The main concern of this study is how the bilingual dictionary of Arabic and English can serve the ArabicEnglish translator in his task of translating all types of Arabic texts. In order to achieve this objective a few issues and problems in bilingual lexicography have been discussed in this thesis and certain recommendations have been made. The thesis is divided in four chapters plus an appendix, as follows: - Chapter I discusses various aspects of the structure of the Arabic word, as it constitutes the largest number of lexical entries in the dictionary. Chapter II discusses the issue of word-meaning and bilingual equivalence and is divided into two sections: Section A discusses the signification of the word. Section B discusses bilingual equivalence in relation to the Ar-Eng dictionary, including discussions of certain semantic relations, viz., a1'ishtirak a11afZiy 'homonymy', a1taraduf 'synonymy' and a1' aDdad 'contranyms' (see Ch. III), and semantic fields theory. - Chapter III addresses the question of how translators would like the bilingual dictionary prepared for their own needs, and is divided into two sections as follows: Section A introduces the Ar-Eng Translator's Dictionary (AETD) as proposed by this study, and discusses through practical examples some of the major problems of bilingual dictionaries. Section B is devoted to discussing some real problems found in the most widely used Ar-Eng dictionary, Hans Wehr's Arabic-English dictionary, especially to highlight the importance of avoiding them in the AETD. - Chapter IV is concerned with the actual making of the AETD, and is divided into three sections as follows: Section A discusses the various issues and aspects involved in the preparation of the AETD; for instance, the entrysystem of the dictionary, what should be entered and what should not, the treatment of different lexemes, the choice of BEs, and meaning discrimination. Section B introduces a proposed framework of the AETD, i.e., how it should look in relation to its form and content. It also includes some important notes for the AETD lexicographer, and finally a conclusion for the whole study with recommendations for further research. The Appendix consists of a list of sample entries employing the recommendations suggested for the AETD in the study, in addition to providing comparative notes with the same entries as cited in HW. To sum up, it is quite important that translators should have in their possession an interlingual dictionary that is specifically designed for them to suit their specific needs. This will save them time, money and effort which would otherwise be spent on numerous reference works alone.

The explosion of a massive star results in an immense expulsion of energy and stellar debris (ejecta) that are heated to extremely high temperatures forming what is known as a super va remnant (SNR). Presented is a CHANDRA 0.5-10 keV X-ray study of the SNR RCW 103, a bright SNR that contains the unusual compact object 1E 161348-5055. This study is the first dedicated and complete imaging and spatially resolved spectroscopic study of the SNR aimed at addressing the intrinsic properties of the SNR, including the explosion energy, ambient density, age, and distance. The SNR's X-ray spectrum is dominated by thermal X-ray emission, requiring globally two components with temperatures at ~0.6 keV and ~0.27 keV and di fferent ionization timescales and abundances. We identify clumpy regions of enhanced abundances suggesting the presence of ejecta. The SNR age is estimated at 1.0-3.7 kyr at a distance of 3.1 kpc. / May 2016

Using the computer code Monte Carlo N-Particle (MCNP), doses were calculated for organs of interest such as the large intestine, urinary bladder, testes, and kidneys while patients were undergoing prostate brachytherapy. This research is important because the doses delivered to the prostate are extremely high and the organs near the prostate are potentially at risk for receiving high doses of radiation, leading to increased probabilities of adverse health effects such as cancer. In this research, two MCNP version 4C codes were used to calculate the imparted energies to the organs of interest delivered by 125I and 103Pd. As expected, the organs nearest to the prostate received the highest energy depositions and the organs farthest from the prostate received the lowest energy depositions. Once the energy depositions were calculated, the doses to the organs were calculated using the known volumes and densities of the organs. Finally, the doses to the organs over an infinite time period were calculated.

Using the computer code Monte Carlo N-Particle (MCNP), doses were calculated for organs of interest such as the large intestine, urinary bladder, testes, and kidneys while patients were undergoing prostate brachytherapy. This research is important because the doses delivered to the prostate are extremely high and the organs near the prostate are potentially at risk for receiving high doses of radiation, leading to increased probabilities of adverse health effects such as cancer. In this research, two MCNP version 4C codes were used to calculate the imparted energies to the organs of interest delivered by 125I and 103Pd. As expected, the organs nearest to the prostate received the highest energy depositions and the organs farthest from the prostate received the lowest energy depositions. Once the energy depositions were calculated, the doses to the organs were calculated using the known volumes and densities of the organs. Finally, the doses to the organs over an infinite time period were calculated.

The steel company SSAB in Borlänge will, in the near future, replace its protective relays in one of their substations due to the condition and age of the relays. In connection with the change, SSAB intended to switch the current communication protocol IEC 60870-5-103 (IEC 103) to IEC 61850. They were thus interested in knowing what differences there were between these protocols and what were the technical and economical pros and cons for the change. To answer SSAB's questions, this bachelor thesis project was initiated with the aim of a feasibility study regarding the relays change and the protocol switching. To this purpose, the relevant parts of the substation and its functions were first examined to have an overall picture and the understanding of how they worked and interacted. After that, the communication protocols IEC 103 and IEC 61850 were investigated separately and comparatively. After a few weeks a visit was paid to SSAB to visually see what was to be done and to obtain a better understanding. During the visit, the substation that would receive new protection relays were shown and how their parts in the system were connected and interacted. Besides, other electrical devices were also shown, for example, large step-down transformers and a capacitor bank. After this, further study of the protocols, the relays as well as the associated parts were conducted and the information collected. Finally, the collected information was analysed, compared and documented in this thesis to generate a result and a comparison. From this feasibility study, it is clear that the new protocol had many advantages technically and some economically, which in particular include: 1) communication where IEC 103 uses master/slave at speeds up to 10 Mbit/s and IEC 61850 uses client/server and peer to peer at speeds between 100 Mbit/s to 1 Gbit/s; 2) connection where IEC 103 was point to point and with IEC 61850 it will be connected in ring formation for better redundancy; 3) interoperability where IEC 103 was limited by vendor specific codes, whereas IEC 61850 enabled interoperability through a common language and file format called SCL.

Nous savons que la grande majorité des étoiles WC9 produit de la poussière à base de carbone. Cette dernière doit se former dans des zones de très haute densité afin de survivre à l’environnement hostile qu’est celui du vent d’une étoile WR. Les étoiles WC appartenant à un système binaire WR + O produisent de la poussière quand les vents des deux étoiles entrent en collision et forment une zone de choc pouvant augmenter la densité du gaz d’un facteur 1000. Par contre, plusieurs étoiles WC9 n’ont, à ce jour, montré aucun signe de la présence d’un compagnon. Le but du projet est de tenter d’identifier un mécanisme alternatif responsable de la formation de poussière dans les étoiles WC9 n’appartenant pas à un système binaire. Nous présentons les résultats d’une campagne d’observation visant à caractériser la variabilité spectroscopique d’un échantillon de huit étoiles WC9 et une étoile WC8d. Nos résultats indiquent que la majorité des étoiles montrent des variations à grande échelle dans la raie d’émission C III 5696, soit à un niveau d’au moins 5% du flux de la raie et que les structures dans le vent ont une dispersion de vitesses de l’ordre de 150-300 km/s. De manière générale, les variations de vitesse radiales sont anti-corrélées avec le coefficient d’asymétrie de la raie, ce qui semble infirmer la présence d’un compagnon. Des observations en photométrie de l’étoile WR103 montrent une période de 9.1 ± 0.6 jours qui s’accorde avec les variations spectroscopiques et qui ne semble pas, de manière évidente, d’origine binaire. / We know that the majority of WC9 stars produces carbon-based dust. To survive in the hot and harsh environement that is the wind of a WR star, the dust grains must be formed in regions of very high density. We know that WC stars that are part of a WR + O system can produce dust at periastron passage where the collision of the two stellar winds is strong enough to produce shocks that compress the gas to densities up to a factor 103 higher than that of the WR star. However, so far, many WC9 stars have shown no signs of a companion. The goal of the current project is to identify a mechanism that could be responsible for the formation of dust in single WC9 stars. We present the results of an observing campaign which aimed to characterize the spectroscopic variability of eight WC9 stars and one WC8d star. Our results indicate that most stars show large scale variations of their C III 5696 emission line that reach at least 5% of the total line flux, and that the structures in the wind have a mean velocity dispersion of 150-300 km/s. In general, the radial velocity variations are anti-correlated with the skewness variations. This seems to indicate that the variations are not due to the presence of a companion. Photometric observations of WR 103 show a period of 9.1 ± 0.6 days that agrees with the spectroscopic variations and does not seem from binary origin.

Nous savons que la grande majorité des étoiles WC9 produit de la poussière à base de carbone. Cette dernière doit se former dans des zones de très haute densité afin de survivre à l’environnement hostile qu’est celui du vent d’une étoile WR. Les étoiles WC appartenant à un système binaire WR + O produisent de la poussière quand les vents des deux étoiles entrent en collision et forment une zone de choc pouvant augmenter la densité du gaz d’un facteur 1000. Par contre, plusieurs étoiles WC9 n’ont, à ce jour, montré aucun signe de la présence d’un compagnon. Le but du projet est de tenter d’identifier un mécanisme alternatif responsable de la formation de poussière dans les étoiles WC9 n’appartenant pas à un système binaire. Nous présentons les résultats d’une campagne d’observation visant à caractériser la variabilité spectroscopique d’un échantillon de huit étoiles WC9 et une étoile WC8d. Nos résultats indiquent que la majorité des étoiles montrent des variations à grande échelle dans la raie d’émission C III 5696, soit à un niveau d’au moins 5% du flux de la raie et que les structures dans le vent ont une dispersion de vitesses de l’ordre de 150-300 km/s. De manière générale, les variations de vitesse radiales sont anti-corrélées avec le coefficient d’asymétrie de la raie, ce qui semble infirmer la présence d’un compagnon. Des observations en photométrie de l’étoile WR103 montrent une période de 9.1 ± 0.6 jours qui s’accorde avec les variations spectroscopiques et qui ne semble pas, de manière évidente, d’origine binaire. / We know that the majority of WC9 stars produces carbon-based dust. To survive in the hot and harsh environement that is the wind of a WR star, the dust grains must be formed in regions of very high density. We know that WC stars that are part of a WR + O system can produce dust at periastron passage where the collision of the two stellar winds is strong enough to produce shocks that compress the gas to densities up to a factor 103 higher than that of the WR star. However, so far, many WC9 stars have shown no signs of a companion. The goal of the current project is to identify a mechanism that could be responsible for the formation of dust in single WC9 stars. We present the results of an observing campaign which aimed to characterize the spectroscopic variability of eight WC9 stars and one WC8d star. Our results indicate that most stars show large scale variations of their C III 5696 emission line that reach at least 5% of the total line flux, and that the structures in the wind have a mean velocity dispersion of 150-300 km/s. In general, the radial velocity variations are anti-correlated with the skewness variations. This seems to indicate that the variations are not due to the presence of a companion. Photometric observations of WR 103 show a period of 9.1 ± 0.6 days that agrees with the spectroscopic variations and does not seem from binary origin.

This paper sets out a particular concept of intellectual history for discussion and debate concerning the guidelines for our project for the International Dictionary of Intellectual Historians. First let me advance the idea that intellectual history is written everywhere, not only in West European countries, where it emerged, but in East European countries, too, and second that it really is a concept that applies not just to Europe alone but to the whole world, although this suggestion will vastly complicate our notions of intellectual history.

by Henry Gabbay. / Work performed under Contract N00014-67-A-0204-0076, Office of Naval Research, Multilevel Logistics Organization Models, NR 347-027, MIT/OSP 81138. / Bibliography: leaves 19-21.

Thesis (Ph.D.)--Syracuse University, 2008. / "Publication number: AAT 3333563."