This thesis aims a critical reading of two American series also aired in Brazil: Star Trek and Heroes. The survey proposes to observe dissensus from the multitude present on both TV series. The multitude (HARDT; NEGRI, 2000) is a social force capable of challenging the sovereign power and to establish new forms of social organization, their presence may present dissensus (RANCIÈRE, 2010), new elements to what is conventionally considered and sense, the sensitive system already established. This movement is associated with materialistic conception of history that suggests seeking tensions against the dominant social order (BENJAMIN, 1987). The Star Trek series debuted in 1966 and its last episode was broadcast in 1969. The series was produced by Desilu Productions and broadcast by NBC, and your transmission took place at a time when American foreign policy has to tend less to an imperialist activity than to a policing action to a supranational order service. The hypothesis is that his narrative shows the will of the multitude to prevent the exercise of the former European sovereignty and to overcome the nationalist struggles. The Heroes series was produced in partnership by Tailwind Productions, NBC, Universal Television and Universal Media Studios. Four seasons were exhibited from 2006 to 2009. The series covers the history of characters who, because of genetic mutations, discover powers that make them special. Although they appear in different parts of the world, there is some force that, in many ways, remains interconnection between the characters. The hypothesis is that the special abilities of Heroes characters may be attached to faculties of the multitude able to oppose the order of global capitalism. The overall objective of this research is, as stated initially, to look for dissensus from multitude inside the series. It is possible to see that these cultural objects do not carry a single system of presentation attached to commercial logic, but let see, within their respective contexts of production, transformative capacities against the established order. It can be said that the tensions in the series denote trouble for tradition defended by the dominator, presenting challenging ways to read the story doing justice to the dominated. / Submitted by Carolini da Rocha (carolini.rocha@unisul.br) on 2017-05-09T12:50:52Z No. of bitstreams: 2 jeanrzhoullou.pdf: 2355014 bytes, checksum: 53c7c03bc132c6a3dc6fa6c11cf22807 (MD5) Jean Raphael Zimmermann Houllou.pdf: 770947 bytes, checksum: 818c2879f4b96ee04555885d98022d3e (MD5) / Approved for entry into archive by Carolini da Rocha (carolini.rocha@unisul.br) on 2017-05-09T12:52:32Z (GMT) No. of bitstreams: 2 jeanrzhoullou.pdf: 2355014 bytes, checksum: 53c7c03bc132c6a3dc6fa6c11cf22807 (MD5) Jean Raphael Zimmermann Houllou.pdf: 770947 bytes, checksum: 818c2879f4b96ee04555885d98022d3e (MD5) / Made available in DSpace on 2017-05-09T12:52:32Z (GMT). No. of bitstreams: 2 jeanrzhoullou.pdf: 2355014 bytes, checksum: 53c7c03bc132c6a3dc6fa6c11cf22807 (MD5) Jean Raphael Zimmermann Houllou.pdf: 770947 bytes, checksum: 818c2879f4b96ee04555885d98022d3e (MD5) Previous issue date: 2016 / A presente tese pretende uma leitura crítica de dois seriados norte-americanos, também veiculados no Brasil: Star Trek e Heroes. O exame propõe observar dissensos da multidão presentes em ambos os seriados de TV. A multidão (HARDT; NEGRI, 2000) é como uma força social capaz de desafiar o poder soberano e instituir novas formas de organização social; sua presença pode apresentar dissensos (RANCIÈRE, 2010), ou seja, novos elementos para aquilo que convencionalmente é considerado e sentido, o regime do sensível já estabelecido. Esse movimento se associa a concepção de história materialista que sugere a procura de tensões contra a ordem social dominante (BENJAMIN, 1987). O seriado Star Trek estreou em 1966 e seu último episódio foi transmitido em 1969. A série foi produzida pela Desilu Productions e exibida pela NBC, e sua transmissão se deu num momento em que a política externa americana passou a tender menos para uma atividade imperialista do que para uma ação de policiamento a serviço de uma ordem supranacional. A hipótese é a de que sua narrativa apresenta a vontade da multidão em impedir o exercício da antiga soberania europeia e em superar as lutas nacionalistas. O seriado Heroes foi produzido em parceria pela Tailwind Productions, NBC,Universal Television e Universal Media Studios. Foram exibidas quatro temporadas de 2006 a 2009. A série aborda a história de personagens que, em razão de mutações genéticas, se descobrem portadores de poderes que os tornam especiais. Embora apareçam em diferentes partes do mundo, existe alguma força que, de variadas formas, mantém os personagens interconectados. A hipótese em Heroes é a de que as habilidades especiais dos personagens podem ser associadas às faculdades da multidão capazes de se opor à ordem do capitalismo global. O objetivo geral desta pesquisa consiste, como afirmado inicialmente, em averiguar dissensos da multidão dentro dos seriados. É possível observar que estes objetos da cultura não carregam um regime único de apresentação ligado à lógica mercantil, mas permitem constatar, dentro de seus respectivos contextos de produção, capacidades transformadoras contra a ordem constituída. Pode-se afirmar que as tensões observadas nos seriados denotam problemas para a tradição defendida pelo dominador apresentando formas desafiadoras à leitura da história e fazendo justiça aos dominados.

White dwarf stars are the most common final stage of stellar evolution, corresponding to 99% of all stars in the Galaxy. White dwarf models can be used to obtain the age of stellar populations, to build an initial to final mass relation to understand the connection between the properties of white dwarfs and their progenitors, determine the upper mass limit that separates white dwarfs progenitors from Type II supernovae, enhance the comprehension of the physical properties of high density matter and derive ages and masses for observed white dwarfs from the cooling tracks. The literature is populated with low mass and intermediate mass white dwarf models, however the massive white dwarfs are often forgotten and the evolutionary sequences are incomplete. In this dissertation, we compute full evolutionary sequences for massive white dwarfs, exploring the evolution of hydrogen-rich and hydrogen-deficient white dwarfs stars with masses between 1.012 and 1.307 M , and initial metallicity of Z = 0.02. These sequences are the result of main sequence stars with masses between 8.8 and 11.8 M . The simulations were performed with the Modules for Experiments in Stellar Astrophysics - MESA code, starting at the zero-age main sequence, through thermally pulsing and mass-loss phases, ending as the white dwarfs at the cooling sequence. Our simulations are full evolutionary, in which we consider the entire evolutionary history of the progenitors. We present reliable nuclear chemical profiles for the whole mass range considered, covering the different expected central compositions, i.e. C/O, O/Ne and Ne/O/Mg, and their dependence with the stellar mass. In addition, we present detailed chemical profiles of hybrid C/O-O/Ne core white dwarfs, found in the mass range between 1.024 and 1.150 M . We present the initial-to-final mass relation, mass-radius relation, and cooling times with improved crystallization limits, considering the effects of atmosphere and core composition.

abstract: Green pea galaxies are a class of rare, compact starburst galaxies that have powerful optical emission line [OIII]$\lambda$5007. They are the best low-redshift analogs of high-redshift (z$>$2) Lyman-alpha emitting galaxies (LAEs). They provide unique opportunities to study physical conditions in high-redshift LAEs in great detail. In this dissertation, a few physical properties of green peas are investigated. The first study in the dissertation presents star formation rate (SFR) surface density, thermal pressure in HII regions, and a correlation between them for 17 green peas and 19 Lyman break analogs, which are nearby analogs of high-redshift Lyman break galaxies. This correlation is consistent with that found from the star-forming galaxies at z $\sim$ 2.5. In the second study, a new large sample of 835 green peas in the redshift range z = 0.011 -- 0.411 are assembled from Data Release 13 of the Sloan Digital Sky Survey (SDSS) with the equivalent width of the line [OIII]$\lambda$5007 $>$ 300\AA\ or the equivalent width of the line H$\beta$ $>$ 100\AA. The size of this new sample is ten times that of the original 80 star-forming green pea sample. With reliable T$_e$-based gas-phase metallicity measurements for the 835 green peas, a new empirical calibration of R23 (defined as ([OIII]$\lambda$$\lambda$4959,5007 + [OII]$\lambda$$\lambda$3726,3729)/H$\beta$) for strong line emitters is then derived. The double-value degeneracy of the metallicity is broken for galaxies with large ionization parameter (which manifests as log([OIII]$\lambda$$\lambda$4959,5007/[OII]$\lambda$$\lambda$3726,3729) $\geq$ 0.6). This calibration offers a good way to estimate metallicities for extreme emission-line galaxies and high-redshift LAEs. The third study presents stellar mass measurements and the stellar mass-metallicity relation of 828 green peas from the second study. The stellar mass covers 6 orders of magnitude in the range 10$^{5}$ -- 10$^{11}$ M$_{\odot}$, with a median value of 10$^{8.8}$ M$_{\odot}$. The stellar mass-metallicity relation of green peas is flatter and displays about 0.2 - 0.5 dex offset to lower metallicities in the range of stellar mass higher than 10$^{8}$ M$_{\odot}$ compared to the local SDSS star-forming galaxies. A significant dependence of the stellar mass-metallicity relation on star formation rate is not found in this work. / Dissertation/Thesis / Doctoral Dissertation Astrophysics 2018

Ma thèse est centrée sur l'étude de l'interaction entre les étoiles massives et le milieu environnant. Je suis particulièrement intéressé par l'effet qu'ont ces étoiles sur les jeunes objets stellaires observés autour d'elles. Les étoiles massives forment des régions d'hydrogène ionisé (HII) dont l'expansion supersonique conduit à la formation d'une couche de gaz et de poussières où les conditions paraissent favoriser la formation stellaire. Mon travail consiste à étudier les propriétés des jeunes objets stellaires autour de ces régions HII et à savoir si la région HII a influencé positivement la formation de ces sources.En utilisant les données Herschel, issues des programmes HOBYS et Hi-GAL, complétées par d'autres observations, j'ai étudié deux régions HII galactiques (RCW~79 et RCW~120) afin de caractériser la formation stellaire observée à leurs frontières. Pour étudier l'impact de la photoionisation, j'ai calculé le taux de formation stellaire (SFR) pour ces deux régions. Cette grandeur suggère que RCW~79 et RCW~120 sont des régions de formation stellaire actives malgré leur relative faible densité surfacique de gaz. Une nouvelle étude de la région G345 est en cours. Cette région HII est située au-dessus du plan galactique et forme activement des étoiles. Avec les données disponibles, les propriétés de la formation stellaire seront discutées. Cette étude nous donne l'opportunité de mieux comprendre les effets de la photoionisation en dehors du plan galactique. Cette région viendra augmenter notre échantillon de régions HII, ce qui est nécessaire pour avoir une vision globale des mécanismes en jeu et pour mieux comprendre l'efficacité de la formation stellaire. / My PhD thesis deals with the study of the interaction between high mass stars and their surrounding medium. I am particularly interested in the way high-mass stars affect the young stars observed around them. Massive stars form ionized (HII) regions which, during their supersonic expansion, lead to the formation of a layer of gas and dust where the conditions seem to favor star formation. My work aims at understanding the properties of star formation around Galactic HII regions.Using \herschel\, data (HOBYS and Hi-GAL programs) complemented with ancillary data, I studied two Galactic \HII\, regions (RCW~79 and RCW~120) to characterize the star formation observed at their edges. To study the impact of the ionization pressure, I computed the Star Formation Rate (SFR), which suggests that RCW~79 and RCW~120 are active star-forming regions despite their low gas surface density.A new study about the G345 region is in progress. This HII region is located above the Galactic plane and is actively forming stars. With the data available, the star formation's properties is being derived such as the spatial distribution of clumps, their stellar content, the SFR and CFE. This new study offers another opportunity to better understand the photoionization feedback out of the Galactic plane. Moreover, this will complete the sample of detailed studies of \HII\, regions, allowing us to obtain a global view of the mechanisms at play and of the efficiency of star formation in these regions.

Context: Unmanned Aerial Vehicles are being widely being used for various scientific and non-scientific purposes. This increases the need for effective and efficient path planning of Unmanned Aerial Vehicles.Two of the most commonly used methods are the A-star algorithm and Mixed Integer Linear Programming.Objectives: Conduct a simulation experiment to determine the performance of A-star algorithm and Mixed Integer Linear Programming for path planning of Unmanned Aerial Vehicle in a simulated environment.Further, evaluate A-star algorithm and Mixed Integer LinearProgramming based computational time and computational space to find out the efficiency. Finally, perform a comparative analysis of A star algorithm and Mixed Integer Linear Programming and analyse the results.Methods: To achieve the objectives, both the methods are studied extensively, and test scenarios were generated for simulation of Objectives: Conduct a simulation experiment to determine the performance of A-star algorithm and Mixed Integer Linear Programming for path planning of Unmanned Aerial Vehicle in a simulated environment.Further, evaluate A-star algorithm and Mixed Integer LinearProgramming based computational time and computational space to find out the efficiency. Finally, perform a comparative analysis of A star algorithm and Mixed Integer Linear Programming and analyse the results.Methods: To achieve the objectives, both the methods are studied extensively, and test scenarios were generated for simulation of Methods: To achieve the objectives, both the methods are studied extensively, and test scenarios were generated for simulation of these methods. These methods are then implemented on these test scenarios and the computational times for both the scenarios were observed.A hypothesis is proposed to analyse the results. A performance evaluation of these methods is done and they are compared for a better performance in the generated environment. Results: It is observed that the efficiency of A-star algorithm andMILP algorithm when no obstacles are considered is 3.005 and 12.03functions per second and when obstacles are encountered is 1.56 and10.59 functions per seconds. The results are statistically tested using hypothesis testing resulting in the inference that there is a significant difference between the computation time of A-star algorithm andMILP. Performance evaluation is done, using these results and the efficiency of algorithms in the generated environment is obtained.Conclusions: The experimental results are analysed, and the Conclusions: The experimental results are analysed, and the efficiencies of A-star algorithm and Mixed Integer Linear Programming for a particular environment is measured. The performance analysis of the algorithm provides us with a clear view as to which algorithm is better when used in a real-time scenario. It is observed that Mixed IntegerLinear Programming is significantly better than A-star algorithm.

We present an extremely deep CO(1-0) observation of a confirmed z = 1.62 galaxy cluster. We detect two spectroscopically confirmed cluster members in CO(1-0) with signal-to-noise ratio >5. Both galaxies have log (M-star/M-circle dot) > 11 and are gas rich, with M-mol/(M-star + M-mol) similar to 0.17-0.45. One of these galaxies lies on the star formation rate (SFR)-M-star sequence, while the other lies an order of magnitude below. We compare the cluster galaxies to other SFR-selected galaxies with CO measurements and find that they have CO luminosities consistent with expectations given their infrared luminosities. We also find that they have gas fractions and star formation efficiencies (SFE) comparable to what is expected from published field galaxy scaling relations. The galaxies are compact in their stellar light distribution, at the extreme end for all high-redshift star-forming galaxies. However, their SFE is consistent with other field galaxies at comparable compactness. This is similar to two other sources selected in a blind CO survey of the HDF-N. Despite living in a highly quenched protocluster core, the molecular gas properties of these two galaxies, one of which may be in the process of quenching, appear entirely consistent with field scaling relations between the molecular gas content, stellar mass, star formation rate, and redshift. We speculate that these cluster galaxies cannot have any further substantive gas accretion if they are to become members of the dominant passive population in z < 1 clusters.

Esta dissertação apresenta uma breve revisão introdutória de alguns aspectos importantes de astrofísica nuclear e da fenomenologia do plasma de quarks e glúons a baixas temperaturas. Acredita-se que tal estado da matéria existe no núcleo de estrelas de nêutron e possivelmente de outros objetos compactos em astrofísica. Uma equação de estado para tal sistema é derivada incluindo as influências dos condensados de glúon e do campo magnético que também é uma característica importante das estrelas de nêutron. Finalmente, essa equação de estado é aplicada para o estudo de estrutura estelar de estrelas compactas e alguns resultados importantes são discutidos. / This dissertation presents a brief introductory overview of some key aspects of nuclear astrophysics and of the phenomenology of the quark gluon plasma at cold temperatures which is believed to exist inside the core of neutron stars and possible other compact astrophysical objects. An equation of state for this state of matter is derived incluing the influence of gluon condensates and the magnetic field which is also an important characteristic of neutron stars. And finally this equation of state is applied to the study of compact stellar structure and some important results are discussed.

Orientador: Florência Cecília Menegalli / Dissertação (mestrado) - Universidade Estadual de Campinas, Faculdade de Engenharia de Alimentos / Made available in DSpace on 2018-08-16T13:52:13Z (GMT). No. of bitstreams: 1 Goncalves_JulianadeAlmeida_M.pdf: 23795201 bytes, checksum: bfbabbd676cb98b26b07e555c628e1a8 (MD5) Previous issue date: 2010 / Resumo: A carambola e fonte de importantes nutrientes como vitaminas, minerais e muitos fitoquimicos que exercem papeis importantes na saude humana. No entanto, o seu elevado conteudo de agua e a interferencia de agentes externos, como oxigenio e microorganismos, tornam esse produto perecivel e de facil deterioracao. O objetivo deste trabalho foi estudar o efeito da formulacao de coberturas comestiveis aditivadas com antioxidantes, aplicadas previamente a secagem, que assegurem a manutencao das propriedades funcionais de carambola em fatias. Na primeira etapa deste trabalho, fatias de carambolas foram revestidas com coberturas de pectina (2% m/m) e acidos citrico (0,5% m/m) e ascorbico (0,5% m/m), com coberturas de alginato (1% m/m) e acidos citrico (0,5% m/m) e ascorbico (0,5% m/m), com coberturas de pectina (2% m/m) e suco de uva (26% m/m) e com coberturas de alginato (1% m/m) e suco de uva (26% m/m), e desidratadas em secador de ar convectivo nas temperaturas de 50, 60 e 70°C, a fim de verificar a influencia da aplicacao das coberturas sobre a cinetica de secagem e sobre o encolhimento das amostras. Na segunda etapa do trabalho, as amostras foram novamente revestidas, secas e entao armazenadas por 21 dias, com temperatura controlada de 35°C, para avaliar suas caracteristicas nutricionais e fisicas. Verificou-se que a aplicacao das coberturas nao influenciou na cinetica de secagem. A manutencao da forca maxima de ruptura foi mais eficaz nas amostras revestidas, e a retencao da cor foi mais eficiente nas amostras cobertas com pectina e acidos. Em relacao as propriedades nutricionais, a aplicacao das coberturas de pectina auxiliou na retencao de carotenoides, vitamina C e polifenois / Abstract: The star fruit is a source of important nutrients such as vitamins, minerals and phytochemicals that play many important roles in human health. However, its high water content and the interference of external agents, such as oxygen and microorganisms, make this perishable product and easy to damage. The aim of this work was to study the effect of the formulation of biodegradable coatings added with antioxidants, applied prior to drying to ensure the maintenance of functional properties of star fruit slices. In the first stage of this work, star fruit slices were coated with pectin (2% w / w) and citric acid (0.5% w/w) and ascorbic (0.5% w / w) with coat of alginate (1% w / w) and citric acid (0.5% w / w) and ascorbic (0.5% w/ w) with coat of pectin (2% w / w) and grape juice (26%, w / w) and coated with alginate (1% w / w) and grape juice (26% w / w) and were dried in an air convective dryer at temperatures of 50, 60 and 70 ° C to verify the influence the application of the coating on the kinetics of drying and the shrinkage of the samples. In the second stage of this work, the samples were again coated, dried and then stored for 21 days, at temperatures of 35°C, to evaluate their nutritional and physical characteristics. It was found that the application of the coating did not influence the drying kinetics. The maintaining of the maximum tensile was more effective in samples coated and the color retention was more efficient in samples coated with pectin and acid. In relation to nutritional properties, the application of the coatings of pectin help in the retention of carotenoids, vitamin C and polyphenols / Mestrado / Mestre em Engenharia de Alimentos

Submitted by Jaqueline Duarte (1157279@mackenzie.br) on 2018-04-25T22:04:35Z No. of bitstreams: 2 Sheila Darcy Antonio Rodrigues.pdf: 5602212 bytes, checksum: c59de0a2c11682e90be6d1453a6f1116 (MD5) license_rdf: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5) / Approved for entry into archive by Eliana Barboza (eliana.silva1@mackenzie.br) on 2018-04-26T12:20:00Z (GMT) No. of bitstreams: 2 Sheila Darcy Antonio Rodrigues.pdf: 5602212 bytes, checksum: c59de0a2c11682e90be6d1453a6f1116 (MD5) license_rdf: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5) / Made available in DSpace on 2018-04-26T12:20:00Z (GMT). No. of bitstreams: 2 Sheila Darcy Antonio Rodrigues.pdf: 5602212 bytes, checksum: c59de0a2c11682e90be6d1453a6f1116 (MD5) license_rdf: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5) Previous issue date: 2018-02-06 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior / Fundo Mackenzie de Pesquisa / When we thinking about the production of the contemporary literature we can notice that a considerable part of the new releases, mainly those coming from the Unites States of America market, are part of great projects of the entertainment industry. Some of these projects may be called according to what was proposed by the researcher Henry Jenkins of transmedia storytelling and they are those types in which it is expanded the way of telling a story for the use of the most different types of existing media. One of the most successful cases of this kind of transmedia storytelling, which may even be considered a paradigm for this type of narrative is the case of Star Wars saga. Started in the year of 1976 with the release of Star Wars: from the adventures of Luke Skywalker, this saga have been developed for years and still is in the active. It has turned into a complex universe of films, cartoons, comics, ga mes and countless books that help to narrate the most diverses adventures, that happen in a galaxy, far, far away. Considering that the today revenue of the Star Wars saga is around fourty billion dollars and that of this amount, approximately, three billion dollars had came from the commercialization of books, it becomes interesting and necessary to investigate and to understand why there is the interest in a literature production, linked to this type of narrative, as well as to seek the knowledge of how to think about projects that are part of the entertainment industry, which encompass different media, and among them the literary media and that can become a success of audience. / Ao se pensar sobre produção literária contemporânea, pode-se observar que uma considerável parcela dos novos lançamentos, principalmente dos provenientes do mercado norte americano, fazem parte de grandes projetos da indústria do entretenimento. Alguns desses projetos podem ser denominados, de acordo com o proposto pelo pesquisador Henry Jenkins, de narrativas transmidiáticas (transmedia storytelling) e eles são aqueles nos quais se busca expandir a forma de se contar uma história para a utilização dos mais distintos tipos de mídias existentes. Um dos casos de maior sucesso desse tipo de narrativa transmidiática, que pode, até mesmo, ser considerado um paradigma para esse tipo de narrativa, é o da saga Star Wars. Iniciada em 1976 com o lançamento do livro Star Wars: from the adventures of Luke Skywalker, essa saga, desenvolvida durante anos e ainda na ativa, se transformou em um complexo universo do qual fazem parte filmes, desenhos animados, histórias em quadrinho, jogos e inúmeros livros que ajudam a narrar as mais diversas aventuras, que se passam em uma galáxia tão, tão distante. Considerando-se que hoje o faturamento da saga Star Wars se encontre em torno de quarenta bilhões de dólares e que deste montante quase três bilhões de dólares são provenientes da comercialização de livros, torna-se interessante e necessário que se busque pesquisar e compreender o porquê do interesse por uma produção de literatura, atrelada a esse tipo de narrativa, bem como buscar o conhecimento de como se pensar em projetos para a indústria do entretenimento, que englobem distintas mídias, e dentre elas a literária e que possam se converter em sucesso de público.

Though there has been a considerable amount of work investigating the early stages of low-mass star formation in recent years, the general theory is only broadly understood and several open questions remain. Specifically, the dominant physical mechanisms which connect large-scale molecular cloud structures, intermediate-scale filamentary gas flows, and small-scale collapsing prestellar envelopes in the interstellar medium are poorly constrained. Even for an individual forming protostar, the evolution of the mass accretion rate from the envelope onto the central object is debated with little observational evidence to help guide the theoretical framework. In addition, with the development of new technology such as the continuum imaging instrument in operation at the James Clerk Maxwell Telescope (JCMT), the Submillimetre Common User Bolometer Array 2 (SCUBA-2), the best practices for data reduction and image calibration for ground-based, submillimetre wavelength observations are still being investigated. In this dissertation, I address facets of these open questions in five main projects with an overarching focus on the flow of material from the largest to the smallest scales in a molecular cloud. By performing synthetic observations of a numerical simulation of a turbulent molecular cloud, I investigate the nature of prestellar envelopes and find evidence of larger mass reservoirs that form filamentary structures and feed cluster formation. Then, after robustly investigating and suggesting improvements for ground-based, submillimetre data reduction techniques, I continue to probe the connection between larger and smaller scales by characterising structure fragmentation in the Southern Orion A Molecular Cloud from the perspective of 850 m continuum data. Finally, I follow star forming material to even smaller scales by exploring the evolution of the mass accretion rate onto individual protostars. This examination has required designing and implementing unprecedented spatial alignment and flux calibration techniques at 850 m. Using these newly calibrated images, I am able to identify several candidate sources that show evidence for submillimetre variability, suggesting changes in protostellar accretion rates over several year timescales. / Graduate