ABSTRACT Medieval xenophobia fostered attitudes that viewed anything foreign or distasteful as monstrous. Accordingly, insular inhabitants of the Middle Ages were constantly striving to distinguish Self from Other. My dissertation argues that sixteenth-century England began to reverse this trend: it began to reconcile difference, not by distinguishing Self from Other, but by blurring those distinctions. Visions of ancient Self and contemporary Other began to fuse as proponents of Imperial Britain sought to assimilate foreign monsters that were once considered barbaric, inferior, or inhuman. This method of assimilation is especially apparent during the Elizabethan Age of conquest in the New World. England's prophetic destiny was inextricably tied to its epic history, its Trojan ancestry, and its most glorified rulers, Brutus and his distant successor, King Arthur. Thus, reestablishing and rewriting Britain's legendary past became an exercise in securing its future. I maintain that John Dee (c. 1527-1608/9) and Edmund Spenser (c. 1552-1599) strategically fused ancient Britain and the New World via the figures of King Arthur and his alleged descendant, Queen Elizabeth. Portions of Dee's Brytanici Imperii Limites are explored to illustrate this connection, as are some of his arcane mystical pursuits. I further examine sections of Spenser's Faerie Queene in relation to Queen Elizabeth and King Arthur, and interpret Arthur in Faery lond as a metaphor for England in the New World. My introduction establishes the key features of the Galfridian tradition and its significance to the Tudor dynasty. It further discusses medieval perceptions of the monstrous that influenced the early-modern era. Subsequent chapters argue that England's assimilation of Other extended to pagan deities and giants, Native Americans, ancient Israelites, and (in Elizabeth's case) to the feminine Other. My final chapter demonstrates how Queen Elizabeth, via her affiliation with King Arthur, became a temporal bridge uniting England's epic past with its future glory.

Made available in DSpace on 2014-12-17T15:13:41Z (GMT). No. of bitstreams: 1 SauloCM.pdf: 959868 bytes, checksum: 64b02736330e52023dcc97349273dfec (MD5) Previous issue date: 2007-10-22 / Coordena??o de Aperfei?oamento de Pessoal de N?vel Superior / In the past 50 years, large efforts have been made toward the understanding of the stellar evolution. In the observational context, large sets of precise measurements of projected rotational velocity were produced, in particular by the Natal and Geneva groups. From these data, it is now possible to establish the behavior of stellar rotation from the turnoff to the red giant branch. In addition, these data have shown the role of tidal effects on stellar rotation in close binary systems. Nevertheless, relatively little attention has been paid to theoretical studies on the evolution of rotation along the HR Diagram, a topic itself directly associated to the evolution of the stars. Basically, there are two reasons for such a fact, (i) spherical symmetry is not assumed, what leads to a substantial increase in the numerical complexity of equations and (ii) non rotating models have been very successful in explaining relevant observational data, including the mass-luminosity relation and chemical abundances. In spite of these facts, it is clear that considerable work remains to be done on the role of rotation in the later stages of the evolution, where clear disagreements arise from confrontations between theoretical predictions and observations. In the present work we study the evolutionary behavior of stellar rotation along the HR Diagram, taking into account constraint conditions issued from recent observational survey of rotational velocity carried out with high precision procedures and new evolutionary codes / Nos ?ltimos cinq?enta anos, grandes esfor?os foram feitos no intuito de se entender a evolu??o estelar. No contexto observacional, medidas precisas da velocidade rotacional projetada foram produzidas, em particular, pelos grupos de Natal e Genebra. Destes dados ? poss?vel no presente momento estabelecer o comportamento da rota??o estelar do turnoff at? o ramo das gigantes vermelhas. Em adicional, estes dados t?m mostrado o papel dos efeitos de mar?s na rota??o estelar em sistemas bin?rios pr?ximos. Mesmo tendo sido feitos bons avan?os c no ambito observacional, pouca aten?? tem sido dada a estudos te?ricos da evolu??o da rota??o ao longo do diagrama HR, um t?pico que est? intimamente ligado a evolu??o das estrelas. Basicamente, existem dois motivos para tal fato,(i) a n?o suposi??o de simetria esf?rica leva a um aumento substancial da complexidade num?rica das equa??es, e (ii) os modelos sem rota??o t?m tido bastante sucesso na explica??o de relevantes dados observacionais, incluindo as rela??es entre massa e luminosidade e abund?ncias qu?micas. Diante do avan?o do estudo da rota??o, ainda restam trabalhos a serem feitos sobre o seu papel em est?gios mais tardios da evolu??o, uma vez que existem discord?ncias entre predi??es te?ricas e observacionais. No presente trabalho, n?s estudamos o comportamento evolucion?rio da rota??o ao longo do diagrama HR, levando em conta condi??es de contorno baseadas em recentes medidas de velocidade rotacional obtidas a partir de procedimentos de alta precis?o e novos c?digos evolutivos

Surface brightness asymmetries are a very common feature of stars. Among other effects they cause a difference between the projected centre of mass and the photocentre. The evolution of those surface features makes this difference time-dependent. In some cases the displacement can be a non-negligible fraction of the star radius R, and if R>1 AU, of the parallax. We investigate the impact of surface brightness asymmetries on the Gaia astrometric solution and on the data processing flow. In particular we derive analytical expressions for the change in the derived astrometric parameters for a single-star, with respect to the parameters for a uniformly-bright star, as a function of the characteristics of the surface brightness asymmetries. These predictions are confirmed by the results of the processing of simulated astrometric Gaia data where a photocentre motion caused by surface brightness asymmetries has been added using a Gaussian Markovian model.<p>In the case of a red supergiant star, the average photocentre shift is about 0.1 AU. Such a photocentric noise translates in a 10% inaccuracy on the parallax (independently of the distance), which becomes larger than the statistical error on the parallax derived from the data reduction for stars that are up to about 4 kpc away. For the most nearby stars, we derive an inaccuracy on the parallax that can be 10 times its statistical error. Finally we estimate that up to about 4000 stars among red supergiants and bright giants may have astrometric parameters that are inaccurate at levels bigger than expected because of the surface brightness asymmetries. In the determination of this number, a crucial role is played by the Gaia observable magnitude range. The fact that Gaia will not observe stars brighter than 5.6 in the Gaia G band means that the closest stars will not be observed. Yet, the impact of the surface brightness asymmetries is proportional to their angular size, meaning that the stars whose astrometric accuracy would be most affected are not observed.<p>Various non-Gaussian spot models (as applicable in the case of magnetic spots) have been implemented and analytical predictions for the effects of such magnetic spots are computed for the most representative classes of magnetic stars.<p>Another effect of the presence of surface brightness asymmetries is their impact on Gaia data processing flow. The quality of the fit of the data is evaluated with the F2 parameter that is a transformation of χ2 such that it has a unit normal distribution when the model is adequate and it is independent of the number of measurements. If the goodness-of-fit F2 of the single-star solution is not good enough (F2>3), a chain of solution of growing complexity is tried until a satisfactory one (with F2<3) is obtained. If no good solution is found, a so-called stochastic solution is computed where a "cosmic" error is added to the data in order to obtain a single-star solution with F2=0. We show that the photocentre noise induces an increase in the goodness-of-fit parameter, causing this chain of solutions to be entered. Depending on the characteristics of the photocentre noise, a variable fraction of the stars in our simulations end up with a non-single-star solution. Yet, we show that these (orbital) solutions are not acceptable because non-significant or non-physical. Finally, an important fraction of stars is assigned a stochastic solution with a cosmic noise matching well the photocentric noise.<p><p>/<p><p>Les asymétries de brillance de surface sont une caractéristique commune des étoiles. Parmi d'autres effets, elles provoquent une différence entre la projection du centre de masse et le photocentre. L'évolution de ces structures de surface rend cette différence variable avec le temps. Dans certains cas, le déplacement du photocentre peut être une fraction non négligeable du rayon de l'étoile R et, si R>1 UA, de la parallaxe. Nous examinons l'impact des asymétries de brillance de surface sur la solution astrométrique de Gaia et sur le processus de traitement des données. En particulier nous dérivons des expressions analytiques pour le changement des paramètres astrométriques déerivées pour une étoile simple, par rapport aux paramètres pour une étoile uniformément lumineuse, en fonction des caractéristiques des asymétries de brillance de surface. Ces prévisions sont confirmées par les résultats de simulations du traitement des données astrométriques de Gaia, auxquelles des mouvements du photocentre causés par des asymétries de brillance de surface ont été ajoutés en utilisant un modèle gaussien markovien.<p><p>Dans le cas d'une étoile super-géante rouge, le décalage moyen du photocentre est d'environ 0.1 UA. Un bruit photocentrique de cette amplitude se traduit dans une imprécision de 10% sur la parallaxe (indépendamment de la distance), qui peut devenir plus grande que l'erreur statistique sur la parallaxe déerivée par la réduction des données, pour les étoiles plus proches d'environ 4 kpc. Pour les étoiles les plus proches, nous évaluons une imprécision sur la parallaxe qui peut être 10 fois leur erreur statistique. Finalement, nous estimons que jusqu'à environ 4000 étoiles parmi les super-géantes rouges et géantes brillantes peuvent avoir des paramètres astrométriques inexactes à des niveaux plus grands que prévu en raison des asymétries de brillance de surface. Dans la détermination de ce nombre, la gamme de magnitudes observables par Gaia joue un rôle crucial. Le fait que Gaia n'observera pas les étoiles plus brillantes que 5.6 mag (en bande Gaia) signifie que les étoiles les plus proches ne seront pas observées. Pourtant, l'impact des asymétries de brillance de surface est proportionnel à leur taille angulaire, ce qui signifie que les étoiles dont la précision astrométrique seraient la plus affecté ne seront pas observées.<p>Différents modèles de taches ont été réalisés et des prédictions analytiques pour les effets de ces taches magnétiques sont calculés pour les classes les plus représentatives des étoiles magnétiques. <p>Un autre effet de la présence des asymétries de brillance de surface est leur impact sur le traitement des données de Gaia. La qualité de l'ajustement des données est évaluée avec le paramètre F2 qui est une transformation de χ2 telle qu'il ait une distribution normale lorsque le modèle est adéquat. Si la qualité de l'ajustement F2 de la solution étoile-simple n'est pas acceptable (F2>3), une chaîne de solutions de complexité croissante est essayée jusqu'à ce qu'une solution satisfaisante (avec F2<3) soit obtenue. Si aucune solution satisfaisante n'est trouvée, une solution dite stochastique est calculée où une erreur "cosmique" est ajoutée aux données afin d'obtenir une solution étoile-simple avec F2=0. Nous montrons que le bruit du photocentre induit une augmentation de F2, ce qui provoque l'activation de cette chaîne de solutions. Selon les caractéristiques du bruit du photocentre, une solution étoile-non-simple est obtenue pour une fraction variable des étoiles dans nos simulations. Nous montrons que ces solutions (orbitales) ainsi obtenues ne sont pas acceptables car non significatives ou non-physiques. Enfin, une fraction importante d'étoiles se voient attribuer une solution stochastique avec un bruit cosmique correspondant au bruit photocentrique. / Doctorat en Sciences / info:eu-repo/semantics/nonPublished

Abstract The subject of this study is ancient stone structures found in Middle and Northern Ostrobothnia. Their shape, distribution, topography and relation to the ancient shorelines of different ages are the main themes of the research. The sites are classified into different categories according to those attributes. The function and the cultural context of the stone structures are also discussed in the study. The dating of the stone structures is based solely on shoreline chronology. A model is proposed for the of social organization of Stone Age and Early Metal Age hunter-gatherer societies in Ostrobothnia. Spatial data relating to the sites was gathered both from the field and archives. The data is discussed on two levels. The cairns, dwelling sites and Giants' Churches have been studied in the larger Ostrobothnian study area. Other stone structures i.e. dwelling depressions in stone field, pits with walls and pits in stone fields, were studied in two limited research areas in Middle and Northern Ostrobothnia. The research database contains location and attribute data from 444 cairn sites with altogether 1133 cairns. There is also data from 34 Giants' Churches and 1191 other archaeological remains. The relations between the sites and ancient shorelines were analysed with GIS applications and digital elevation models. The hypothesis is put forward that the first cairn building tradition originated in the study area by 3000-2500 cal BC. This Stone Age cairn tradition is related to the middle Neolithic "Giants? Church culture". This Cairn building tradition continued most likely without chronological gaps and gave rise to the Early Metal Age cairn tradition. The large number of cairns at the 2500 cal BC shoreline zone is clearly connected to its higher number of dwelling depressions. The explanation for the increasing number of dwelling depressions and dwelling planes of the period around 3000 and 2500 cal BC is the growth of population. Giants? Churches and cairns appear around the same time. These new features and changes in the archaeological record reflect developments which took place within the hunter-gatherer societies of Ostrobothnia. This development led to more complex social structures. / Tiivistelmä Tutkimukseni aiheena ovat Keski- ja Pohjois-Pohjanmaan rannikon esihistorialliset kiinteiksi muinaisjäännöksiksi luokiteltavat kivirakennelmat. Kohteissa olevien rakennelmien muoto, sijoittuminen ympäristöön ja suhde eri muinaisrantapintoihin ovat työn keskeisiä teemoja. Kohteita ryhmitellään rakennelmien muodon, kombinaation ja topografisten piirteiden perusteella. Tarkastelussa ovat sekä rakennelmien käyttötarkoitus että kulttuurinen konteksti. Röykkiöiden ja kivirakennelmien ajoitusta hahmotellaan rannansiirtymiskronologialla. Lisäksi tutkimuksessa esitetään tulkinta tutkimusalueen kivikauden ja varhaismetallikauden yhteisöjen sosiaalisesta rakenteesta. Kohteiden paikkatiedot on koottu sekä maastokäynneillä että arkistolähteistä. Kerätyn aineiston tarkastelu tapahtuu kahdella tasolla. Röykkiöitä, asuinpaikkoja ja jätinkirkkoja tarkastellaan laajan osan Pohjanmaata kattavalla tutkimusalueella. Toinen taso on maantieteellisesti suppeampi, mutta aineistoltaan laajempi. Siinä tarkastellaan kaikkia kivirakennelmatyyppejä kahdella rajatulla tutkimusalueella Keski- ja Pohjois-Pohjanmaalla. Pohjanmaan tutkimusalueen aineisto koostuu 444:stä röykkiökohteesta, joissa on yhteensä 1133 röykkiötä. Tämän lisäksi tutkimusta varten kerättiin sijainti- ja ominaisuustiedot 34:stä jätinkirkosta ja 1191:stä muusta kiinteästä muinaisjäännöksestä. Aineiston topografisessa analyysissä tarkastellaan röykkiökohteiden sijaintikorkeutta ja sijoittumista eri muinaisrantavyöhykkeille. Kohteiden suhdetta toisiinsa ja muihin muinaisjäännöskohteisiin käsitellään lähimpään naapuruuteen perustuvassa analyysissä. Lisäksi kohteiden hierarkiaa selvitetään arvo-koko-analyysillä. Muinaisjäännöskohteiden tarkasteleminen suhteessa eri muinaisrantoihin toteutettiin GIS-paikkatietosovelluksen ja korjatun yleistetyn korkeusmallin avulla hahmottelemalla yhdeksän muinaista rantavyöhykettä. Oletuksena on, että vyöhykkeillä sijaitsevat kohteet ovat olleet merenrantasidonnaisia. Röykkiöiden rakentaminen Pohjanmaalla alkaa noin 3000-2500 eKr., ja traditio liittyy keskineoliittiseen "jättiläiskirkkokulttuuriin", kuten Aarne Europaeus vuonna 1925 kirjoittamassaan artikkelissa otaksui. Röykkiöiden määrän nousu kivikauden muinaisrantavyöhykkeillä näyttäisi liittyvän asumuspainanteiden, asuinpaikkapintojen ja jätinkirkkojen määrän nousuun. Kehityksen taustalla on rannikon metsästäjä-keräilijä-yhteisöjen sosiaalisten rakenteiden muutos. Kivikauden loppu ja varhaismetallikausi merkitsevät muutosta kohti yksinkertaisempia sosiaalisia rakenteita. Röykkiöiden rakentamisen perinne jatkui Pohjanmaalla kivikaudelta varhaismetallikaudelle, mutta rakentamisen takana ollut ideologia muuttui. Röykkiöiden määrä nousee yhdessä keittokuoppien määrän kanssa rautakauden alussa 500 eKr. tienoilla uudestaan. Mutta huippukausi jää lyhyeksi, sillä röykkiökohteiden ja muidenkin muinaisjäännösten määrät laskevat tämän jälkeen nopeasti ja lopullisesti.

Wetlands within South Africa are an important source of water and nutrients necessary for biological productivity and often the survival of the local people. In a country where the rural communities depend on wetlands for their day to day provision of water, food and materials it has become necessary to understand the functions within wetland systems, so that proper conservation measures can be applied in order to protect and ensure the sustainable use of wetlands. Due to the fact that South Africa has a semi arid climate, thereby affecting the availability of water it is sensible that studies are under-taken in which, more is explored about the water resources, the protection as well as the sustainable use of the wetlands within the region. Despite the fact that the total area which wetlands cover in South Africa is relatively small, the functions which they provide is of fundamental magnitude not only to wildlife but also as an essential part of the human life support system. Wetlands have the ability to regulate regional flow regimes and are often situated in areas of impeded drainage, which may contribute to the regulation of water. It is thus plausible that if headwater/palustrine wetlands are destroyed, many of the streams and rivers which under normal circumstance are perennial, would not only become non- perennial but the consequence of a drought would be far more severe, as well as increasing the risk in flood damage further down the river. In Giants Castle Game Reserve, situated in the KwaZulu-Natal Drakensberg, several palustrine wetlands where studied to identify the geomorphic attributes which contribute to the origin and maintenance of these wetlands. An added motive for the study was the fact that, according to Ramsar, one of the reasons for conserving the Drakensberg wetlands is to ensure the maintenance and production of water quality to KwaZulu-Natal. Seven wetlands within the Boesmans river upper catchment were identified and studied. Soil investigations were undertaken in an effort to determine the driving forces behind the origin and maintenance, as well as to improve the understanding relating to the functioning of the wetlands. The geomorphic attributes which were identified as being important to the genesis and maintenance of wetlands were found to be the following: low relief, soil piping within wetlands, sediment trapping ability of wetlands, the surface roughness of wetlands, channeling within wetlands, organic matter accumulation as well as geological barriers within wetland system. The adaptability of Longmore’s (2001) Hydro-Geomorphic classification to different catchment areas was also tested and was found suitable for these wetlands, although the influence of piping on wetlands evidently requires further investigation and incorporation into classifications. / Dissertation (MA)--University of Pretoria, 2006. / Geography, Geoinformatics and Meteorology / MA / Unrestricted

We have observed our Universe in many different wavelengths, from gamma ray to radiowaves and have observed countless stars, galaxies, and everything else in between. These measurements slowly add to our understanding of what our Universe is, how it formed, and where it is heading next. In Chapter 2 we introduce the Ultraviolet GAlactic Plane Survey (UVGAPS), which produced a high resolution map of the Milky Way’s Galactic plane in the NUV using the Galaxy Evolution Explorer (GALEX), an orbiting ultraviolet space telescope operated by NASA and Caltech between 2003-2013. Of the many astrophysical phenomena observable in ultraviolet wavelengths, we choose to focus on a few interesting objects: red clump stars and OB type stars, and the Galactic dust that impacts them. We use an image source extractor to obtain the NUV photometry and apply several cuts to clean the data. We present a catalog of 2,843,399 objects with GALEX NUV band mea- surements. Despite the difference in observing strategy and analysis pipeline, we find good agreement between previously targeted GALEX observations and the UVGAPS catalog in overlapping regions. The data were cross matched to Gaia DR2 and Pan-STARRS DR2, two visible-band surveys that have considerable coverage of the Galactic Plane. We characterize matched objects in color-magnitude and color-color space to highlight a range of objects, from main sequence stars to binaries detected with these data. Although core helium-burning red clump (RC) stars are faint at ultraviolet wavelengths, their ultraviolet-optical color is a unique and accessible probe of their physical properties. In Chapter 3, using data from the GALEX All Sky Imaging Survey, Gaia DR2, and the SDSS APOGEE DR14 survey, we find that spectroscopic metallicity is strongly correlated with the location of a RC star in the UV-optical color magnitude diagram. The RC has a wide spread in (NUV - G)0 color of over 4 magnitudes compared to a 0.7-magnitude range in (G BP - G RP )0 . We propose a photometric, dust-corrected, ultraviolet-optical (NUV - G)0 - [Fe/H] color-metallicity relation using a sample of 5,175 RC stars from APOGEE. We show that this relation has a scatter of 0.16 dex and is easier to obtain for large, wide-field samples than spectroscopic metallicities. Importantly, the effect may be comparable to the spread in RC color attributed to extinction in other studies. In Chapter 4 we extend our RC analysis to UVGAPS and include new age and mass measurements. We find that RC stars separate into two distinct populations in the thin and thick disk. Thick disk stars tend to be old, low mass stars while thin disk stars are more heterogeneous, containing mostly young, massive stars but also some old, low-mass stars typical of the thick disk. These last two chapters are just two of many projects that UVGAPS enables.

No description available.

The aim of this diploma thesis is a comparative analysis of the image of a forsaken child in the stories written by a popular English writer Neil Gaiman. The survey of a forsaken child in the Gothic, Romantic and Victorian literature (Walpole, Radcliffe, Blake, Dickens, the Brontë sisters) precedes the interpretation. In addition, this diploma thesis considers the separation of the young hero from his family and friends in traditional fairy tales. In this respect, the thesis discusses the role of transitional rituals and their links to the theme of the test in adventurous literature (Gennep, Bachtin). The first, theoretical chapters point out the fact that the transition to a new existence (adulthood) is often accompanied by horror elements or the nearness of death in the adventurous stories. The novel Coraline is a basis for the literary analysis. The psychological characteristic of the main heroine and her family is linked to the function of home and the role of "the other mother" as a source of the Gothic atmosphere and danger. The following chapters analyse other Gaiman's works ("M is for Magic", The Graveyard Book, Odd and the Frost Giants, Fortunately, the Milk, The Ocean at the End of the Zone) in order to study the relations between the reality and dreams, violence and interpersonal relationships, and to describe the heroes' search for the individual identity.

Den här uppsatsen undersöker på sociologiskt vis möjligheterna att spåra möten mellan tidigamänniskor och jätteprimaten Gigantopithecus från östra Asien i myter som överlevt fram till idag,detta för att försöka peka på ett gemensamt ursprung till den ofta förekommande figurtypen jätten imyter och folksagor i världen. Teoretikerna som uppbådas till hjälp är Emile Durkheim, MartinCortazzi, Josef Ludvik Fisher samt Forrester Sibelan, vilka visar på dels hur myter fungerar och kanuppstå och hur de fungerar i relation till människor.Till metod har arbetet utgått ifrån diskursteori då denna lämpar sig väl för att förstå relationenmellan den sociala verklighet en text rör sig inom och den text sagda verklighet bidrar till att skapa.Arbetet börjar med att försöka motivera sin hypotes genom att påvisa dels belägg för att primatenoch människan i urtiden mötts och dels genom att visa på att myter och berättelser i muntlig formkan överleva länge nog för att det ska vara rimligt. Den fortsätter med att presentera och beskrivamytbildningar från olika delar av världen; Nordiska, Grekiska, Babyloniska, Indiska Afrikanska,Nord- och Sydamerikanska samt Kinesiska där fokus ligger på att jämföra och sammanföra myterför att försöka peka på samband som andra forskare redan upptäckt eller sådana som pekar mot denöstasiatiska primaten.Det visar sig snabbt att några sådana belägg inte finns att finna under de förhållanden den härundersökningen utgår ifrån när den går in på ämnet. Istället försöker den fokusera på att visa på debevisliga ursprungen från de jätterelaterade myter som i världen förekommer. Till stor del härrör de,enligt forskarna uppsatsen använder som källor, från Mesopotamien och rent sociologiskt så kanuppsatsen peka på ett samband mellan ett behov av politisk kontroll och den roll jättar i mytbildningbrukar få. Platser som Grekland, Inkariket och Kina har oberoende av varandra utvecklat deursprungliga mytbildningarna på ett sätt som underbygger auktoritära figurer både inom och utanförmyterna så att berättelserna passar den grupp som styr området, något som i viss utsträckning gällerför alla mytbildningar som undersöktes. Jättarna får ofta roller såsom förfäder eller fientliga folksom människor och deras gudar obrydda kan avsky eller diskreditera. Genomgående så stämmer dei teoridelen presenterade forskarnas teorier med det sätt som myterna som undersöks visas fungerapå. / This paper tries to explore the sociological possibilities of finding a link between interactionsbetween the giant primate Gigantopithecus and early humans of eastern Asia and surviving mythsfrom around the world that have survived up until today. Theorists that have been drafted to attemptto prove this are Emile Durkheim, Martin Cortazzi, Josef Ludvik Fischer and Forrester Sibelan,who's work revolve around the area of the inner workings of myth and its relation to the peoplesustaining them.As Method the paper operates on the basis of discourse theory as it is well suited to explain theways in which reality and text co-opt in the creation of the other.To begin with the paper puts out hypothesis strengthening research to try to show ways that theprimate in theory could have acted as a forefather to the giant, due to prehistoric humans havinginteracted with Gigantopithecus and the way oral myth is able to survive for very long stretches oftime. It continues by presenting and describing various myths from around the world; Nordic,Greek, Babylonian, Indian, African, North and South American as well as Chinese. The focus lieson showing the many themes the myths share between themselves, with an initial focus on pinningits origins to Gigantopithecus.Early on any such connections prove to be without credible proof, and as it is the paper is illequipped to attempt to claim any connections between the myths and the primate. To stay relevant,the paper tries to present other more substantiated potential origins of the concept of giants andfinds other researchers pointing towards old Mesopotamia. Sociologically however the paper canpoint towards connections between political control and the role of the giants of myths in the storiesof many of the stories it presents. Places such as Greece, the Inca empire and China all, apparentlyindependently of one another created and developed myths wherein giants assist in reinforcing theauthoritarian positions of leader characters both within and outside of the stories. Giants in mythoften played the role of ancient ancestors or non human or non tribe people that gods and peoplebereft of conscience could paint as enemies or buffoons.

The KwaZulu-Natal Drakensberg, South Africa, is predominantly a grassland ecosystem maintained by fire. The effect of the current burning regime on invertebrate and flowering forb diversity in this ecosystem is poorly understood. The overall aim ofthis study was to contribute towards the development of an effective burning regime for the KwaZulu-Natal Drakensberg that will conserve invertebrates and indigenous forbs, two major components of biodiversity. The objectives were to examine the effect of fire and fire frequency on flowering forb and invertebrate species diversity, to determine whether fire frequency, time since last burn or locality were influencing species composition, and to identify potential biodiversity indicators that reflect overall species richness for use in monitoring of invertebrates and forbs. Sampling took place in March, September and November of 2002 at Giants Castle Game Reserve. Invertebrates were sampled using sweep netting and targeted netting along transects, yellow pan traps and soil quadrats. Invertebrate taxa sampled were ants (Formicidae), butterflies (Lepidoptera), grasshoppers (Orthoptera), leafboppers (Cicadellidae), bees (Apoidea), bee flies (Bombyliidae), hover flies (Syrphidae), robber flies (Asilidae), spiders (Araneae), earthworms (Oligochaeta) and millipedes (Diploda). These were identified to species level with the assistance of taxon experts. Flowering forbs were sampled using five replicates of five by five metre quadrats randomly placed in each site. Overall flowering forb and invertebrate species diversity was higher in grasslands that were burnt for two consecutive years in 2001 and 2002 than in grasslands that were not burnt during those two years. Frequently (annual) and intermediately (biennial) burnt grasslands had significantly higher invertebrate and flowering forb diversity than infrequently (five years without burning) burnt grasslands. This, together with the fact that grasslands burnt during the year of sampling had higher species richness than grasslands burnt two and five years previously suggests that invertebrates and forbs are generally resilient to fire and many forb species appear to be stimulated by fire. However, each burn frequency had its own suite of unique flowering forb and invertebrate species. Invertebrate communities were influenced mostly by locality and the length of time past since the last fire and flowering forb communities were influenced mostly by the length oftime past since the last fire. Fire frequency had the least influence on both invertebrate and forb communities. Ecological succession occurred after each fire in the invertebrate communities but forb communities appear to need more than five years without fire for ecological succession to occur. The findings of this study therefore suggest that using a combination of three fire frequencies would result in patches of grassland in various stages of ecological succession, and would conserve species unique to each burning frequency, and would therefore conserve maximum diversity. Flowering forb species richness and certain invertebrate taxa (ants, leafboppers, spiders and bees) have the potential to act as indicators of overall invertebrate species richness for use in monitoring programmes. / Thesis (M.Sc.)-University of KwaZulu-Natal, Pietermaritzburg, 2006.