With modern computer systems becoming more and more complicated, theimportance of rigorous testing to ensure the quality of the product increases.This, however, means that the cost to perform tests also increases. In orderto address this problem, a lot of research has been conducted during thelast years to find a more automated way of testing software systems. Inthis thesis, different algorithms to automatically explore and test a systemhave been implemented and evaluated. In addition to this, a second setof algorithms have been implemented with the objective to isolate whichinteractions with the system were responsible for a failure. These algorithmswere also evaluated and compared against each other. In the first evaluationtwo explorers, which I called DeBruijn and LStarExplorer, were consideredsuperior to the other. The first used a DeBruijn sequence to brute forcea solution while the second used the L*-algorithm to build an FSM overthe system under test. This FSM could then be used to provide a moreaccurate description for when the failure occurred. The result from thesecond evaluation were two reducers which both tried to recreate a failureby first applying interactions performed just before the failure occurred. Ifthis was not successful, they tried interactions further and further away, untilthe failure was triggered. In addition to this, the thesis contains descriptionsabout the framework used to run the different strategies. / D ̊a v ̊ara moderna datasystem blir allt mer komplicerade,  ̈okar detta st ̈andigtbehovet av rigor ̈osa tester f ̈or att s ̈akerst ̈alla kvaliteten p ̊a den slutgiltiga pro-dukten. Det h ̈ar inneb ̈ar dock att kostnaden f ̈or att utf ̈ora testerna ocks ̊ao  ̈ kar. F ̈or att f ̈ors ̈oka hitta en l ̈osning p ̊a det h ̈ar problemet har forsknin-gen under senare tid arbetat med att ta fram automatiserade metoder atttesta mjukvarusystem. I den h ̈ar uppsatsen har olika algoritmer, f ̈or attutforska och testa ett system, implementerats och utv ̈arderats. D ̈arut ̈overhar ocks ̊a en grupp algoritmer implementerats som ska kunna isolera vilkainteraktioner med ett system som f ̊ar det att fallera.  ̈aven dessa algoritmerhar utv ̈arderats och testats mot varandra. Resultatet fr ̊an det f ̈orsta ex-perimentet var tv ̊a explorers, h ̈ar kallade DeBruijn och LStarExplorer, somvisade sig vara b ̈attre  ̈an de andra. Den f ̈orsta av dessa anv ̈ande en DeBruijn-sekvens f ̈or att hitta felen, medan den andra anv ̈ande en L*-algoritm f ̈or attbygga upp en FSM  ̈over systemet. Den h ̈ar FSM:en kunde sedan anv ̈andasf ̈or att mer precist beskriva n ̈ar felet uppstod. Resultatet fr ̊an det andraexperimentet var tv ̊a reducers, vilka b ̊ada f ̈ors ̈okte  ̊aterskapa fel genom attf ̈orst applicera interaktioner som ursprungligen utf ̈ordes percis innan feletuppstod. Om felet inte kunde  ̊aterskapas p ̊a detta s ̈att, fortsatte de medatt applicera interaktioner l ̈angre bort tills felet kunde  ̊aterskapas. Ut ̈overdetta inneh ̊aller uppsatsen ocks ̊a beskrivningar av ramverken som anv ̈andsf ̈or att k ̈ora de olika strategierna.

This thesis studies the approximation of solutions to partial differential equations (PDEs) over domains discretized by the dual of a simplicial mesh. While `primal' methods associate degrees of freedom (DoFs) of the solution with specific geometrical entities of a simplicial mesh (simplex vertices, edges, faces, etc.), a `dual discretization method' associates DoFs with the geometric duals of these objects. In a tetrahedral mesh, for instance, a primal method might assign DoFs to edges of tetrahedra while a dual method for the same problem would assign DoFs to edges connecting circumcenters of adjacent tetrahedra. Dual discretization methods have been proposed for various specific PDE problems, especially in the context of electromagnetics, but have not been analyzed using the full toolkit of modern numerical analysis as is considered here. The recent and still-developing theories of finite element exterior calculus (FEEC) and discrete exterior calculus (DEC) are shown to be essential in understanding the feasibility of dual methods. These theories treat the solutions of continuous PDEs as differential forms which are then discretized as cochains (vectors of DoFs) over a mesh. While the language of DEC is ideal for describing dual methods in a straightforward fashion, the results of FEEC are required for proving convergence results. Our results about dual methods are focused on two types of stability associated with PDE solvers: discretization and numerical. Discretization stability analyzes the convergence of the approximate solution from the discrete method to the continuous solution of the PDE as the maximum size of a mesh element goes to zero. Numerical stability analyzes the potential roundoff errors accrued when computing an approximate solution. We show that dual methods can attain the same approximation power with regard to discretization stability as primal methods and may, in some circumstances, offer improved numerical stability properties. A lengthier exposition of the approach and a detailed description of our results is given in the first chapter of the thesis. / text

A Milky Way region in the direction of the North America and Pelican Nebulae is investigated using CCD photometry of 2600 stars in the Vilnius seven-color system. Its central part was covered with a CCD camera on the Maksutov wide-field telescope of the Moletai Observatory. Deeper CCD exposures for most interesting selected targets were taken with the 1 m telescope of the USNO Flagstaff Station. The author developed a new method for CCD data processing trying to reduce systematic errors and to increase photometric accuracy. This allowed us to measure M67 stars with high precision and use it as a CCD standard region in all our subsequent observations. To investigate interstellar extinction law in the area we obtained spectra for 33 B-type stars with the 2.3 m telescope of Steward Observatory at Kitt Peak. We also used near-infrared 2MASS data and other data sources when they were available. From photometric results in the Vilnius system we determined two-dimensional spectral types, color excesses, interstellar extinctions and distances of ~1300 stars. For more accurate determination of open cluster ages we recalibrated the zero-age main sequence in absolute magnitude vs. color diagram of the Vilnius system. We also investigated the possible connection between two open clusters in the area and surrounding star-forming region. Young stellar objects and possible ionizing sources of the NAP gas clouds were identified. / Naudojant CCD fotometriją, ištirta Paukščių Tako sritis Šiaurės Amerikos ir Pelikano ūkų kryptimi. Vilniaus fotometrinėje sistemoje išmatuota 2600 žvaigždžių. Didesnė sritis, apimanti abu ūkus ir tarp jų esantį dulkių debesį L935 buvo eksponuojama Molėtų observatorijos plataus lauko Maksutovo sistemos teleskopu. Mažesnės sritys, turinčios svarbių objektų, buvo eksponuojamos JAV laivyno observatorijos Flagstafo stoties 1 m. teleskopu. Autorius sukūrė metodiką. kaip ženkiai sumažinti sistematines redukcijos paklaidas ir padidinti CCD fotometrijos tikslumą. Tiksliai išmatuoti CCD fotometriniai standartai padrikąjame spiečiuje M67 bus naudojami tolimesniuose stebėjimuose. Ekstinkcijos dėsnio tyrimui buvo gauti 33 O-B žvaigždžių spektrai Stiuarto observatorijos 2.3 m teleskopu. Taip pat buvo panaudota 2MASS infraraudonosios fotometrijos katalogas ir kiti duomenys. Iš CCD ekspozicijų Vilniaus sistemoje fotometrijos daugumai fotometruotų žvaigždžių nustatyta: spektrinė ir šviesio klasė (MK sistemoje), spalvos ekscesas, tarpžvaigždinė ekstinkcija ir nuotolis. Tikslesniam padrikųjų spiečių amžiaus nustatymui iš naujo sukalibruota nulinio amžiaus pagrindinė seka Vilniaus fotometrinėje sistemoje. Ištirti du padrikieji žvaigždžių spiečiai esantys Šiaurės Amerikos ūko kryptimi ir patikrintas jų ryšys su aplinkine žvaigždėdaros sritimi. Aptikta apie 30 jaunų emisinių žvaigždžių ir 4 ar 5 žvaigždės, kurios galėtų būti ūkų jonizacijos šaltiniai.

Naudojant CCD fotometriją, ištirta Paukščių Tako sritis Šiaurės Amerikos ir Pelikano ūkų kryptimi. Vilniaus fotometrinėje sistemoje išmatuota 2600 žvaigždžių. Didesnė sritis, apimanti abu ūkus ir tarp jų esantį dulkių debesį L935 buvo eksponuojama Molėtų observatorijos plataus lauko Maksutovo sistemos teleskopu. Mažesnės sritys, turinčios svarbių objektų, buvo eksponuojamos JAV laivyno observatorijos Flagstafo stoties 1 m. teleskopu. Autorius sukūrė metodiką. kaip ženkiai sumažinti sistematines redukcijos paklaidas ir padidinti CCD fotometrijos tikslumą. Tiksliai išmatuoti CCD fotometriniai standartai padrikąjame spiečiuje M67 bus naudojami tolimesniuose stebėjimuose. Ekstinkcijos dėsnio tyrimui buvo gauti 33 O-B žvaigždžių spektrai Stiuarto observatorijos 2.3 m teleskopu. Taip pat buvo panaudota 2MASS infraraudonosios fotometrijos katalogas ir kiti duomenys. Iš CCD ekspozicijų Vilniaus sistemoje fotometrijos daugumai fotometruotų žvaigždžių nustatyta: spektrinė ir šviesio klasė (MK sistemoje), spalvos ekscesas, tarpžvaigždinė ekstinkcija ir nuotolis. Tikslesniam padrikųjų spiečių amžiaus nustatymui iš naujo sukalibruota nulinio amžiaus pagrindinė seka Vilniaus fotometrinėje sistemoje. Ištirti du padrikieji žvaigždžių spiečiai esantys Šiaurės Amerikos ūko kryptimi ir patikrintas jų ryšys su aplinkine žvaigždėdaros sritimi. Aptikta apie 30 jaunų emisinių žvaigždžių ir 4 ar 5 žvaigždės, kurios galėtų būti ūkų jonizacijos šaltiniai. / A Milky Way region in the direction of the North America and Pelican Nebulae is investigated using CCD photometry of 2600 stars in the Vilnius seven-color system. Its central part was covered with a CCD camera on the Maksutov wide-field telescope of the Moletai Observatory. Deeper CCD exposures for most interesting selected targets were taken with the 1 m telescope of the USNO Flagstaff Station. The author developed a new method for CCD data processing trying to reduce systematic errors and to increase photometric accuracy. This allowed us to measure M67 stars with high precision and use it as a CCD standard region in all our subsequent observations. To investigate interstellar extinction law in the area we obtained spectra for 33 B-type stars with the 2.3 m telescope of Steward Observatory at Kitt Peak. We also used near-infrared 2MASS data and other data sources when they were available. From photometric results in the Vilnius system we determined two-dimensional spectral types, color excesses, interstellar extinctions and distances of ~1300 stars. For more accurate determination of open cluster ages we recalibrated the zero-age main sequence in absolute magnitude vs. color diagram of the Vilnius system. We also investigated the possible connection between two open clusters in the area and surrounding star-forming region. Young stellar objects and possible ionizing sources of the NAP gas clouds were identified.

Les naines brunes sont des astres incapables de déclencher et soutenir des réactions nucléaires dans leur cœur. En l’absence de cette source d’énergie, leur luminosité diminue avec le temps jusqu’à leur extinction complète. Leur flux aux longueurs d’onde de 0,8 à 2,35 μm est particulièrement altéré par l’humidité contenue dans l’atmosphère terrestre, ce qui complique l’étude de ces astres. Le but de la présente recherche est de vérifier si la division par un spectre d’étoile A0 est un moyen de corriger l’altération causée par l’atmosphère terrestre sur cette partie de leur spectre. Tout d’abord, des notions, pertinentes à la compréhension de ce travail, sont abordées. L’introduction présente quelques notions sur les naines brunes et sur l’atmosphère terrestre. Le deuxième chapitre concerne le traitement des données. Il traite de la calibration, de la mise en évidence du problème de non-répétabilité de la position de la fente du spectromètre SIMON ainsi que de ses causes. Il porte aussi sur l’uniformisation de la réponse des pixels et de la soustraction du ciel pour extraire les spectres. La méthode employée pour étudier l’effet de l’atmosphère terrestre sur les spectres de naines brunes y est présentée. Le troisième chapitre analyse les résultats obtenus par l’utilisation de l’étoile de référence de type A0 comme calibration pour corriger le spectre de naine brune, en assumant un même effet de l’atmosphère terrestre sur les deux types d’astres. Nous ne pouvons conclure, avec certitude, que l’absorption tellurique affecte de la même façon les deux spectres ni de quelle façon exactement ils sont affectés. Une recherche supplémentaire nécessitant de nouvelles prises de données à des masses d’air et à des taux d’humidité variés est requise. / Brown dwarfs are celestial bodies unable to sustain nuclear reactions. For this reason their luminosity declines until complete extinction. Their flux, particularly in the band between 0,8 and 2,35 μm, is absorbed by the water vapor in the terrestrial atmosphere. The goal of this research is to find a way to correct this part of their spectra affected by this effect. First, general notions needed to understand the project are exposed. The second chapter concerns the data reduction. The calibration, the problem of the position repeatability of the slit of the spectrometer SIMON and his cause are exposed. It discusses techniques to even up the pixels’ response and the substraction of the sky from the spectra. The method used to study the atmosphere effect on brown dwarf spectra is presented. The third chapter analyses the results that use the A0 reference star to correct the brown dwarf spectrum. We cannot conclude that the A0 spectrum is affected in the same way as the brown dwarf spectrum by the terrestrial atmosphere. The data from a single night do not allow a good analysis of this effect as a function of air mass and humidity level. Others missions are needed.

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The gastrula stage represents the point in development at which the three primary germ layers diverge. At this point the gene regulatory networks that specify the germ layers are established and the genes that define the differentiated states of the tissues have begun to be activated. These networks have been well characterized in sea urchins, but not in other echinoderms. Embryos of the brittle star Ophiocoma wendtii share a number of developmental features with sea urchin embryos, including the ingression of mesenchyme cells that give rise to an embryonic skeleton. Notable differences are that no micromeres are formed during cleavage divisions and no pigment cells are formed during development to the pluteus larva stage. More subtle changes in timing of developmental events also occur. To explore the molecular basis for the similarities and differences between these two echinoderms, the gastrula transcriptome of Ophiocoma wendtii was sequenced and characterized. I identified brittle star transcripts that correspond to 3385 genes in existing databases, including 1863 genes shared with the sea urchin Strongylocentrotus purpuratus gastrula transcriptome. I have characterized the functional classes of genes present in the transcriptome and compared them to those found in sea urchin. I then examined which members of the germ-layer specific gene regulatory networks (GRNs) of S. purpuratus are expressed in the O. wendtii gastrula. The results indicate that there is a shared "genetic toolkit" central to the echinoderm gastrula, a key stage in embryonic development, though there are also differences that reflect changes in developmental processes. The brittle star expresses genes representing all functional classes at the gastrula stage. Brittle stars and sea urchins have comparable numbers of each class of genes, and share many of the genes expressed at gastrula. Examination of the brittle star genes whose sea urchin orthologs are utilized in germ layer specification reveals a relatively higher level of conservation of key regulatory components compared to the overall transcriptome. I also identify genes that were either lost or whose temporal expression has diverged from that of sea urchins. Overall, the data suggest that embryonic skeleton formation in sea urchins and brittle stars represents convergent evolution by independent cooptation of a shared pathway utilized in adult skeleton formation. Transcription factors are of central importance to both development and evolution. Patterns of their expression and interactions form the gene regulatory networks which control the building of the embryonic body. Alterations in these patterns can result in the construction of altered bodies. To help increase understanding of this process, I compared the transcription factor mRNAs present in early gastrula-stage embryos of the brittle star Ophiocoma wendtii to those found in two species of sea urchins and a starfish. Brittle star homologs were found for one third of the transcription factors in the sea urchin genome and half of those that are expressed at equivalent developmental stages in sea urchins and starfish. Overall, the patterns of transcription factors found and not found in brittle star resemble those of other echinoderms, with the differences largely consistent with morphological differences. This study provides further evidence for the existence of deeply conserved developmental genetic processes, with various elements shared among echinoderms, deuterostomes, and metazoans.

Polarized deep inelastic scattering experiments play a vital role in the exploration of the spin structure of the proton. The polarized proton-proton collider at RHIC provides direct access to the gluon spin distribution through longitudinal double spin asymmetry measurements of inclusive jets, pions, and dijets. This thesis presents the measurement of the dijet double differential cross-section in proton-proton collisions at center of mass energies of √s = 500 GeV. The data represent an integrated luminosity of 8.7 pb-1 recorded by the STAR detector during the 2009 RHIC run. A comprehensive jet analysis was performed to determine the ideal jet algorithm and jet parameters used in √s = 500 GeV collisions at the STAR detector. The cross-section is measured as a function of the dijet invariant mass (30 ≤ Mij ≤ 152 GeV) in the mid rapidity region with a maximum rapidity range of |ymax| ≤ 0.8. This result shows agreement with theoretical next-to-leading order pQCD calculations, motivating the use of dijet asymmetries at STAR to further constrain the shape of Δg(x).

microRNAs (miRNAs) are small (20-23 nt), non-coding single stranded RNA molecules that play an important role in post-transcriptional regulation of protein-coding genes. miRNAs have been found in all animal lineages, and have been implicated as critical regulators during development in multiple species. The echinoderms, Strongylocentrotus purpuratus (sea urchin) and Patiria miniata (sea star) are excellent model organisms for studying development due to their well-characterized transcriptional gene networks, ease of working with their embryos in the laboratory and phylogenetic position as invertebrate deuterostomes. Literature on miRNAs in echinoderm embryogenesis is limited. It has been shown that RNAi genes are developmentally expressed and regulated in sea urchin embryos, but no study in the sea urchin has examined the expression of miRNAs. The goal of my work has been to study miRNA regulation in echinoderm developmental gene networks. I have identified developmentally regulated miRNAs in sea urchin and sea star embryos, using a combination of computational and wet lab experimental techniques. I developed a probabilistic model (named HHMMiR) based on hierarchical hidden Markov models (HHMMs) to classify genomic hairpins into miRNA precursors and random stem-loop structures. I then extended this model to make an efficient decoder by introduction of explicit state duration densities. We used the Illumina Genome Analyzer to sequence small RNA libraries in mixed stage population of embryos from one to three days after fertilization of S. purpuratus and P. miniata. We developed a computational pipeline for analysis of these miRNAseq data to reveal the miRNA populations in both species, and study their differential expression. We also used northern blots and whole mount in situ hybridization experimental techniques to study the temporal and spatial expression patterns of some of these miRNAs in sea urchin embryos. By knocking down the major components of the miRNA biogenesis pathway, we studied the global effects of miRNAs on embryo morphology and differentiation genes. The biogenesis genes selected for this purpose are the RNAse III enzyme, Dicer and Argonaute. Dicer is necessary for the processing of mature miRNAs from hairpin structures while Ago is a necessary part of the RISC (RNA interference silencing complex) assembly, which is required for the miRNA to hybridize to its target mRNA site. Knocking down these genes hinders normal development of the sea urchin embryo and leads to loss of the larval skeleton, a novel phenotype not seen in sea stars, as well as abnormal gastrulation. Comparison of differentiation gene marker expression between control and Ago knocked down sea urchin embryos shows interesting patterns of expansion and suppression of adjoining some embryonic territories, while ingression of larval skeletogenesis progenitors does not occur.

This study consisted of an optical photometric and spectroscopic analysis on a 7′ 7′ field around the Southern high mass star forming region RCW 34. A previous study on RCW 34 in the NIR discov- ered many deeply embedded young stellar objects which were suspected to be T Tauri stars and which justified further investigation. The data used in this study consisted of three sets, the first two are photometric and spectroscopic data sets which were obtained during the first two weeks of February 2002. A third data set of spectroscopic observations was obtained by the author during the second week of 2011 of selected candidates using results from the NIR study and from the photometric data sets. All of the spectroscopy was conducted with the long slit spectrograph on the 1.9-m telescope and the photometry with DANDICAM on the 1.0-m telescope at the South African Astronomical Observatory (SAAO) in Sutherland. Objectives accomplished in the course of this study were to understand, ob- tain, reduce and interpret photometric and long slit spectroscopic CCD images. From the photometric results 57 stars showed excess blue emission on a colour-colour diagram which could be generated by circumstellar matter. The spectroscopic study showed 5 stars that showed H emission and 2 with strong Li absorption lines which confirm the suspicions of the NIR study about T Tauri stars in the region. All of the stars from the spectroscopic study in 2011 were identified as low-mass K or M type stars. Using colour-magnitude diagrams it was possible to see that the majority of the stars in the cluster are low-mass pre-main sequence stars. The stars matching between the optical and NIR filters were plotted on NIR colour-colour diagrams showing that the 5 stars that had H emission lines also had NIR colours characteristic to T Tauri stars. Out of the 5 stars that showed H emission, 2 were found to be classical T Tauris and three were found to be weak line T Tauris. / Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013