Dissertations / Theses: 'PlaNet'

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Armour, Cheryl. "Planet Place." Thesis, National Library of Canada = Bibliothèque nationale du Canada, 1997. http://www.collectionscanada.ca/obj/s4/f2/dsk2/ftp04/mq25951.pdf.

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Greene, Jason. "New planet." Honors in the Major Thesis, University of Central Florida, 2001. http://digital.library.ucf.edu/cdm/ref/collection/ETH/id/278.

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This item is only available in print in the UCF Libraries. If this is your Honors Thesis, you can help us make it available online for use by researchers around the world by following the instructions on the distribution consent form at http://library.ucf.edu/Systems/DigitalInitiatives/DigitalCollections/InternetDistributionConsentAgreementForm.pdf You may also contact the project coordinator, Kerri Bottorff, at kerri.bottorff@ucf.edu for more information.
Bachelors
Arts and Sciences
Liberal Studies

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Tolbert, Clayton T. "Lonely Planet." Digital Commons at Loyola Marymount University and Loyola Law School, 2013. https://digitalcommons.lmu.edu/etd/8.

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hojat, roxana. "Plantiod Planet." VCU Scholars Compass, 2017. http://scholarscompass.vcu.edu/etd/5048.

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This thesis examines my studio practice and research during my studies at Virginia Commonwealth University in the Photo & Film MFA program, which has culminated into my thesis exhibition. Through traditional portraiture and landscape photography that utilize contemporary photographic practices such as digital processing and material studies, my work in Plantiod Planet creates a fiction which examines plant intelligence and the gendering of landscape.

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Williams, Gareth Vaughan. "Minor planet astrophotometry." Thesis, Open University, 2012. http://oro.open.ac.uk/54834/.

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Historically, the Minor Planet Center (MPC) has concentrated on improving the quality of the astrometric observations and the resulting orbits of minor planets. In light of long-standing complaints in the literature about the quality of the photometric parameters for the minor planets, there has been a need to improve the quality of the absolute magnitudes, H, and slope parameters, G. However, this task is complex, as the bulk of the minor-planet magnitude estimates are suppl ied by the astrometric observers. These observations are not made through standard fillers and are made with respect to the (indifferent) magnitudes in numerous astrometric reference catalogues. Such magnitude estimates are labelled "astrophotometry", to reflect their low quality. This thesis describes a method for correcting the catalogue- and observer-specific errors present in the astrophotometry. This method was applied to more than 70 million astrometric observations with magnitude estimates. New H determinations have been made for 322 607 numbered minor planets, while new G determinations have been made for 64 348 numbered minor planets. New assumed G values have been determined for 258 259 numbered minor planets. Analysis of the results shows that the problems identified in the literature have been removed, particularly the -0.5 magnitude offset at H14 that is present in the current MPC HG data set. Implications of the new H magnitudes on the albedos determined by the WISE space mission and on the differential H distributions of various types of solar-system object are discussed.

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Buchen, Callista Mary. "The Bloody Planet." Bowling Green State University / OhioLINK, 2010. http://rave.ohiolink.edu/etdc/view?acc_num=bgsu1269214700.

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Brickman, Jacklyn E. "Experiments in Biological Planet Formation and Plants: Nourishing Bodies, Nourishing Planets." The Ohio State University, 2020. http://rave.ohiolink.edu/etdc/view?acc_num=osu1595340630648528.

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Montgomery, Ryan Michael. "Planet formation and searches /." Diss., Digital Dissertations Database. Restricted to UC campuses, 2009. http://uclibs.org/PID/11984.

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Mekritthikrai, Kanit. "High Resolution Planet Rendering." Thesis, Linköpings universitet, Institutionen för teknik och naturvetenskap, 2011. http://urn.kb.se/resolve?urn=urn:nbn:se:liu:diva-69214.

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Planet rendering plays an important role in universe visualization and geographic visualization. The recent tools and methods allow better data acquisition, usually with very high resolution. However in computer graphics, there is always the limitation on the resolution of geometry and texture due to numerical imprecision. Not many applications can handle high resolution data effectively. This thesis introduces, Implicit Surface Scene, a level of detail scene management inspired by dynamic coordinate system and SCALEGRAPH™ which change over time depending on the current camera position relative to the planet surface. Our method is integrated into Uniview and allows Uniview to render high resolution planet geometry with dynamic texture composition and with a surface positioning system that does not suffer from precision issue.

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Gerbrandy, Jelle Douwe. "Bisimulations on planet Kripke." Amsterdam : Amsterdam : Institute for Logic, Language and Computation, Universiteit van Amsterdam ; Universiteit van Amsterdam [Host], 1999. http://dare.uva.nl/document/33058.

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Гладченко, Оксана Робертівна, Оксана Робертовна Гладченко, Oksana Robertivna Hladchenko, and V. Zhuravel. "Pollution of our planet." Thesis, Видавництво СумДУ, 2008. http://essuir.sumdu.edu.ua/handle/123456789/16002.

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Robinson, Sarah Elaine. "Chemistry of planet formation /." Diss., Digital Dissertations Database. Restricted to UC campuses, 2008. http://uclibs.org/PID/11984.

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Heymans, Suzanne Elizabeth Art College of Fine Arts UNSW. "Plant planet; recording / recoding invisible energy via the lens of the land." Awarded by:University of New South Wales. Art, 2009. http://handle.unsw.edu.au/1959.4/44700.

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This research investigates the ???earth / human equation???, in which the land is identified as the indispensable nutrient for human existence. Observation of the ongoing processes of exploitation of the land and the images that result from this, leads to a questioning of some of the Western ideas and concepts that provided the legal and ethical framework for colonisation. A perceived connection between material form and energy as the fundamental paradigm for my studio practice informs my enquiry into theories about energy and its representation. I have chosen to methodologically allegorise and illustrate human dependence upon and connection to the earth by a series of references located in science and spirituality. Concepts of energy, codification and pattern are seen in the terms of ???exchangeable currency???, where organic models function as a ???template??? informing a philosophical framework, illustrative of the complexities of the relationship between earth and people. Within this hybrid structure, part hard science and part intuitive interpretation, some of the patterns formed in the exchange of energy between the earth and its peoples are interpreted in terms of a cultural stance and siting of the land in relation to the self.

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Armstrong, John C. "Wind erosion and long period climate change on Mars /." Thesis, Connect to this title online; UW restricted, 2003. http://hdl.handle.net/1773/5447.

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Hood, Ben Andrew Ashcom. "Extrasolar planet search and characterisation." Thesis, St Andrews, 2007. http://hdl.handle.net/10023/359.

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Ayliffe, Benjamin A. "Giant planet formation and migration." Thesis, University of Exeter, 2009. http://hdl.handle.net/10036/85873.

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This thesis describes efforts to improve the realism of numerical models of giant planet formation and migration in an attempt to better understand these processes. A new approach has been taken to the modelling of accretion, designed to mimic reality by allowing gas to accumulate upon a protoplanetary surface. Implementing this treatment in three-dimensional self-gravity radiation hydrodynamics calculations provides an excellent model for planet growth, allowing an exploration of the factors that affect accretion. Moreover, these calculations have also been extended to investigate the migration of protoplanets through their parent discs as they grow. When focusing on the growth of non-migrating protoplanets, the models are performed using small sections of disc, enabling excellent resolution right down to the core; gas structures and flow can be resolved on scales from ~ 10^4 to 10^11 metres. Using radiative transfer, these models reveal the importance of opacity in determining the accretion rates. For the low mass protoplanets, equivalent in mass to a giant planet core (~ 10 M⊕), the accretion rates were found to increase by up to an order of magnitude for a factor of 100 reduction in the grain opacity of the parent circumstellar disc. However, even these low opacities lead to growth rates that are an order of magnitude slower than those obtained in locally-isothermal conditions. For high mass protoplanets (>~ 100M⊕), the accretion rates show very little dependence upon opacity. Nevertheless, the rates obtained using radiative transfer are still lower than those obtained in locally-isothermal models by a factor of ~2, due to the release of accretion energy as heat. Only high mass protoplanets are found to be capable of developing circumplanetary discs, and this ability is dependent upon the opacity, as are the scaleheights of such discs. However, their radial extents were found to be independent of the opacity and the protoplanet mass, all reaching ≈ RH/3, inline with analytic predictions. Migration is investigated using global models, ensuring a self-consistently evolved disc. Using locally-isothermal calculations, it was found that the capture radius of an accreting sink particle, used to model a protoplanet without a surface, must be small (<< RH) to yield migration timescales consistent with linear theory of Type I migration. In the low mass regime of Type I migration, accreting sinks with such small radii yield timescales consistent with those models in which a protoplanetary surface is used. However, for high mass protoplanets, undergoing Type II migration, the surface treatment leads to faster rates of migration, indicating the importance of a realistic accretion model. Using radiative transfer, with high opacities, leads to a factor of ~ 3 increase in the migration timescale of the lowest mass protoplanets, improving their chances of survival. As suitable gas giant progenitors, their survival is key to understanding the growth of giant planets. An unexpected result of the radiative transfer was a reduction in the migration timescale of high mass planets. This appears to be a result of the less thoroughly evacuated gaps created by planets in non-locally-isothermal discs, which affects the corotation torque.

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Mullins, Shena. "Alien on a Savage Planet." ScholarWorks@UNO, 2014. http://scholarworks.uno.edu/td/1934.

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This paper details the process of creating the UNO Graduate thesis film Alien on a Savage Planet. Each major step in the filmmaking process is covered: screenwriting, producing, directing, cinematography, sound, production design, costumes, hair and makeup, workflow, editing, color correction, music and post- sound. A comprehensive assessment of the filmmaking process and the successes and failures of the project are discussed in length.

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Howe, Alex Ryan. "Topics in Extrasolar Planet Characterization." Thesis, Princeton University, 2016. http://pqdtopen.proquest.com/#viewpdf?dispub=10167564.

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I present four papers exploring different topics in the area of characterizing the atmospheric and bulk properties of extrasolar planets. In these papers, I present two new codes, in various forms, for modeling these objects. A code to generate theoretical models of transit spectra of exoplanets is featured in the first paper and is refined and expanded into the APOLLO code for spectral modeling and parameter retrieval in the fourth paper. Another code to model the internal structure and evolution of planets is featured in the second and third papers. The first paper presents transit spectra models of GJ 1214b and other super-Earth and mini-Neptune type planets—planets with a “solid”, terrestrial composition and relatively small planets with a thick hydrogen-helium atmosphere, respectively—and fit them to observational data to estimate the atmospheric compositions and cloud properties of these planets. The second paper presents structural models of super-Earth and mini-Neptune type planets and estimates their bulk compositions from mass and radius estimates. The third paper refines these models with evolutionary calculations of thermal contraction and ultraviolet-driven mass loss. Here, we estimate the boundaries of the parameter space in which planets lose their initial hydrogen-helium atmospheres completely, and we also present formation and evolution scenarios for the planets in the Kepler-11 system. The fourth paper uses more refined transit spectra models, this time for hot jupiter type planets, to explore the methods to design optimal observing programs for the James Webb Space Telescope to quantitatively measure the atmospheric compositions and other properties of these planets.

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Galicher, R., C. Marois, B. Macintosh, B. Zuckerman, T. Barman, Q. Konopacky, I. Song, et al. "The International Deep Planet Survey." EDP SCIENCES S A, 2016. http://hdl.handle.net/10150/622797.

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Context. Radial velocity and transit methods are effective for the study of short orbital period exoplanets but they hardly probe objects at large separations for which direct imaging can be used. Aims. We carried out the international deep planet survey of 292 young nearby stars to search for giant exoplanets and determine their frequency. Methods. We developed a pipeline for a uniform processing of all the data that we have recorded with NIRC2/Keck II, NIRI/Gemini North, NICI/Gemini South, and NACO/VLT for 14 yr. The pipeline first applies cosmetic corrections and then reduces the speckle intensity to enhance the contrast in the images. Results. The main result of the international deep planet survey is the discovery of the HR8799 exoplanets. We also detected 59 visual multiple systems including 16 new binary stars and 2 new triple stellar systems, as well as 2279 point-like sources. We used Monte Carlo simulations and the Bayesian theorem to determine that 1.05(-0.70)(+2.80)% of stars harbor at least one giant planet between 0.5 and 14 MJ and between 20 and 300AU. This result is obtained assuming uniform distributions of planet masses and semi-major axes. If we consider power law distributions as measured for close-in planets instead, the derived frequency is 2.30(-1.55)(+5.95)%, recalling the strong impact of assumptions on Monte Carlo output distributions. We also find no evidence that the derived frequency depends on the mass of the hosting star, whereas it does for close-in planets. Conclusions. The international deep planet survey provides a database of confirmed background sources that may be useful for other exoplanet direct imaging surveys. It also puts new constraints on the number of stars with at least one giant planet reducing by a factor of two the frequencies derived by almost all previous works.

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Paiva, Inês Nisa Caetano Pereira de Almeida e. "Houses for a small planet." Master's thesis, Universidade de Lisboa, Faculdade de Arquitetura, 2018. http://hdl.handle.net/10400.5/18003.

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Dissertação de Mestrado Integrado em Arquitetura, com a especialização em Arquitetura apresentada na Faculdade de Arquitetura da Universidade de Lisboa para obtenção do grau de Mestre.
Desafiando a tendência de homogeneização na concepção de lugares em megacidades num mundo cada vez mais globalizado, este projecto procura encontrar pistas em traços culturais perseverantes, reiterando elementos fundamentais da identidade japonesa e, simultaneamente, construindo pontes entre múltiplas gerações. Com foco em diversos desafios paradigmáticos enfrentados por Tóquio no século XXI, e através de um retrato fenomenológico da sua sociedade singular, o presente estudo visa reinterpretar os valores ancestrais - que paradoxalmente prevaleceram face aos mais cáusticos eventos da história quando praticamente nada mais nesta cidade o conseguiu - em todos os complexos sistemas da contemporaneidade. Impulsionando a revitalização da monofuncional zona de escritórios em Nishi-Shinjuku (Shinjuku Oeste) - rastreando o seu legado e reescrevendo a sua história através da criação de lugares intergeracionais e multifuncionais onde a comunidade possa viver, trabalhar, crescer, relaxar, desfrutar, criar e interagir - estabelece-se um novo rumo numa das áreas mais segmentadas da cidade, trazendo a habitação de volta ao centro, através de tipologias habitacionais alternativas em altura. Localizado na fronteira de Nishi-Shinjuku, o Ju-Ni Quarter situa-se precisamente na margem do plano de reordenamento urbano do pós-guerra dos anos sessenta, conferindo-lhe a capacidade de interligar a zona formal de arranha-céus de escritórios com o tecido habitacional que se estende horizontalmente e de determinar até que ponto pode uma sociedade sobrepopulada, orientada para o trabalho e envelhecida beneficiar destas relações intergeracionais.
ABSTRACT: Defying the trend for homogenisation of placemaking in megacities in an increasingly globalised world, this work seeks to find clues in highly persevering cultural traits, reiterating fundamental elements of the Japanese identity and simultaneously building bridges between multiple generations. Focusing on some of the paradigmatic challenges faced by Tokyo in the 21st century, and through a phenomenological portrayal of its singular society, the present study aims to reinterpret the ancestral values - which have paradoxically prevailed through some of the most caustic events in history when barely nothing else in this city had - in all the complex systems of contemporaneity. By igniting the revitalization of the monofunctional office district in Nishi-Shinjuku (West-Shinjuku) - tracing its legacy and retelling its history through the creation of intergenerational and multifunctional places where people are able to live, work, grow, relax, enjoy, create and interact - a new path is set in one of the most segmented areas of the city, bringing housing back to the city centre in high-rise alternative dwelling typologies. Located on the border of Nishi-Shinjuku, Ju-Ni Quarter stands right by the fringe of the 1960s post-war urban redevelopment plan, giving it the ability to connect the formal high-rise office district to the low-rise sprawled residential fabric and to determine to what extent can an overpopulated, work-driven and ageing society benefit from these intergenerational relationships.
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Fischer, Julia Maria. "Houses for a small planet." Master's thesis, Universidade de Lisboa, Faculdade de Arquitetura, 2019. http://hdl.handle.net/10400.5/19202.

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Dissertação de Mestrado Integrado em Arquitetura, com a especialização em Interiores e Reabilitação do Edificado apresentada na Faculdade de Arquitetura da Universidade de Lisboa para obtenção do grau de Mestre.
um pequeno planeta”, iniciado em 2009 no CIAUD. „A quarta fase do projecto é definida pela correlação marcante de Portugal com o mundo desde os tempos mais remotos até aos dias de hoje, destacando vários países e cidades e a sua condição urbana contemporânea com influência portuguesa. Influenciada por ambas, a releitura da rota das descobertas e a imigração de tantas partes do mundo, e o legado patrimonial construído de valor universal execional que permitiu a criação de uma rede de países com patrimônio mundial de influência portuguesa em 2006 - a rede WHPO. “1) É uma contribuição para a investigação da contingência contemporânea de crescimento e densificação, propondo através da reflexão de contextos particulares, abordagens críticas que promovam soluções que sustentem novas urbanidades emergentes. O principal objetivo deste projeto é o desenvolvimento de uma unidade de instalação integrada e sustentável para uma javanesa Kawasan Kumuh (área de favela urbana) em Denpasar, Bali, no campo da urbanização de favelas. Ao impor novas lógicas e estratégias de implementação, promove, a partir de potencialidades locais, soluções de espaço urbano e arquitetônico integrado. O trabalho parte do estudo das realidades concretas: é preciso uma intensa reflexão sobre a sociedade javanesa, a história de Bali e sua arquitetura. Principalmente ilustrado por fotos tiradas no chão. Posteriormente, assume um caráter de reflexão mais geral sobre os vários paradigmas da habitação em contextos de informalidade, descrevendo as áreas de favela em geral e, de forma precisa, o caráter, os problemas e a história. Isso mostra que uma solução arquitetônica contemporânea para os problemas da Kawasan Kumuh é baseada principalmente na detecção e eliminação de processos falsos, mas é tão importante apoiar os aspectos positivos que ocorrem. Assim, a urbanização de favelas é uma das ferramentas mais importantes para ajudar e melhorar. Uma vez que as favelas e sua sociedade viva muitas vezes desenvolveram suas próprias dinâmicas, que são muito difíceis para os estrangeiros entenderem e experimentarem, é importante incluí-los no planejamento e manter essas estruturas de trabalho, conhecimento e dinâmicas positivas.
ABSTRACT: ‚Houses for a Small Planet‘ started in 2009 at CIAUD. „The 4th phase of the project is defined by the striking correlation of Portugal with the world from the earliest times until today, highlighting several countries and cities and their contemporary urban condition with Portuguese influence. Influenced by both, the rereading of the route of discoveries and the immigration from so many parts of the world, and to the patrimonial legacy built of universal execional value that allowed the creation of a network of countries with world heritage assets of Portuguese influence in 2006 - the WHPO network.“ 1) It is a contribution on the investigation of the contemporary contingency of growth and densification, proposing through reflection of particular contexts, critical approaches that promote solutions that support new emerging urbanities. The main objective of this project is the development of an integrated and sustainable facility unit for a Javanese Kawasan Kumuh (urban slum area) in Denpasar, Bali in the field of slum-upgrading. By imposing new logics and implementation strategies, it promotes, from local potentialities, solutions of integrated urban and architectural space. The work starts from the study of concrete realities: It takes an intense contemplation about Javanese society, the history of Bali and its architecture. Mainly illustrated by pictures taken on the ground. Thereafter it assumes a character of more general reflection on the various paradigms of dwelling in contexts of informality by describing slum areas in general and precisly the character, problems and history. It shows that a contemporary architectural solution to the problems of Kawasan Kumuh is mainly based on detecting and eliminating falsely running processes, but it is just as important to support the positive aspects that occur. Thus, slum upgrading is one of the most important tools to help and improve. Since slums and their living society have often developed their own dynamics, which are very difficult for outsiders to understand and experience, it is important to include them in the planning and to maintain these working structures, knowledge and positive dynamics.
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Muto, Takayuki. "Diversity of Disk-Planet Interaction." 京都大学 (Kyoto University), 2010. http://hdl.handle.net/2433/120654.

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Price, Susan Glynis. "Planet Ranch: 1984 through 1990." Thesis, The University of Arizona, 1990. http://hdl.handle.net/10150/291207.

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Russell, Patrick S. "On the activity of water on Mars : investigations into the groundwater system and the stability of ice in the crater-interior environment /." View online version; access limited to Brown University users, 2005. http://gateway.proquest.com/openurl?url_ver=Z39.88-2004&res_dat=xri:pqdiss&rft_val_fmt=info:ofi/fmt:kev:mtx:dissertation&rft_dat=xri:pqdiss:3174667.

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Thesis (Ph.D.)--Brown University, 2005.
Vita. Thesis advisor: James W. Head III. Includes bibliographical references (leaves 43-49, 86-87, 125-130, 191-194, 237-238, 276-277). Also available online.

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Horne, David. "A method to obtain dust and ice cloud optical depths over the cold polar surfaces of Mars /." Connect to Online Resource-OhioLINK, 2007. http://rave.ohiolink.edu/etd/view.cgi?acc_num=toledo1177653341.

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Dissertation (Ph.D.)--University of Toledo, 2007
Typescript. Title on abstract page: A method to obtain thermal spectra of Martian dust storms over cold polar surfaces "Submitted as partial fulfillment of the requirements for The Doctor of Philosophy Degree in Physics." Bibliography: leaves 91-98.

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Cull, Selby C. "Dynamic digital Mars /." Amherst, Mass. : [s.n.], 2005. http://ddm.geo.umass.edu/ddm-marsmin/.

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A Division III examination in the School of Natural Science, Hampshire College, May 2005. Chairperson, Steven Roof.
Typescript. Also available on the World Wide Web. Includes bibliographical references.

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Lin, Min-Kai. "Dynamical instabilities in disc-planet interactions." Thesis, University of Cambridge, 2012. https://www.repository.cam.ac.uk/handle/1810/245135.

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Protoplanetary discs can be dynamically unstable due to structure induced by an embedded giant planet. In this thesis, I discuss the stability of such systems and explore the consequence of instability on planetary migration. I present semi-analytical models to understand the formation of the unstable structure induced by a Saturn mass planet, which leads to vortex formation. I then investigate the effect of such vortices on the migration of a Saturnmass planet using hydrodynamic simulations. I explain the resulting nonmonotonic behaviour in the framework of type III planetary migration. I then examine the role of disc self-gravity on the vortex instabilities. It can be shown that self-gravity has a stabilising effect. Linear numerical calculations confirms this. When applied to disc-planet systems, modes with small azimuthal wavelengths are preferred with increasing disc selfgravity. This is in agreement the observation that more vortices develop in simulations with increasing disc mass. Vortices in more massive discs also resist merging. I show that this is because inclusion of self-gravity sets a minimal vortex separation preventing their coalescence, which would readily occur without self-gravity. I show that in sufficiently massive discs vortex modes are suppressed. Instead, global spiral instabilities develop. They are interpreted as disturbances associated with the planet-induced structure, which interacts with the wider disc leading to instability. I carry out linear calculations to confirm this physical picture. Results from nonlinear hydrodynamic simulations are also in agreement with linear theory. I give examples of the effect of these global modes on planetary migration, which can be outwards, contrasting to standard inwards migration in more typical disc models. I also present the first three-dimensional computer simulations examining planetary gap stability. I confirm that the results discussed above, obtained from two-dimensional disc approximations, persist in three-dimensional discs.

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Gibbons, Peter George. "Planet formation in self-gravitating discs." Thesis, University of Edinburgh, 2013. http://hdl.handle.net/1842/8263.

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The work performed here studies particle dynamics in local two-dimensional simulations of self-gravitating accretion discs with a simple cooling law. It is well known that the structure which arises in the gaseous component of the disc due to a gravitational instability can have a significant effect on the evolution of dust particles. Previous results using global simulations indicate that spiral density waves are highly efficient at collecting dust particles, creating significant local over-densities which may be able to undergo gravitational collapse. This thesis expand on these findings, using a range of cooling times to mimic the conditions at a large range of radii within the disc. The PENCIL Code is used to solve the 2D local shearing sheet equations for gas on a fixed grid together with the equations of motion for solids coupled to the gas solely through aerodynamic drag force. The work contained here shows that spiral density waves can create significant enhancements in the surface density of solids, equivalent to 1-10cm sized particles in a disc following the profiles of Clarke (2009) around a solar mass star, causing it to reach concentrations several orders of magnitude larger than the particles mean surface density. These findings suggest that the density waves that arise due to gravitational instabilities in the early stages of star formation provide excellent sites for the formation of large, planetesimal-sized objects. These results are expanded on, with subsequent results introducing the effects of the particles self-gravity showing these concentrations of particles can gravitationally collapse, forming bound structures in the solid component of the disc.

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Fogg, Martyn John. "Terrstrial planet formation in exoplanetary systems." Thesis, Queen Mary, University of London, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.509700.

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Downey, Brynna G. "Finding the location of Planet Nine." Thesis, Massachusetts Institute of Technology, 2016. http://hdl.handle.net/1721.1/114095.

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Thesis: S.B., Massachusetts Institute of Technology, Department of Earth, Atmospheric, and Planetary Sciences, June 2017.
Cataloged from PDF version of thesis.
Includes bibliographical references (page 19).
To find Planet Nine, we use N-body simulations to find the true anomaly of Planet Nine that would render distant KBOs the most stable. We obtain an interval of 162-198°matching the intervals given by Medvedev & Vavilov (2016) of 176-184° and Brown & Batygin (2016) of 180°. According to our results, Planet Nine should reside in the constellation Lepus.
by Brynna G. Downey.
S.B.

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Ryan, Patrick Thomas. "Methods for extra-solar planet searches." Diss., The University of Arizona, 1996. http://hdl.handle.net/10150/290663.

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Many groups are trying to find faint stellar companions using a variety of techniques. The most obvious is to take long exposure pictures. Here adaptive optics (AO) is useful in correcting the blurring effects of the atmosphere. Starlight is concentrated into a tighter peak and less energy is put into the surrounding halo. Another method is to look for periodic decreases in a star's irradiance due to a planet blocking some of the light as it crosses in front of the star or transits. The most productive technique so far has been to look for periodic doppler shifts in the light coming from a candidate star, i.e. radial velocity searches. Several large planets have been found this way. This dissertation explores aspects of these three methods. The ability to detect a companion amid noise depends on the properties of the noise. While theoretical expectations exist for the properties of the halo produced by an AO system, experimental studies are few. The temporal and spatial characteristics of the halo produced by the AO system at the Starfire Optical Range are explored from the viewpoint of searching for faint stellar companions. We set limiting companion magnitudes for stars imaged while searching for brown dwarfs. The primary limitation to ground based transit searches is scintillation, irradiance fluctuations due to atmospheric turbulence. We explore reduction of this noise via differencing signals from binary stars. Theory is extended to include temporal and angular separation effects simultaneously. Evaluation of the derived equations and simulations demonstrate the benefits and limitations. Finally the design of an echelle spectrograph for use on the 6.5 m MMT or the Magellan telescope that is well suited to radial velocity searches for planets is presented. It has throughput between 10% and 18%, resolution of 200,000 per pixel and can sample the entire 0.31 to 1.1 μm range at once. This is accomplished by avoiding metallic reflections whenever possible and by using a mosaic of CCDs fit to the curved focal surface of a Schmidt camera. Efficient simultaneous observation of many spectral lines makes this a powerful instrument for radial velocity companion searches.

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McLeod, Scott Stuart. "Isostatically compensated extensional tectonics on Enceladus." Thesis, Montana State University, 2009. http://etd.lib.montana.edu/etd/2009/mcleod/McLeodS0509.pdf.

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Saturn's moon Enceladus is the smallest body in the solar system known to be geologically active. Extensive, energetic resurfacing processes are ongoing and it possesses a system of geysers at the South Pole that supply material to the E-ring. The South Polar Terrain (SPT) is the youngest region on Enceladus and its contacts with the older cratered and grooved plains to the north are delineated by a variety of complex geologic features including mountain ranges and massive grabens. Many of the geologic features seen on Enceladus bear superficial resemblance to terrestrial structures associated with plate tectonics. A detailed structural geologic analysis, supported by crater counting studies, was used to determine whether the features seen on Enceladus are compatible with terrestrial-style plate tectonics. On Earth, new lithosphere is created at spreading centers and consumed at subduction zones, enabled by the compositional dichotomy between oceanic and continental crust. Enceladus's lithosphere appears to be made entirely of pure water ice, so any newly formed crust will have the same composition, but lower density due to higher temperature, making subduction and consequently spreading, as we understand it on Earth, impossible. Geometrically, the absence of fold-thrust belts and transform faults in the presence of normal faults and basin and range-style features implies extension without corresponding shortening elsewhere. This is not possible in a conventional (terrestrial) plate tectonic regime as surface area is not conserved; therefore, an alternate explanation is required. Topographic features associated with density contrasts between old and new terrain that are diagnostic of terrestrial spreading centers are also not observed on Enceladus. I conclude that features observed on Enceladus are inconsistent with terrestrial-style plate tectonic spreading, and represent a style of tectonism peculiar to bodies with icy lithospheres. I present an interpretation in which the cordillera surrounding the SPT is a broadly developed extensional regime, and describe a model for its formation that is consistent with the known physical properties of Enceladus, dependent on the presence of a water-ice phase transition below the south polar terrain.

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Turse, Carol Louise. "Testing the hydrogen peroxide-water hypothesis of life on Mars using the differential scanning calorimeter as an analog for the TEGA instrument on the Mars Phoenix lander." Pullman, Wash. : Washington State University, 2009. http://www.dissertations.wsu.edu/Thesis/Summer2009/c_turse_072309.pdf.

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Thesis (M.S. in environmental science)--Washington State University, August 2009.
Title from PDF title page (viewed on Sept. 22, 2009). "School of Earth and Environmental Sciences." Includes bibliographical references (p. 92-97).

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Kraus, Stefan, John D. Monnier, Michael J. Ireland, Gaspard Duchêne, Catherine Espaillat, Sebastian Hönig, Attila Juhasz, et al. "Planet Formation Imager (PFI): science vision and key requirements." SPIE-INT SOC OPTICAL ENGINEERING, 2016. http://hdl.handle.net/10150/622530.

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The Planet Formation Imager (PFI) project aims to provide a strong scientific vision for ground-based optical astronomy beyond the upcoming generation of Extremely Large Telescopes. We make the case that a breakthrough in angular resolution imaging capabilities is required in order to unravel the processes involved in planet formation. PFI will be optimised to provide a complete census of the protoplanet population at all stellocentric radii and over the age range from 0.1 to similar to 100 Myr. Within this age period, planetary systems undergo dramatic changes and the final architecture of planetary systems is determined. Our goal is to study the planetary birth on the natural spatial scale where the material is assembled, which is the "Hill Sphere" of the forming planet, and to characterise the protoplanetary cores by measuring their masses and physical properties. Our science working group has investigated the observational characteristics of these young protoplanets as well as the migration mechanisms that might alter the system architecture. We simulated the imprints that the planets leave in the disk and study how PFI could revolutionise areas ranging from exoplanet to extragalactic science. In this contribution we outline the key science drivers of PFI and discuss the requirements that will guide the technology choices, the site selection, and potential science/technology tradeoffs.

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Natalini, Simone. "Ricerca di pianeti extrasolari: microlensing planet finder." Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2020. http://amslaurea.unibo.it/21585/.

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Questa tesi studia il fenomeno astronomico chiamato lente gravitazionale, in cui un oggetto massivo (lente) causa una curvatura della luce proveniente da un oggetto sullo sfondo (sorgente). Il lavoro è una ricerca bibliografica che parte da manuali di relatività generale e ne approfondisce gli argomenti con articoli scientifici più specifici e alcuni testi di presentazione di progetti pubblicati dalla NASA. Nel dettaglio si tratta il caso particolare dei fenomeni di microlensing, in cui l’effetto della lente sia piccolo e non si riesca ad individuare più di un’immagine distinta. Lo studio di questo tipo di fenomeni è molto importante nel campo della ricerca di pianeti extrasolari poiché copre un range di osservazione che non sarebbe possibile con altri metodi. Lo sviluppo dell’argomento procede partendo dallo studio della lente gravitazionale come caso generale per estrarre successivamente l’equazione ottica. Vengono poi studiati i parametri associati a quest’ultima e l’analisi dei modelli necessari per spiegare il fenomeno in esame. A ciò segue l’analisi delle caratteristiche e dei vantaggi di una ricerca planetaria di questo tipo eseguita da un telescopio orbitale. In conclusione si mostrano le caratteristiche e lo scopo di una proposta di missione spaziale presentata alla NASA per eseguire un censimento di pianeti extrasolari che possa misurare tutte le possibili distanze di ciascuno di essi dal proprio sole. In essa si rileva la necessità di dedicare una missione spaziale alla osservazione di una sezione di cielo appartenente alla costellazione del Sagittario per eseguire un censimento planetario statisticamente accurato, altrimenti impossibile a causa della bassa sensibilità dell’osservazione del cielo con un telescopio posizionato a terra e della totale mancanza di altri metodi per osservare corpi orbitanti e non orbitanti con masse così piccole.

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Lee, Aaron Thomas. "Star and Planet Formation through Cosmic Time." Thesis, University of California, Berkeley, 2018. http://pqdtopen.proquest.com/#viewpdf?dispub=10619929.

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The computational advances of the past several decades have allowed theoretical astrophysics to proceed at a dramatic pace. Numerical simulations can now simulate the formation of individual molecules all the way up to the evolution of the entire universe. Observational astrophysics is producing data at a prodigious rate, and sophisticated analysis techniques of large data sets continue to be developed. It is now possible for terabytes of data to be effectively turned into stunning astrophysical results. This is especially true for the field of star and planet formation. Theorists are now simulating the formation of individual planets and stars, and observing facilities are finally capturing snapshots of these processes within the Milky Way galaxy and other galaxies. While a coherent theory remains incomplete, great strides have been made toward this goal.

This dissertation discusses several projects that develop models of star and planet forma- tion. This work spans large spatial and temporal scales: from the AU-scale of protoplanetary disks all the way up to the parsec-scale of star-forming clouds, and taking place in both contemporary environments like the Milky Way galaxy and primordial environments at redshifts of z ~ 20.

Particularly, I show that planet formation need not proceed in incremental stages, where planets grow from millimeter-sized dust grains all the way up to planets, but instead can proceed directly from small dust grains to large kilometer-sized boulders. The requirements for this model to operate effectively are supported by observations. Additionally, I draw suspicion toward one model for how you form high mass stars (stars with masses exceeding ~ 8 M_sun), which postulates that high-mass stars are built up from the gradual accretion of mass from the cloud onto low-mass stars. I show that magnetic fields in star forming clouds thwart this transfer of mass, and instead it is likely that high mass stars are created from the gravitational collapse of large clouds. This work also provides a sub-grid model for computational codes that employ sink particles accreting from magnetized gas. Finally, I analyze the role that radiation plays in determining the final masses of the first stars to ever form in the universe. These stars formed in starkly different environments than stars form in today, and the role of the direct radiation from these stars turns out to be a crucial component of primordial star formation theory.

These projects use a variety of computational tools, including the use of spectral hydrodynamics codes, magneto-hydrodynamics grid codes that employ adaptive mesh refinement techniques, and long characteristic ray tracing methods. I develop and describe a long characteristic ray tracing method for modeling hydrogen-ionizing radiation from stars. Additionally, I have developed Monte Carlo routines that convert hydrodynamic data used in smoothed particle hydrodynamics codes for use in grid-based codes. Both of these advances will find use beyond simulations of star and planet formation and benefit the astronomical community at large.

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Östergaard, Johan. "Planet Rendering Using Online High-Resolution Datasets." Thesis, Linköpings universitet, Institutionen för teknik och naturvetenskap, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:liu:diva-95360.

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A large amount of image datasets are publicly available online through the web map service standard. The contents of the datasets span from satellite imagery of the earth and other planets of our solar system to various scientific data. This thesis presents an implementation of a planet renderer streaming high resolution image and height data from online datasets. The planet renderer uses a level of detail technique based on nodes connected by a quad tree data structure. The level of detail is determined by the size of the nodes in screen coordinates which ensures a sufficient texel to pixel ratio of the image data and a reasonably consistent polygon size in screen space. The project will be implemented in Uniview which is an application developed by SCISS AB and is primarily used in planetarium domes to visualize the Universe. Being able to visualize the high resolution image data and scientific measurements in a dome environment will provide the viewers a greater perspective of the data.

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Hellary, Phil. "Planet formation in radiatively inefficient protoplanetary discs." Thesis, Queen Mary, University of London, 2013. http://qmro.qmul.ac.uk/xmlui/handle/123456789/8465.

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I examine the effects on planetary system formation of radiatively inefficient disc models where positive corotation torques may counter the rapid inward migration of low-mass planets driven by Lindblad torques. I use N-body simulations coupled with algorithms to model the evolution of the gas disc, type I migration, gap formation and type II migration, planetary atmospheres that enhance the probability of planetesimal accretion by protoplanets, gas accretion on to forming planetary cores and gas disc dispersal. The inclusion of entropy and vorticity related corotation torques can lead to a net positive torque thus giving rise to outward migration of planets. This can allow larger planets to survive for a longer period of time, allowing some planets to accrete enough gas within the lifetime of the disc to undergo runaway gas accretion thus forming gas giant planets. I review the current status of extrasolar planet observations and the methods with which these observations are made, and provide a contextual review of the theory of planet formation. Using these models, I have successfully formed a number of gas giant planets with semi-major axes ranging from 0.1 AU up to 75 AU and masses from 100 Earth masses through to 700 Earth masses, as well as a large number of terrestrial sized planets. In later simulations, a large number of super-Earth, Neptune-mass and gas planets that are too small to be considered giants were formed also.

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Mutter, Matthew M. "Disc and planet evolution in circumbinary systems." Thesis, Queen Mary, University of London, 2018. http://qmro.qmul.ac.uk/xmlui/handle/123456789/31857.

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The inner regions of discs around close binary systems are dominated by tidally truncated eccentric cavities. These are believed to play a key role in dictating where planets formed in these circumbinary discs halt their disc-driven migration. In this thesis we present work examining processes which could impact the evolution and structure of this region, and the planets which interact with it. First, we investigate the role of self-gravity and disc-mass on circumbinary discs and planets. The greatest impact of self-gravity was found in discs around highly eccentric binaries, and in discs with high masses. In these cases, self-gravity acts to compact the scale of the inner cavity region. For the highest disc masses, additional eccentric features arise in the outer disc. A range of scenarios examining planetary migration, accretion and disc dissipation find that if planets form and evolve in a high-mass environment, the disc structures formed by self-gravity can leave a fingerprint on the planetary architecture once the disc has dissipated. We also significantly modify the publicly available fargo-adsg hydrodynamical code, to include radiative effects such as disc irradiation by the binary stars, radiative transport and disc surface cooling. We present preliminary results of simulations of adiabatic circumbinary discs with these effects included, and consider also the migration of protoplanets within them. Fully radiative discs produce a smaller inner cavity than obtained in previous isothermal models - a promising result for the end point of planet migration in these discs. Whilst we have found significant alteration of the circumbinary enviroment by self-gravity and radiative effects, future simulations that capture the 3-D nature of these discs will be required to fully describe the observed architecture of the circumbinary systems.

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Yan, Charles XiaoJian. "Planet photo-topography using shading and stereo." Thesis, Massachusetts Institute of Technology, 1993. http://hdl.handle.net/1721.1/17353.

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Perrine, Tim. "Forbidden Planet: Film Score for Full Orchestra." Digital Commons @ Butler University, 2003. http://digitalcommons.butler.edu/grtheses/400.

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The intent of my master's thesis is two-fold. First, I wanted to present a largescale work for orchestra that showcased the skills and craft I have developed as a composer (and orchestrator) to date. Secondly, since my goal as a composer is to work in Hollywood as a film composer, I wanted my large-scale work to function as a film score, providing the emotional backbone and highlighting action for a major motion picture. In order to achieve this, I needed a film that was both larger-than-life and contained, in my opinion, an easily replaceable score (or no score at all). After considering and viewing several different films of various genres, the 1956 MGM sci-fi classic Forbidden Planet seemed to be the perfect choice.

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Гладченко, Оксана Робертівна, Оксана Робертовна Гладченко, Oksana Robertivna Hladchenko, and A. Baranova. "Some problems of pollution of our planet." Thesis, Видавництво СумДУ, 2008. http://essuir.sumdu.edu.ua/handle/123456789/16026.

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Peng, Wentao. "Binary Planet–Satellite Nanostructure Using RAFT Polymer." Doctoral thesis, Niedersächsische Staats- und Universitätsbibliothek Göttingen, 2020. http://hdl.handle.net/21.11130/00-1735-0000-0005-144A-2.

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Sallum, Stephanie Elise, and Stephanie Elise Sallum. "Imaging Planet Formation Inside the Diffraction Limit." Diss., The University of Arizona, 2017. http://hdl.handle.net/10150/625645.

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For decades, astronomers have used observations of mature planetary systems to constrain planet formation theories, beginning with our own solar system and now the thousands of known exoplanets. Recent advances in instrumentation have given us a direct view of some steps in the planet formation process, such as large-scale protostar and protoplanetary disk features and evolution. However, understanding the details of how planets accrete and interact with their environment requires direct observations of protoplanets themselves. Transition disks, protoplanetary disks with inner clearings that may be caused by forming planets, are the best targets for these studies. Their large distances, compared to the stars normally targeted for direct imaging of exoplanets, make protoplanet detection difficult and necessitate novel imaging techniques. In this dissertation, I describe the results of using non-redundant masking (NRM) to search for forming planets in transition disk clearings. I first present a data reduction pipeline that I wrote to this end, using example datasets and simulations to demonstrate reduction and imaging optimizations. I discuss two transition disk NRM case studies: T Cha and LkCa 15. In the case of T Cha, while we detect significant asymmetries, the data cannot be explained by orbiting companions. The fluxes and orbital motion of the LkCa 15 companion signals, however, can be naturally explained by protoplanets in the disk clearing. I use these datasets and simulated observations to illustrate the effects of scattered light from transition disk material on NRM protoplanet searches. I then demonstrate the utility of the dual-aperture Large Binocular Telescope Interferometer's NRM mode on the bright B[e] star MWC 349A. I discuss the implications of this work for planet formation studies as well as future prospects for NRM and related techniques on next generation instruments.

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Fukue, Tsubasa. "Polarimetric Study of Star/Planet-Forming Regions." 京都大学 (Kyoto University), 2009. http://hdl.handle.net/2433/124422.

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Leftwich, Timothy E. "Geophysical investigations of the crustal structure and evolution of Mars." Columbus, Ohio : Ohio State University, 2006. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1147893346.

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BARLOW, NADINE GAIL. "RELATIVE AGES AND THE GEOLOGIC EVOLUTION OF MARTIAN TERRAIN UNITS (MARS, CRATERS)." Diss., The University of Arizona, 1987. http://hdl.handle.net/10150/184013.

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Existing martian relative age chronologies rely entirely or predominantly on Mariner 9 images, extrapolated numbers of craters, and craters 500(DEGREES)K) for the planet are consistent with the derived chronology.

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Chilcote, Jeffrey, Laurent Pueyo, Robert J. De Rosa, Jeffrey Vargas, Bruce Macintosh, Vanessa P. Bailey, Travis Barman, et al. "1–2.4 μm Near-IR Spectrum of the Giant Planet β Pictoris b Obtained with the Gemini Planet Imager." IOP PUBLISHING LTD, 2017. http://hdl.handle.net/10150/623806.

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Using the Gemini Planet Imager located at Gemini South, we measured the near-infrared (1.0-2.4 mu m) spectrum of the planetary companion to the nearby, young star beta. Pictoris. We compare the spectrum obtained with currently published model grids and with known substellar objects and present the best matching models as well as the best matching observed objects. Comparing the empirical measurement of the bolometric luminosity to evolutionary models, we find a mass of 12.9. +/- 0.2. M-Jup, an effective temperature of 1724. +/- 15 K, a radius of 1.46. +/- 0.01. R-Jup, and a surface gravity of log g = 4.18. 0.01 [dex] (cgs). The stated uncertainties are statistical errors only, and do not incorporate any uncertainty on the evolutionary models. Using atmospheric models, we find an effective temperature of 1700-1800 K and a surface gravity of log g = 3.5-4.0 [dex] depending upon the model. These values agree well with other publications and with "hot-start" predictions from planetary evolution models. Further, we find that the spectrum of beta Pic. b best matches a low surface gravity L2. +/- 1 brown dwarf. Finally, comparing the spectrum to field brown dwarfs, we find the the spectrum best matches 2MASS J04062677- 381210 and 2MASS J03552337 + 1133437.

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Morrison, Sarah J., and Kaitlin M. Kratter. "ORBITAL STABILITY OF MULTI-PLANET SYSTEMS: BEHAVIOR AT HIGH MASSES." IOP PUBLISHING LTD, 2016. http://hdl.handle.net/10150/621257.

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In the coming years, high-contrast imaging surveys are expected to reveal the characteristics of the population of wide-orbit, massive, exoplanets. To date, a handful of wide planetary mass companions are known, but only one such multi-planet system has been discovered: HR 8799. For low mass planetary systems, multi-planet interactions play an important role in setting system architecture. In this paper, we explore the stability of these high mass, multi-planet systems. While empirical relationships exist that predict how system stability scales with planet spacing at low masses, we show that extrapolating to super-Jupiter masses can lead to up to an order of magnitude overestimate of stability for massive, tightly packed systems. We show that at both low and high planet masses, overlapping mean-motion resonances trigger chaotic orbital evolution, which leads to system instability. We attribute some of the difference in behavior as a function of mass to the increasing importance of second order resonances at high planet-star mass ratios. We use our tailored high mass planet results to estimate the maximum number of planets that might reside in double component debris disk systems, whose gaps may indicate the presence of massive bodies.

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Picogna, Giovanni. "Planet formation in binary star systems and its relevance during target selection for extrasolar planet search with the transit method." Doctoral thesis, Università degli studi di Padova, 2014. http://hdl.handle.net/11577/3424033.

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In this Thesis I have studied the impact of binary stars on planet formation and evolution in order to maximize the process of target selection in a future space mission devoted to planet detection. The impact has been firstly addressed via a statistical analysis of the frequency and characteristics of planets in those complex systems. Then, a more in-depth investigation has been made by modeling different planet formation stages in circumbinary and circumstellar environments. I have also studied the impact of close stellar encounters on the evolution of planetary systems in order to explore the relevance of this effect on the statistics of exoplanet mass and orbital distributions. According to the outcome of my simulations the presence of the companion star has a strong impact on planet formation and evolution process. The protoplanetary disk is strongly perturbed, exhibiting tidal waves and developing an overall eccentric shape. In the third dimension hydraulic jumps are observed that could prevent the dust sedimentation and halt the planetesimal formation. In circumbinary disks, the planetesimal evolution appears strongly affected by the asimmetry of the gravitational field of the eccentric disk, that excites mutual planetesimal velocities, favouring fragmentation rather than accretion, thus preventing planet formation. All these effects together influence the overall statistics of planets in binaries and must be taken into account when deriving the general properties of exoplanet systems since the majority of stars are born in multiple configurations, and nearly half of the them are part of a binary system in the Galactic field. Planets in binaries are expected to be a frequent and interesting occurrence and will have a high impact on the target selection process. Future space missions will for sure improve our statistic of these planetary systems, and allow a better understanding of the complex process of planet formation in these esotic environments.
In questa tesi ho studiato l'impatto della binarietà sulla formazione ed evoluzione planetaria allo scopo di massimizzare il processo di selezione dei target in una futura missione spaziale dedicata alla scoperta di transiti planetari. L'impatto è stato studiato prima con un'analisi statistica della frequenze e delle caratteristiche dei pianeti in questi sistemi complessi. In seguito, si è eseguito uno studio più dettagliato dalla modellizzazione di diversi scenari di formazione planetaria in sistemi circumbinari e circumstellari in binarie. Inoltre, ho studiato l'impatto dei flyby stellari sull'evoluzione dei sistemi planetari per capire la rilevanza di questo fenomeno sulla distribuzione statistica della massa e dei parametri orbitali dei pianeti extrasolari osservati. Dal risultato delle simulazioni effettuate, la presenza della compagna stellare nel sistema binario ha un forte impatto sul processo di formazione ed evoluzione dei sistemi planetari. I dischi protoplanetari sono fortemente perturbati, mostrando delle onde mareali e sviluppando una forma eccentrica. Nella terza dimensione si osservano dei salti idraulici che possono prevenire la sedimentazione e bloccare il processo di formazione planetaria. Nei dischi circumbinari, l'evoluzione dei planetesimi appare fortemente influenzata dall'asimmetria del campo gravitazionale del disco eccentrico, portando ad un incremento delle velocità mutue e favorendo la frammentazione piuttosto che l'accrescimento in protopianeti. Tutti questi effetti influenzano la statistica dei pianeti in binarie e devono essere presi in considerazione quando si vuole derivare le proprietà generali dei sistemi planetari, poiché la maggior parte delle stelle si è formata in configurazioni multiple e circa la metà di esse nel campo galattico è parte di un sistema binario. Ci si aspetta che i pianeti in binarie siano un evento frequente ed interessante e dunque abbiano un impatto notevole nel processo di selezione dei target. Le missioni spaziali future sicuramente miglioreranno la statistica di questi sistemi planetari, e permetteranno una più profonda comprensione dei complessi processi di formazione planetaria in questi ambienti esotici.

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Dissertations / Theses on the topic 'PlaNet'

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