Tesis sobre el tema "Scalar field cosmology"
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Castro, Fábio Chibana de. "Tachyon Scalar Field Cosmology". Universidade de São Paulo, 2017. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-17052017-063702/.
Texto completoNeste trabalho testamos um modelo cosmológico com uma interação entre energia escura e matéria escura, onde um campo escalar taquiônico desempenha o papel da energia escura. Para isso, desenvolvemos um código computacional que resolve as equações numericamente e vincula os parâmetros cosmológicos e, assim, comparamos os resultados do modelo taquiônico interagente com os de outros candidatos à energia escura. Nossas análises mostram que o modelo, de fato, consegue explicar os dados observacionais, além de possuir propriedades cosmológicas interessantes, mas apresenta dificuldades quando comparado a outros modelos de energia escura.
Westmoreland, Shawn. "Energy conditions and scalar field cosmology". Kansas State University, 2013. http://hdl.handle.net/2097/15811.
Texto completoDepartment of Physics
Bharat Ratra
In this report, we discuss the four standard energy conditions of General Relativity (null, weak, dominant, and strong) and investigate their cosmological consequences. We note that these energy conditions can be compatible with cosmic acceleration provided that a repulsive cosmological constant exists and the acceleration stays within certain bounds. Scalar fields and dark energy, and their relationships to the energy conditions, are also discussed. Special attention is paid to the 1988 Ratra-Peebles scalar field model, which is notable in that it provides a physical self-consistent framework for the phenomenology of dark energy. Appendix B, which is part of joint-research with Anatoly Pavlov, Khaled Saaidi, and Bharat Ratra, reports on the existence of the Ratra-Peebles scalar field tracker solution in a curvature-dominated universe, and discusses the problem of investigating the evolution of long-wavelength inhomogeneities in this solution while taking into account the gravitational back-reaction (in the linear perturbative approximation).
Kujat, Jens. "Scalar fields in cosmology". Columbus, Ohio : Ohio State University, 2006. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1142978764.
Texto completoLaycock, Andrew Mark. "Aspects of non-minimally coupled scalar field cosmology". Thesis, University of Sussex, 1995. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.282083.
Texto completoGraham, Alexander Alan Hewetson. "Scalar fields in cosmology and black holes". Thesis, University of Cambridge, 2016. https://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.709524.
Texto completoParsons, Paul. "Scalar-field models of the early universe". Thesis, University of Sussex, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.390077.
Texto completoLeith, Ben Maitland. "Scalar Fields and Alternatives in Cosmology and Black Holes". Thesis, University of Canterbury. Physics and Astronomy, 2007. http://hdl.handle.net/10092/1444.
Texto completoBertacca, Daniele. "Unified Dark Matter in Scalar Field Cosmologies". Doctoral thesis, Università degli studi di Padova, 2008. http://hdl.handle.net/11577/3425159.
Texto completoFoster, Scott. "Singularity structure of scalar field cosmologies /". Title page, contents and abstract only, 1996. http://web4.library.adelaide.edu.au/theses/09PH/09phf757.pdf.
Texto completoRossi, Massimo. "Dark energy as a scalar field non-minimally coupled to gravity". Master's thesis, Alma Mater Studiorum - Università di Bologna, 2017. http://amslaurea.unibo.it/12825/.
Texto completoSamushia, Lado. "Constraining scalar field dark energy with cosmological observations". Diss., Manhattan, Kan. : Kansas State University, 2009. http://hdl.handle.net/2097/1524.
Texto completoGordon, Christopher. "Adiabatic and entropy perturbations in cosmology". Thesis, University of Portsmouth, 2001. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.369474.
Texto completoLyons, Glenn. "Time asymmetry". Thesis, University of Cambridge, 1993. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.309076.
Texto completoGENGO, MASSIMO MANUEL. "INTEGRABLE MULTIDIMENSIONAL COSMOLOGIES WITH MATTER AND A SCALAR FIELD". Doctoral thesis, Università degli Studi di Milano, 2019. http://hdl.handle.net/2434/613446.
Texto completoMetcalf, Thomas Patrick. "Dissipative effects in the Early Universe". Thesis, University of Edinburgh, 2015. http://hdl.handle.net/1842/15863.
Texto completoWilhelm, Söderkvist Vermelin. "3+1 Approach to Cosmological Perturbations : Deriving the First Order Scalar Perturbations of the Einstein Field Equations". Thesis, Karlstads universitet, Fakulteten för hälsa, natur- och teknikvetenskap (from 2013), 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:kau:diva-43257.
Texto completoAshcroft, P. R. "Cosmology with scalar fields". Thesis, University of Cambridge, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.596177.
Texto completoEscobal, Anderson Almeida. "Matéria escura como campo escalar : aspectos teóricos e observacionais /". Guaratinguetá, 2020. http://hdl.handle.net/11449/192424.
Texto completoResumo: Estudamos o campo escalar real como um possível candidato para explicar a matéria escura no universo. No contexto de um campo escalar livre com potencial quadrático, após encontrar as equações dinâmicas do modelo usamos os dados observacionais para limitar os parâmetros livres e assim encontrar um limite inferior para o valor da massa que foi da ordem de $10^{-34}$eV, esse valor está próximo ao encontrado por alguns autores. Não foi possível encontrar um limite superior para a massa da matéria escura do campo escalar combinando os dados de $H(z)$, SN Ia. Como verificado neste trabalho e observado em outros estudos, a matéria escura pode ser descrita por um campo escalar real. Em outra linha de pesquisa, usando um método estatístico não-paramétrico envolvendo os chamados Processos Gaussianos, obtivemos um valor do redshift de transição, $z_t$, de $z_t = 0.59^{+0.12}_{-0.11}$ para dados de $H(z)$ e $z_t= 0.683^{+0.11}_{-0.082}$ para dados de SNs Ia.
Abstract: We studied the real scalar field as a possible candidate to explain the dark matter in the universe. In the context of a free scalar field with quadratic potential, after finding the dynamic equations of the model we used the observational data to limit the free parameters and thus find a lower limit for the mass value that was in the order of 10−34 eV , this value is close to that found by some authors. It was not possible to find an upper limit for the mass of dark matter in the scalar field by combining the H(z) + SNe Ia data. As verified in this work and observed in other studies, dark matter can be described by a real scalar field. In another line of research, using a non-parametric statistical method involving the so-called Gaussian Processes, we obtained a value of the transition redshift, zt , of zt = 0.59+0.12 −0.11 for H(z) data and zt = 0.683+0.11 −0.082 for SNs Ia data.
Mestre
Gundlach, C. "Classical and quantum scalar fields in cosmology". Thesis, University of Cambridge, 1992. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.240140.
Texto completoEasther, Richard John Maddock. "The evolution of scalar fields and inflationary cosmology". Thesis, University of Canterbury. Physics, 1993. http://hdl.handle.net/10092/8058.
Texto completoNunes, Nelson. "Attractor solutions in cosmology and particle physics". Thesis, University of Sussex, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.247958.
Texto completoPerrotta, Francesca. "Cosmologies with a Dynamical Vacuum Energy". Doctoral thesis, SISSA, 2000. http://hdl.handle.net/20.500.11767/4331.
Texto completoBartrum, Sam John Richard. "Scalar fields : fluctuating and dissipating in the early Universe". Thesis, University of Edinburgh, 2015. http://hdl.handle.net/1842/11760.
Texto completoSANTOS, Maria Aparecida dos. "Modelos de campos escalares no estudo da cosmologia inflacionária". Universidade Federal de Campina Grande, 2014. http://dspace.sti.ufcg.edu.br:8080/jspui/handle/riufcg/2021.
Texto completoMade available in DSpace on 2018-10-18T19:17:48Z (GMT). No. of bitstreams: 1 MARIA APARECIDA DOS SANTOS – DISSERTAÇÃO (PPGFísica) 2014.pdf: 628300 bytes, checksum: be5188c733755263bec183578258ca27 (MD5) Previous issue date: 2014-02
Capes
Considerando as diferentes abordagens possíveis referentes ao Universo, este trabalho está voltado para o estudo da Cosmologia Padrão e Inflacionária utilizando campos escalares para descrever a fase de expansão acelerada do Universo. Assim, através da Teoria da Gravitação proposta pela Relatividade Geral é possível determinar as equações de Friedmann e utilizando a Teoria de Campos em Cosmologia podemos obter uma equação de movimento que descreve a evolução temporal de um campo escalar chamado ínflaton, responsável pela inflação. Nesse sentido, propomos como alternativa a utilização de alguns modelos de potenciais já existentes, dentre os quais: V ( ) =12m2 2 (quadr atico), V ( ) = C cos2 (tipo cosseno), V ( ) = C sin2 (tipo seno), V ( ) = (t) 4 e o potencial constante V = V0. Buscando dessa forma descrever a evolução temporal do fator de escala a(t) e o comportamento do parâmetro de desaceleração q(t) com o objetivo de analisar a fase inflacionária, identi cando regiões de aceleração e desaceleração do Universo nos cenários dos espaços plano e curvo.
Taking into consideration the set of di erent approaches to the Universe existent today this work focuses on standard cosmology and in ationary expansion of the said using scalar elds to describe the expansion acceleration rate. Therefore, through a gravitation theory proposed by General Relativity is possible to set Friedmann`s equations and using Field Theory applied to Cosmology to obtain an equation of motion which describes the temporal evolution of a scalar eld called in action, which is responsible for the in ationary process. In this sense, we propose as alternative some models whose potentials are already established, among them: V ( ) = 12m2 2 (quadratic), V ( ) = C cos2 (cosinelike) , V ( ) = C sin2 (sinelike), V ( ) = (t) 4 and the constant potential V = V0 . We seek with this to describe the temporal evolution of the scale factor a(t) and how the decelerating parameter behaves and then analyze the in ationary faze, indentifying periods when the Universe was accelerating or decelerating given curve or plane space scenarios.
Radermacher, Katharina Maria. "Strong Cosmic Censorship and Cosmic No-Hair in spacetimes with symmetries". Doctoral thesis, KTH, Matematik (Avd.), 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-220400.
Texto completoDenna avhandling består av tre artiklar som undersöker det asymptotiska beteendet hos kosmologiska rumstider med symmetrier som uppstår i Matematisk Allmän Relativitetsteori. I Artikel A och B studerar vi rumstider med Bianchi symmetri och där materiemodellen är en ideal fluid. Vi undersöker beteendet av sådana rumstider nära ursprungssingulariteten ('Big Bang'). I Artikel A bevisar vi att den Starka Kosmiska Censur-förmodan håller för icke-exceptionella Bianchi klass B-rumstider. Med hjälp av expansions-normaliserade variabler visar vi detaljerade asymptotiska uppskattningar. I Artikel B visar vi liknande uppskattningar för stela fluider. I Artikel C betraktar vi T2-symmetriska rumstider som uppfyller Einsteins ekvationer för ett icke-linjärt skalärfält. För givna begynnelsedata visar vi global existens och entydighet av lösningar till motsvarande differentialekvationer för all framtid. I det speciella fallet med en konstant potential, en situation som motsvarar ett linjärt skalärfält på en bakgrund med en positiv kosmologisk konstant, undersöker vi i detalj det asymptotiska beteendet mot framtiden. Vi visar att den Kosmiska Inget-Hår-förmodan håller för lösningar som uppfyller en ytterligare a priori uppskattning, en uppskattning som vi visar gäller i T3-Gowdy-symmetri.
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Ma, Yin-Zhe. "Cosmology with CMB and large scale structure". Thesis, University of Cambridge, 2011. https://www.repository.cam.ac.uk/handle/1810/239394.
Texto completoValente, Ema Filipa dos Santos. "A simple model of exotic compact objects : interaction with a scalar field". Master's thesis, Universidade de Aveiro, 2017. http://hdl.handle.net/10773/23655.
Texto completoModelos de objetos compactos exóticos (OCEs) foram propostos nas últimas décadas como alternativas aos buracos negros. Esses modelos visam reproduzir a fenomenologia que caracteriza os (candidatos a) buracos negros observados. No entanto, para superar os problemas associados ao horizonte de eventos (e à consequente singularidade de curvatura, de acordo com o teorema de Penrose), estes OCEs não possuem horizonte de eventos. Nesta dissertação, exploramos um modelo simples de um OCE, descrito pela métrica de Kerr-Newman no exterior de uma superfície com condições de fronteira reflectivas, localizada fora do horizonte de eventos de Kerr-Newman. Nesta geometria, estudamos OCEs que podem estar em equilíbrio com con figurações estáticas de um campo escalar. Consideramos um campo escalar sem massa, tanto no caso eletricamente não carregado como no caso carregado, e obtemos, através de métodos analíticos, um conjunto discreto de raios críticos da superfície do OCE que podem suportar con figurações estáticas não triviais do campo escalar. Dentro deste conjunto discreto, o OCE com maior raio crítico separa os OCEs estáveis e instáveis relativamente à instabilidade superradiante, induzida por um campo escalar. O conjunto discreto de raios críticos da superfície do OCE foi construído para os três regimes diferentes da métrica de Kerr-Newman: regime sub-extremo, regime extremo e regime super-extremo. Estes espectros de ressonância dependem dos parâmetros físicos {a, Q, q, l,m }
Models of exotic compact objects (ECOs) have been proposed in the past decades as alternatives to black holes. These models aim at reproducing the phenomenology that characterises the observed black hole (candidates). However, to overcome the problems associated to the event horizon (and the consequent curvature singularity, following from Penrose's singularity theorem), these ECOs do not possess an event horizon. In this thesis, we explore a simple ECO model, described by the Kerr-Newman metric in the exterior of a surface wherein re ective boundary conditions are imposed, placed outside the event horizon of the Kerr-Newman geometry. We then study, on this geometry, ECOs that may be in equilibrium with static scalar eld con- gurations. We consider both electrically charged and uncharged massless scalar elds, and, using analytical methods, we obtain a discrete set of critical ECO surface radii that can support static scalar eld con gurations. Within this discrete set, the ECO with the largest critical surface radius separates stable and unstable Kerr-Newman-type ECOs against the superradiant instability induced by a scalar eld. The discrete set of ECO critical surface radii was constructed for three di erent regimes of the Kerr-Newman metric: sub-extremal regime, extremal regime and super-extremal regime. These resonance spectra are dependent on the physical parameters {a,Q,q,l,m}
Feix, Martin. "Extragalactic and cosmological tests of gravity theories with additional scalar or vector fields". Thesis, University of St Andrews, 2011. http://hdl.handle.net/10023/1901.
Texto completoRubira, Henrique. "Melhorias na predição da estrutura de larga escala do universo por meio de teorias efetivas de campo". Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-08102018-145202/.
Texto completoWith future cosmological surveys, cosmology will enter in the precision era. New data will improve the constraints on the standard cosmological model enhancing our knowledge about the universe history, its components and the behavior of gravity. In this context, it is vital to come up with precise theoretical predictions for the formation of large-scale structure beyond the linear regime. The best way of solving the fluid equations that describe the large-scale universe is through lattice simulations, which faces difficulties in the inclusion of accurate baryonic physics and is very computationally costly. Another approach is the theoreti- cal calculation of the correlation statistics through the perturbative approach, called Standard Perturbation Theory (SPT). However, SPT has several problems: for some cosmologies, it may not converge and even when it converges, we cannot be sure it converges to the right result. Also, it contains a special scale that is the loop momenta upper-bound in the integral. In this work, we show results for the 3-loop calculation. The term of third order is larger than the terms of 2-loops and 3-loops, making explicit SPT problems. In this work, we describe the recent usage of Effective Field Theories (EFTs) on Large Scale Structure problems to correct SPT issues and complement cosmological simulations. EFTs are used in other areas of physics, such as low energy QCD, serving as a complement to lattice calculations. EFT improves the predictions for the matter power spectrum and bispectrum by adding counterterms that need to be fitted. The free parameters, instead of being a problem, bring relevant information about how the small-scale physics affects the scales for which we are trying to make statistical predictions. We show the calculation of the 3-loop EFT counterterms. EFTs are also used to explain main points connecting the matter density field with tracers like galaxies and halos. EFTs highlighted how to construct a complete basis of operators that parametrize the bias. We explain how we can use EFT to improve the bias prediction to non-linear scales. We compute the non-linear halo-bias by fitting the bias parameters in simulations. We also show the EFT renormalization in Lagrangian coordinates. Finally, we explain another critical EFT application to cosmology: in primordial physics. It can be used to parametrize deviations to the slow-roll theory within the inflationary paradigm.
Santos, José Jamilton Rodrigues dos. "Tópicos em cosmologia com campos escalares". Universidade Federal da Paraíba, 2011. http://tede.biblioteca.ufpb.br:8080/handle/tede/5695.
Texto completoCoordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES
Cosmological models involving scalar fields allow the description of a phase of accelerated cosmic expansion and thus appear as a promising alternative for the study of the cosmic inflation and dark energy. We are interested here in analyzing these cosmological models. In particular, we will explore cosmological solutions based on the first order formalism. The inclusion of this method favors the search for analytic solutions with scalar fields in cosmology, and this is particularly important when we consider the component of nonrelativistic matter (dust) in the presence of dark energy, in order to construct a cosmological model capable of explaining, in good agreement with observational data, the current phase of cosmic acceleration. Considering a regime of Lorentz violation, the use of this method allowed us to verify that new considerations must be implemented so that the inflationary regime can now solve the problem of initial conditions. Another question of interest, which can be addressed with the aid of the first order formalism, takes into account the possibility of the dark energy equation of state parameter to be a constant other than −1 and in this case we get that a lot of fine-tuning is needed, which should be interpreted as strong evidence in favor of a dynamic model of dark energy. We also introduce the so-called deformation method on the slow-roll inflationary models, and we explore this framework in applications of current interest to this branch of research.
Modelos cosmológicos envolvendo campos escalares permitem a descrição de uma fase de expansão cósmica acelerada e, portanto, se apresentam como uma alternativa promissora no estudo da inflação cósmica e da energia escura. Estamos aqui interessados em analisar esses modelos cosmológicos; em especial, vamos explorar soluções cosmológicas baseadas no formalismo de primeira ordem. A inclusão desse método favorece a busca por soluções analíticas na cosmologia com campos escalares e isso é particularmente interessante no caso em que consideramos o componente de matéria não relativística (poeira) na presença da energia escura, afim de construir um modelo cosmológico capaz de explicar, em bom acordo com os dados observacionais, a atual fase de aceleração cósmica. Considerando um regime de violação de Lorentz, a utilização desse método nos permitiu verificar que novas considerações devem ser implementadas, para que o regime inflacionário possa resolver o problema das condições iniciais. Outra questão de interesse, que pode ser analisada com auxílio do formalismo de primeira ordem, leva em conta a possibilidade da equação de estado da energia escura ser um constante qualquer diferente de −1 e, nesse caso, obtemos que uma grande quantidade de ajuste fino é necessária, o que deve ser interpretado como uma forte evidência em favor de um modelo dinâmico de energia escura. Também introduzimos o chamado método de deformação a modelos inflacionários sob o regime de rolagem lenta e exploramos essa ferramenta em aplicações de corrente interesse na literatura.
MANCARELLA, MICHELE. "An effective description of dark energy: from theory to phenomenology (titolo originale: Consistency tests of the Universe and cosmic relics)". Doctoral thesis, Université Paris-Saclay, 2017. https://hdl.handle.net/10281/400827.
Texto completoMartineau, Killian. "Quelques aspects de cosmologie et de physique des trous noirs en gravitation quantique à boucles Detailed investigation of the duration of inflation in loop quantum cosmology for a Bianchi I universe with different inflaton potentials and initial conditions Some clarifications on the duration of inflation in loop quantum cosmology A first step towards the inflationary trans-Planckian problem treatment in loop quantum cosmology Scalar spectra of primordial perturbations in loop quantum cosmology Phenomenology of quantum reduced loop gravity in the isotropic cosmological sector Primordial Power Spectra from an Emergent Universe: Basic Results and Clarifications Fast radio bursts and the stochastic lifetime of black holes in quantum gravity Quantum fields in the background spacetime of a polymeric loop black hole Quasinormal modes of black holes in a toy-model for cumulative quantum gravity Seeing through the cosmological bounce: Footprints of the contracting phase and luminosity distance in bouncing models Dark matter as Planck relics without too exotic hypotheses A Status Report on the Phenomenology of Black Holes in Loop Quantum Gravity: Evaporation, Tunneling to White Holes, Dark Matter and Gravitational Waves". Thesis, Université Grenoble Alpes (ComUE), 2019. http://www.theses.fr/2019GREAY044.
Texto completoAfter decades of being confined to mathematical physics, quantum gravity now enters the field of experimental science. Following this trend, we consider throughout this thesis three implementation frameworks of Loop Quantum Gravity (LQG): the Universe as a system, black holes and astroparticles. The last one is only outlined while the first two are presented in more detail.Since the cosmological sector is one of the most promising areas for testing and constraining quantum gravity theories, it was not long before the development of different models attempting to apply the ideas of the LQG to the primordial Universe. The work we present deals with the phenomenology associated with these models; both in the homogeneous sector (where we focus particularly on the duration of the inflation phase), as in the inhomogeneous sector (where this time, we study the fate of the primordial power spectra). These combined studies then allow us to specify to what extent effects of (loop) quantum gravity can be observed in the anisotropies of the cosmic microwave background.On the other hand black holes, not content to be among the strangest and most fascinating objects of the Universe, are also prominent probes to test the theories of gravitation. We develop the phenomenology associated with different treatments of black holes in the loop quantum gravity framework, which intervenes on multiple levels: from the evaporation of Hawking to gravitational waves, including dark matter. This is undoubtedly a rich and vast area.Finally, the existence of a minimal length scale, predicted by the majority of quantum gravity theories, suggests a generalization of the Heisenberg uncertainty principle. On the basis of this observation, we also present in this manuscript a methodology to derive a new relation dispersion of light from the most widely used generalized uncertainty principle
Di, Nella Hélène. "Structure et cinématique de l'univers local". Université Joseph Fourier (Grenoble), 1995. http://www.theses.fr/1995GRE10220.
Texto completoWallisch, Benjamin. "Cosmological probes of light relics". Thesis, University of Cambridge, 2018. https://www.repository.cam.ac.uk/handle/1810/283003.
Texto completoHrycyna, Orest. "Regular and chaotic dynamics in scalar field cosmology". Praca doktorska, 2011. https://ruj.uj.edu.pl/xmlui/handle/item/53490.
Texto completoLi, Bohua. "Cosmology with Bose-Einstein-condensed scalar field dark matter". 2013. http://hdl.handle.net/2152/21308.
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Foster, Scott. "Singularity structure of scalar field cosmologies / Scott Foster". Thesis, 1996. http://hdl.handle.net/2440/18744.
Texto completoBibliography: p. 173-177.
x, 177 p. : ill. ; 30 cm.
The classical dynamical structure of cosomological models in which the matter content of the universe consists of a scalar field with arbitrary non-negative potential is analyzed in full. (abstract)
Thesis (Ph.D.)--University of Adelaide, Dept. of Physics and Mathematical Physics, 1996?
Ahmed, Aqeel. "Scalar fields within warped extra dimension". Doctoral thesis, 2015. https://depotuw.ceon.pl/handle/item/1277.
Texto completoChatwin-Davies, Aidan. "A Covariant Natural Ultraviolet Cutoff in Inflationary Cosmology". Thesis, 2013. http://hdl.handle.net/10012/7759.
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