correlation together with the characteristics of the X-ray spectra enables us to estimate the magnetic field and the distance of the source. The AXP 1E 2259+586 does not display any signs of viscous time-scale in its low frequency power density spectra, and its pulse timing analysis gives a much smaller torque noise value than that expected from accretion powered pulsars. In addition, the analysis results presented in this thesis reveal magnetar-like glitches which differ than those of radio pulsars, due to the presence of the strong magnetic field of the pulsar. These results eliminate the possibility that the AXP is an accretion-powered pulsar.

In this study, vibrational properties and stability of delta-Scuti like pulsating pre-main sequence stars have been investigated. Studies were held in the mass range 2-4 Mo and limited to radial linear adiabatic pulsations. Numerical computations were performed by the oscillation program written by Kirbiyik &amp / Al-Murad (1993). The models were selected to be at the latest phases of the pre-main sequence evolution where the luminosity starts to increase. We have limited our calculations upto the end of the radiative inner regions, since at the surface of the star, our adiabatic perturbation computation does not perfectly fit to the relatively thin non-adiabatic convective envelope of the star. The results of the stability analysis showed that the PMS models undergo an instability whose time period is a function of mass. Instability Strip of pulsating PMS stars was re-drawn with comparison to M. Marconi &amp / F.Palla (1998). The effect of gravitational contraction on stability was also investigated.

This thesis is composed of three published articles. Each chapter is devoted to an article. In the first part the origin of some of the single radio pulsars with relatively low magnetic fields (B &lt / 1e12 G) and with characteristic ages (tau) less than 1e7 years is questioned. We proposed that such pulsars might occur as a result of the disruption of high-mass X-ray binary systems after a second supernova explosion. In these binaries, mass accretion on to the surface of X-ray pulsars may lead to the decrease in the magnetic field from its value at birth (B similar to 1e12 &ndash / 1e13 G) down to B &lt / 1e12 G similar to the processes in low-mass X-ray binaries. In the second part we put together many observational data of SGRs and AXPs and analyzed them with the main purpose of the removal of contradiction between the real age (t) of these objects and their characteristic times of period change (tau). SGRs and AXPs are neutron stars that undergo star-quakes. Magnetic activity increases from time to time. We suggest that as a result of these processes plasma is ejected from the NS and propeller mechanism starts to work. Due to propeller effect dP/dt increases, tau decreases. Indeed, high dP/dt values are observed in SGRs and in half of the AXPs. Then, for a long time NS looses its activity, its dP/dt decreases, tau increases and rapid cooling begins. It seems that there is a possible transition between each NS stage (AXP,SGR,dim). This transient cycle may be repeated once or several times until the spin period of the neutron star becomes P &gt / 10 - 12 s. Observational data and mainly the data of AXP 1E 1048-5937 and DRQNS RX J1308.8+2127 support this idea. In the third part dependence of the X-ray luminosity (Lx) of young single pulsars, due to ejection of relativistic particles, on electric field intensity, rate of rotational energy loss (dE/dt), magnetic field, period and some other parameters of neutron stars are discussed. Influence of the magnetic field and effects of some other parameters of neutron stars on the Lx - dE/dt and the Lx - tau(characteristic time) relations are considered. Evolutionary factors also play an important role in our considerations. Only the pulsars whose X-ray luminosity in the 2 &ndash / 10 keV energy band is greater than 1033 erg/s have pulsar wind nebula around them. The pulsars from which gamma-ray radiation has been observed have low X-ray luminosity in general.

Memoria (para optar al grado de magíster en derecho mención en derecho penal) / El contrato simulado como modalidad de comisión de delitos y no como delito independiente -- El delito del Artículo 466 del Código Penal. Otorgamiento de contrato simulado en perjuicio de los acreedores como modalidad comisiva de insolvencia punible -- El delito del Artículo 471 No. 2. Otorgamiento de contrato simulado en perjuicio de otro como modalidad comisiva de defraudación