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

Uppsatsen ämnar att ge en djupare förståelse för ljud i film och dess funktioner för en autentisk och realistisk filmupplevelse. Ljudet är sällan något man som åskådare lägger aktivt fokus på under en film med undantaget att man tycker att något inte stämmer. Så vad är det som krävs för att man inte ska ifrågasätta ljudet? Kvalitativa intervjuer med två personer yrkesaktiva inom ljudläggning samt en forskare inom ämnet har utförts för att kunna redovisa ingående tankar och åsikter om vad de anser vara ljudets viktigaste funktioner i modern film. Synkro nise ring och klang är centrala begrepp i undersökningen . De är exempel på faktorer som kan påverka hur man uppfattar kopplingen mellan ljud och bild. Med hjälp av uppsatsens insamlade data samt dess teoriavsnitt har dessa faktorer vidare konkretiserats genom en kort analys av tre utvalda scener från filmen Star Wars (1977). Uppsatsens mest centrala resultat baserar sig i idéen om samverkan mellan ljud och bild. Bilden klassas som det mest centrala i en film och ljud finns till för att förstärka eller berätta saker som bilden inte kan. Vad gäller realism inom filmljud så existerar det nästan inte. Det vi uppfattar som realistiskt behöver inte ha något med faktisk realism att göra. Uppsatsens diskussionsavsnitt berör studiens styrkor, svagheter samt förslag till fortsatt forskning.

We investigate the relation between gas and star formation in subgalactic regions, similar to 360. pc to similar to 1.5. kpc in size, within the nearby starburst dwarf NGC 4449, in order to separate the underlying relation from the effects of sampling at varying spatial scales. Dust and gas mass surface densities are derived by combining new observations at 1.1. mm, obtained with the AzTEC instrument on the Large Millimeter Telescope, with archival infrared images in the range 8-500 mu m from the Spitzer Space Telescope and the Herschel Space Observatory. We extend the dynamic range of our millimeter (and dust) maps at the faint end, using a correlation between the far-infrared/millimeter colors F(70)/F(1100) (and F(160)/F(1100)) and the mid-infrared color F(8)/F(24) that we establish for the first time for this and other galaxies. Supplementing our data with maps of the extinction-corrected star formation rate (SFR) surface density, we measure both the SFR-molecular gas and the SFR-total. gas relations in NGC 4449. We find that the SFR-molecular. gas relation is described by a power law with an exponent that decreases from similar to 1.5 to similar to 1.2 for increasing region size, while the exponent of the SFR-total. gas relation remains constant with a value of similar to 1.5 independent of region size. We attribute the molecular law behavior to the increasingly better sampling of the molecular cloud mass function at larger region sizes; conversely, the total gas law behavior likely results from the balance between the atomic and molecular gas phases achieved in regions of active star formation. Our results indicate a nonlinear relation between SFR and gas surface density in NGC 4449, similar to what is observed for galaxy samples.

The purpose with this thesis was to study user activities in a business system, MediusFlow. The overall objective was to identify user related problems and to analyse which of the usability data gathering methods to use in the future development process of the company Medius. The outcome of this study indicated that a cognitive related user problem was the most important problem to solve. A Star Life Cycle method was preferred. Two low-fidelity prototypes were developed to exemplify an alternative design solution to the identified cognitive user problem. Furthermore, the two best methods to use when gathering user related requirements were heuristic evaluation and expert review. In addition a company specific Style Guide was created with generic guidelines as a foundation for development of future applications within Medius.

La régulation du moment cinétique est l'une des questions les plus importantes dans la formation d'étoiles. Du nuage moléculaire à l'étoile finale, le système perd la grande majorité de son moment cinétique et plusieurs processus sont avancés pour l'expliquer. Nous nous concentrons sur la magneto-hydrodynamique (MHD) non-idéale, qui permet de décrire le couplage entre un champ magnétique et un fluide. Son efficacité pour réguler le moment cinétique dans des conditions réalistes a été montrée à plusieurs reprises. Dans un premier temps, nous développons un code qui calcule l'équilibre chimique d'éléments présents dans les premières étapes de la formation d'étoile. Ainsi, nous pouvons retrouver la valeur des coefficients définissant l'intensité de chaque processus de la MHD non-idéale. Nous nous intéressons ensuite à l'un d'entre eux, l'effet Hall, encore peu étudié dans ce contexte. Nous l'implémentons dans le code eulérien RAMSES, et l'utilisons pour quantifier son influence pendant un effondrement gravitationnel. Comme prévu par la théorie, l'effet Hall influence grandement la taille du disque protoplanétaire, dans lequel se forment les planètes, et crée des enveloppes de gas tournant en sens inverse du reste du système / The angular momentum regulation is a hot topic in star formation. From the molecular cloud to th final star, the system loses most of its angular momentum, and several processes are proposed to explain this phenomenon. We focus on non-ideal magnetohydrodynamics (MHD), which describes the coupling between a fluid and its magnetic field. Its efficiency to regulate the angular momentum in realistic conditions has been shown in several studies. First, we develop a code that computes the chemical equilibrium of elements present in the early stages of star formation. We can therefore obtain the values of coefficients defining the strength of the phyical processes associated with non-ideal MHD. We then take interest in one of them, the Hall effect, still poorly studied in this context. We implement it in the eulerian code RAMSES, and use it to quantify its influence during a gravitational collapse. As predicted by theory, the Hall effect greatly influences the size of the protoplanetary disk, in which planets form, and creates envelopes of gas rotating backward compared to the rest of the system

We present new spatially resolved surface photometry in the far-ultraviolet (FUV) and near-ultraviolet (NUV) from images obtained by the Galaxy Evolution Explorer (GALEX) and IRAC1 (3.6 mu m) photometry from the Spitzer Survey of Stellar Structure in Galaxies (S(4)G). We analyze the radial surface brightness profiles mu(FUV), mu(NUV), and mu[3.6], as well as the radial profiles of (FUV - NUV), (NUV -[3.6]), and (FUV -[3.6]) colors in 1931 nearby galaxies (z < 0.01). The analysis of the 3.6 mu m surface brightness profiles also allows us to separate the bulge and disk components in a quasi-automatic way and to compare their light and color distribution with those predicted by the chemo-spectrophotometric models for the evolution of galaxy disks of Boissier & Prantzos. The exponential disk component is best isolated by setting an inner radial cutoff and an upper surface brightness limit in stellar mass surface density. The best-fitting models to the measured scale length and central surface brightness values yield distributions of spin and circular velocity within a factor of two of those obtained via direct kinematic measurements. We find that at a surface brightness fainter than mu([3.6]) = 20.89 mag arcsec(-2), or below 3 x 10(8) M-circle dot kpc(-2) in stellar mass surface density, the average specific star formation rate (sSFR) for star-forming and quiescent galaxies remains relatively flat with radius. However, a large fraction of GALEX Green Valley galaxies show a radial decrease in sSFR. This behavior suggests that an outside-in damping mechanism, possibly related to environmental effects, could be testimony of an early evolution of galaxies from the blue sequence of star-forming galaxies toward the red sequence of quiescent galaxies.

Superfamily Himerometroidea AH Clark, 1908 (Echinodermata: Crinoidea) (formerly Mariametroidea) is the second most speciose superfamily in order Comatulida. Although it includes some of the most common species on tropical western Pacific reefs, its phylogeny is poorly understood. Genus- to species-level taxa are currently distinguished by plastic morphological characters. We revised the superfamily from species- to family-levels using a combined morphological and molecular approach. A phylogeny using two nuclear and three mitochondrial markers recovered Colobometridae and Himerometridae as paraphyletic and Mariametridae and Zygometridae as polyphyletic. Within genus Himerometra (Himerometridae), sequence data and detailed morphological examinations of multiple specimens of H. magnipinna, H. martensi and H. robustipinna indicated that these three taxa are conspecific. A similar examination of specimens attributed on morphological grounds to the genera Dichrometra, Liparometra and Lamprometra (Mariametridae) revealed a lack of substantial enough sequence and morphological differences to maintain them as distinct genera. We have synonymized all three genera and redescribed four species under the senior name Dichrometra. Additional work is needed to more clearly establish characters that will diagnose clades across the superfamily. This study illustrates the importance of reevaluating classifications that incorporate ecophenotypically and ontogenetically variable characters.

We present an analysis of high-resolution ALMA interferometry of CO(4-3) line emission and dust continuum in the "Ruby" (PLCK_G244.8+54.9), a bright, gravitationally lensed galaxy at z = 3.0 discovered with the Planck all-sky survey. The Ruby is the brightest of Planck's dusty GEMS, a sample of 11 of the brightest gravitationally lensed high-redshift galaxies on the extragalactic sub-mm sky. We resolve the high-surface-brightness continuum and CO line emission of the Ruby in several extended clumps along a partial, nearly circular Einstein ring with 1.4 '' diameter around a massive galaxy at z = 1.5. Local star-formation intensities are up to 2000 M-circle dot yr(-1) kpc(-2), amongst the highest observed at high redshift, and clearly in the range of maximal starbursts. Gas-mass surface densities are a few x10(4) M-circle dot pc(-2). The Ruby lies at, and in part even above, the starburst sequence in the Schmidt-Kennicutt diagram, and at the limit expected for star formation that is self-regulated through the kinetic energy injection from radiation pressure, stellar winds, and supernovae. We show that these processes can also inject sufficient kinetic energy and momentum into the gas to explain the turbulent line widths, which are consistent with marginally gravitationally bound molecular clouds embedded in a critically Toomre-stable disk. The star-formation efficiency is in the range 1-10% per free-fall time, consistent with the notion that the pressure balance that sets the local star-formation law in the Milky Way may well be universal out to the highest star-formation intensities. AGN feedback is not necessary to regulate the star formation in the Ruby, in agreement with the absence of a bright AGN component in the infrared and radio regimes.