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Artykuły w czasopismach na temat "Dark energy models"
POLARSKI, DAVID. "DARK ENERGY". International Journal of Modern Physics D 22, nr 14 (grudzień 2013): 1330027. http://dx.doi.org/10.1142/s0218271813300279.
Pełny tekst źródłaMotta, Verónica, Miguel A. García-Aspeitia, Alberto Hernández-Almada, Juan Magaña i Tomás Verdugo. "Taxonomy of Dark Energy Models". Universe 7, nr 6 (26.05.2021): 163. http://dx.doi.org/10.3390/universe7060163.
Pełny tekst źródłaKhurshudyan, Martiros, i Asatur Khurshudyan. "Some Interacting Dark Energy Models". Symmetry 10, nr 11 (2.11.2018): 577. http://dx.doi.org/10.3390/sym10110577.
Pełny tekst źródłaTawfik, Abdel Nasser, i Eiman Abou El Dahab. "Review on Dark Energy Models". Gravitation and Cosmology 25, nr 2 (kwiecień 2019): 103–15. http://dx.doi.org/10.1134/s0202289319020154.
Pełny tekst źródłaSahni, Varun, i Yuri Shtanov. "Braneworld models of dark energy". Journal of Cosmology and Astroparticle Physics 2003, nr 11 (24.11.2003): 014. http://dx.doi.org/10.1088/1475-7516/2003/11/014.
Pełny tekst źródłaSahni, Varun. "Theoretical models of dark energy". Chaos, Solitons & Fractals 16, nr 4 (maj 2003): 527–37. http://dx.doi.org/10.1016/s0960-0779(02)00221-7.
Pełny tekst źródłaYOO, JAEWON, i YUKI WATANABE. "THEORETICAL MODELS OF DARK ENERGY". International Journal of Modern Physics D 21, nr 12 (listopad 2012): 1230002. http://dx.doi.org/10.1142/s0218271812300029.
Pełny tekst źródłaChan, R., M. F. A. da Silva i Jaime F. Villas da Rocha. "Star models with dark energy". General Relativity and Gravitation 41, nr 8 (29.01.2009): 1835–51. http://dx.doi.org/10.1007/s10714-008-0755-9.
Pełny tekst źródłaArun, Kenath, S. B. Gudennavar, A. Prasad i C. Sivaram. "Alternate models to dark energy". Advances in Space Research 61, nr 1 (styczeń 2018): 567–70. http://dx.doi.org/10.1016/j.asr.2017.08.006.
Pełny tekst źródłaPearson, Jonathan A. "Material models of dark energy". Annalen der Physik 526, nr 7-8 (10.06.2014): 318–39. http://dx.doi.org/10.1002/andp.201400052.
Pełny tekst źródłaRozprawy doktorskie na temat "Dark energy models"
Elmufti, Mohammed. "Perturbations of dark energy models". Thesis, University of Western Cape, 2012. http://hdl.handle.net/11394/3386.
Pełny tekst źródłaThe growth of structure in the Universe proceeds via the collapse of dark matter and baryons. This process is retarded by dark energy which drives an accelerated expansion of the late Universe. In this thesis we use cosmological perturbation theory to investigate structure formation for a particular class of dark energy models, i.e. interacting dark energy models. In these models there is a non-gravitational interaction between dark energy and dark matter, which alters the standard evolution (with non-interacting dark energy) of the Universe. We consider a simple form of the interaction where the energy exchange in the background is proportional to the dark energy density. We analyse the background dynamics to uncover the e ect of the interaction. Then we develop the perturbation equations that govern the evolution of density perturbations, peculiar velocities and the gravitational potential. We carefully account for the complex nature of the perturbed interaction, in particular for the momentum transfer in the dark sector. This leads to two di erent types of model, where the momentum exchange vanishes either in the dark matter rest-frame or the dark energy rest-frame. The evolution equations for the perturbations are solved numerically, to show how structure formation is altered by the interaction.
Duran, Sancho Ivan. "Constraining Cosmological Models of Dark Energy". Doctoral thesis, Universitat Autònoma de Barcelona, 2013. http://hdl.handle.net/10803/125917.
Pełny tekst źródłaNowadays the Universe appears to be undergoing a phase of accelerated expansion, as witnessed by supernovae data and later corroborated by a host a cosmological measurements -very recently by the Planck satellite. While this expansion can be described in Einstein’s theory of gravity by invoking the existence of a positive but exceedingly small cosmological constant, Λ, connected to the quantum vacuum, many alternative, and sometimes sophisticated, explanations have been proposed. Roughly, the energy content of the present universe can be split into 5% of baryonic matter and 95% of a non-visible (dubbed the “dark sector” because its components do not interact electromagnetically) whose 25% consists of non-relativistic, weakly interacting massive particles (“cold dark matter”) and a 75% of a component with a huge negative pressure, the so-called “dark energy”. The nature of the latter component is completely unknown; this justifies that many “trial” candidates have been proposed. By far, the simplest and most successful one is the cosmological constant, mentioned above. However, it suffers from two main drawbacks at the theoretical level: the coincidence problem and the fine tuning problem. The aim of this Memoir is to propose and constrain cosmological models of dark energy that circumvent these difficulties. This Memoir is organized as follows: The Chapters §2, §3 and §4 introduce basic concepts widely used when considering the different models that conforms our research work. The following Chapters focus on the different cosmological models. In §5 dark energy is considered connected to the holographic principle and posits that it interacts (also non-gravitationally) with dark matter. The holographic principle sets a length scale, in this case the Hubble length, i.e., the scale of the causally connected events. In §6 the previous model is studied more deeply and an alternative to it is presented. Both models share identical background evolution but each component behaves differently, which induces a diverse behavior at the perturbative level. This allows to observationally discriminate one model from the other. A further holographic dark energy model is proposed in §7; this one based on the Ricci length (i.e., the maximum size a perturbation can have leading to a black hole). Again, a non-gravitational interaction is assumed between dark energy and dark matter. In §8, a unified dark model (featuring a unification between dark matter ad dark energy) previously proposed is studied. Since the parameter space that fits the observational data is very narrow (and also in view of its theoretical interest), we decompose the single energy component into cold dark matter and quantum vacuum interacting with one another. As a consequence the allowed parameter space gets substantially augmented. Although the models mentioned above mimic at the background level the standard ΛCDM model, the dark components evolve very differently. To rigorously study them, the numerical codes for the cosmological perturbations must be suitably modified, with the drawback of notably increasing the computational time. This is much alleviated in §9 where a novel method to calculate the matter power spectrum of dark energy models is proposed. Finally, in §10 three model independent parameterizations of the deceleration parameter, based on solid thermodynamic arguments, are proposed and contrasted with the observational data.
Tamanini, N. "Dynamical systems in dark energy models". Thesis, University College London (University of London), 2014. http://discovery.ucl.ac.uk/1456304/.
Pełny tekst źródłaCosta, André Alencar da. "Observational Constraints on Models with an Interaction between Dark Energy and Dark Matter". Universidade de São Paulo, 2014. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-20012015-123002/.
Pełny tekst źródłaNesta tese vamos além do modelo cosmológico padrão, o LCDM, e estudamos o efeito de uma interação entre a matéria e a energia escuras. Embora o modelo LCDM esteja de acordo com as observações, ele sofre sérios problemas teóricos. Com o objetivo de resolver tais problemas, nós primeiro consideramos um modelo alternativo, onde ambas, a matéria e a energia escuras, são descritas por fluidos com uma interação fenomenológica dada como uma combinação das densidades de energia. Além desse modelo, propomos um modelo mais realista baseado em uma densidade Lagrangiana com uma interação tipo Yukawa. Para vincular os parâmetros cosmológicos usamos dados cosmológicos recentes como as medidas da CMB feitas pelo satélite Planck, bem como medidas de BAO, SNIa, H0 e Lookback time.
Zsembinszki, Gabriel. "Light scalar fields in a dark universe: models of inflation, dark energy and dark matter". Doctoral thesis, Universitat Autònoma de Barcelona, 2007. http://hdl.handle.net/10803/3390.
Pełny tekst źródłaSegún la cosmología estándar del Big Bang, el universo primitivo consistía en un plasma muy caliente y denso que se expandió y se enfrió continuamente hasta el presente, dando paso a una serie de transiciones de fase cosmológicas, donde las teorías que describen el universo en cada fase son distintas. Dado que las energías del universo primitivo fueron mucho más altas que las alcanzadas en experimentos terrestres, el estudio del universo primitivo podría ofrecernos importantes informaciones sobre nuevas interacciones y nuevas partículas, abriendo nuevas direcciones para la extensión del Modelo Estándar de la física de partículas.
Como ya he mencionado anteriormente, durante la expansión del universo ocurrieron varias transiciones de fase que dejaron su huella sobre el estado presente del universo. Las observaciones sugieren que durante una de estas transiciones de fase, el universo primitivo sufrió un periodo de expansión acelerada, conocido como inflación. Aunque no forma parte de la cosmología estándar, la inflación es capaz de solucionar de una manera simple y elegante casi todos los problemas relacionados con el modelo estándar del Big Bang, y debería tenerse en cuenta en cualquier extensión posible de la teoría. Las observaciones también revelan la existencia de dos formas de energía desconocidas, a saber, materia oscura y energía oscura. La materia oscura es una forma de materia no relativista y no bariónica, que solamente puede ser detectada indirectamente, mediante su interacción con la materia normal. La energía oscura es un tipo de sustancia con presión negativa, que empezó a dominar recientemente y que es la causa de la aceleración de la expansión del universo.
En esta tesis doctoral presento varios modelos originales propuestos para resolver algunos de los problemas de la cosmología estándar, como posibles extensiones del modelo del Big Bang. Algunos de estos modelos introducen nuevas simetrías y partículas con el fin de explicar la inflación y la energía oscura y/o la materia oscura en una descripción unificada. Uno de los modelos es propuesto para explicar la energía oscura del universo, a través de un nuevo campo escalar que oscila en un potencial.
The most successful scientific theory today about the origin and evolution of the universe is known as the standard Big Bang model, which is one of the most ambitious intellectual constructions of the humanity. It is based on two consolidated branches of theoretical physics, namely, the theory of General Relativity and the Standard Model of particle physics, and is able to make robust predictions, such as the expansion of the universe, the existence of the cosmic microwave background radiation and the relative primordial abundance of light elements. Some of the theoretical predictions have already been confirmed by very precise observations.
According to the standard Big Bang cosmology, the early universe consisted of a very hot and dense plasma that continuously expanded and cooled up to the present, giving place to a series of cosmological phase transitions, where the theories describing the universe in each phase are different. Given that the energies of the early universe were much higher than those reached in terrestrial experiments, the study of the early universe might give us important information about new interactions and new particles, opening new directions for extending the Standard Model of particle physics.
As already mentioned above, during the expansion of the universe, different phase transitions occurred, which left their imprint on the present state of the universe. Observations suggest that during a very early phase transition the universe suffered a stage of accelerated expansion, known as inflation. Although inflation is not included in the standard cosmology, it is able to solve in a simple and elegant manner almost all of the shortcomings related to the standard Big Bang model, and should be taken into account in any possible extension of the theory. Observations also reveal evidence of the existence of two unknown forms of energy, i.e., dark matter and dark energy. Dark matter is a form of non-relativistic and non-baryonic matter, which can only be detected indirectly, by its gravitational interactions with normal matter. Dark energy is a kind of substance with negative pressure, which started to dominate recently and causes the accelerated expansion of the universe.
In this PhD Thesis, I present a few original models proposed to solve some of the shortcomings of the standard cosmology, as possible extensions of the Big Bang model. Some of these models introduce new symmetries and particles in order to explain inflation and dark energy and/or dark matter in a unified description. One of the models is proposed for explaining the dark energy of the universe, by means of a new scalar field oscillating in a potential.
The most successful scientific theory today about the origin and evolution of the universe is known as the standard Big Bang model, which is one of the most ambitious intellectual constructions of the humanity. It is based on two consolidated branches of theoretical physics, namely, the theory of General Relativity and the Standard Model of particle physics, and is able to make robust predictions, such as the expansion of the universe, the existence of the cosmic microwave background radiation and the relative primordial abundance of light elements. Some of the theoretical predictions have already been confirmed by very precise observations.
According to the standard Big Bang cosmology, the early universe consisted of a very hot and dense plasma that continuously expanded and cooled up to the present, giving place to a series of cosmological phase transitions, where the theories describing the universe in each phase are different. Given that the energies of the early universe were much higher than those reached in terrestrial experiments, the study of the early universe might give us important information about new interactions and new particles, opening new directions for extending the Standard Model of particle physics.
As already mentioned above, during the expansion of the universe, different phase transitions occurred, which left their imprint on the present state of the universe. Observations suggest that during a very early phase transition the universe suffered a stage of accelerated expansion, known as inflation. Although inflation is not included in the standard cosmology, it is able to solve in a simple and elegant manner almost all of the shortcomings related to the standard Big Bang model, and should be taken into account in any possible extension of the theory. Observations also reveal evidence of the existence of two unknown forms of energy, i.e., dark matter and dark energy. Dark matter is a form of non-relativistic and non-baryonic matter, which can only be detected indirectly, by its gravitational interactions with normal matter. Dark energy is a kind of substance with negative pressure, which started to dominate recently and causes the accelerated expansion of the universe.
In this PhD Thesis, I present a few original models proposed to solve some of the shortcomings of the standard cosmology, as possible extensions of the Big Bang model. Some of these models introduce new symmetries and particles in order to explain inflation and dark energy and/or dark matter in a unified description. One of the models is proposed for explaining the dark energy of the universe, by means of a new scalar field oscillating in a potential.
Mania, Data. "Constraints on dark energy models from observational data". Thesis, Kansas State University, 2012. http://hdl.handle.net/2097/14178.
Pełny tekst źródłaDepartment of Physics
Bharat Ratra
Recent observations in cosmology suggest that the universe is undergoing accelerating expansion. Mysterious component responsible for acceleration is called "Dark Energy" contributing to 70% of total energy density of the universe. Simplest DE model is [Lambda]CDM, where Einstein’s cosmological constant plays role of the dark energy. Despite the fact that it is consistent with observational data, it leaves some important theoretical questions unanswered. To overcome these difficulties different Dark energy models are proposed. Two of these models XCDM parametrization and slow rolling scalar field model [phi]CDM, along with "standard" [Lambda]CDM are disscussed here, constraining their parameter set. In this thesis we start with a general theoretical overview of basic ideas and distance measures in cosmology. In the following chapters we use H II starburst galaxy apparent magnitude versus redshift data from Siegel et al.(2005) to constrain DE model parameters. These constraints are generally consistent with those derived using other data sets, but are not as restrictive as the tightest currently available constraints. Also we constrain above mentioned cosmological models in light of 32 age measurements of passively evolving galaxies as a function of redshift and recent estimates of the product of the cosmic microwave background acoustic scale and the baryon acoustic oscillation peak scale.
Rivera, Echeverri José David [UNESP]. "ISW effect through dark energy quintessence and ΛCDM models". Universidade Estadual Paulista (UNESP), 2013. http://hdl.handle.net/11449/92030.
Pełny tekst źródłaFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
Observações atuais do satélite Wilkinson Microwave Anisotropy Probe (WMAP) da Radiação Cósmica de Fundo (CMB) e estruturas de grande escala (LSS) têm permitido melhorar os estudos das anisotropias secundárias, especialmente o efeito Sachs-Wolfe Integrado (ISW). Usando a correlação cruzada entre a CMB e mapas da LSS, o sinal do efeito ISW pode ser detectado. Nós podemos usar o efeito ISW junto com o modelo cosmológico padrão (neste caso o Universo esta dominado pela constante cosmológica e a Matéria Escura Fria, ΛCDM) mais algoritmos numéricos para restringir os parâmetros em um modelo cosmológico com energia escura. Para diferentes casos com um único parâmetro livre de um model de Quintessência parametrizado,' w IND. 0' < 0 e 2,0 < 'w IND. a' <−2,0, podemos encontrar bins de largura [−1,926,−0,323] em 'w ind. 0' e [−0,855, 1,190]. Nestes intervalos, obtemos um sigma de nivel tomando o 68% da amostra que melhor se ajusta ao modelo cosmológico padrão
Current observations of the Wilkinson Microwave Anisotropy Probe (WMAP) satellite of Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) have allowed to improve studies of the secondary anisotropies, especially the Integrated Sachs-Wolfe effect (ISW). Using the cross-correlation between the CMB and LSS maps, the ISW effect signal can be detected. We can use the ISW effect together with standard cosmological model (in this case the Universe is dominated by the cosmological constant and Cold Dark Matter, ΛCDM) plus numerical algorithms to constrain the parameters in a cosmological model with dark energy. For cases different with a single free parameter of a parameterised Quintessence model, 'w ind. 0' < 0 and 2,0 < 'w ind. a' <−2,0, we can find bins of width [−1,926,−0,323] in 'w ind. 0' and [−0,855, 1,190] in wa. In these intervals, we obtain one sigma level by taking the 68% of the sample which best fit the standard cosmological model
Rivera, Echeverri José David. "ISW effect through dark energy quintessence and ΛCDM models /". São Paulo, 2013. http://hdl.handle.net/11449/92030.
Pełny tekst źródłaCoorientador: Felipe Batoni Abdalla
Banca: Marcos Vinícius Borges Teixeira Lima
Banca: Laerte Sodré Junior
Resumo: Observações atuais do satélite Wilkinson Microwave Anisotropy Probe (WMAP) da Radiação Cósmica de Fundo (CMB) e estruturas de grande escala (LSS) têm permitido melhorar os estudos das anisotropias secundárias, especialmente o efeito Sachs-Wolfe Integrado (ISW). Usando a correlação cruzada entre a CMB e mapas da LSS, o sinal do efeito ISW pode ser detectado. Nós podemos usar o efeito ISW junto com o modelo cosmológico padrão (neste caso o Universo esta dominado pela constante cosmológica e a Matéria Escura Fria, ΛCDM) mais algoritmos numéricos para restringir os parâmetros em um modelo cosmológico com energia escura. Para diferentes casos com um único parâmetro livre de um model de Quintessência parametrizado,' w IND. 0' < 0 e 2,0 < 'w IND. a' <−2,0, podemos encontrar bins de largura [−1,926,−0,323] em 'w ind. 0' e [−0,855, 1,190]. Nestes intervalos, obtemos um sigma de nivel tomando o 68% da amostra que melhor se ajusta ao modelo cosmológico padrão
Abstract: Current observations of the Wilkinson Microwave Anisotropy Probe (WMAP) satellite of Cosmic Microwave Background (CMB) and Large Scale Structure (LSS) have allowed to improve studies of the secondary anisotropies, especially the Integrated Sachs-Wolfe effect (ISW). Using the cross-correlation between the CMB and LSS maps, the ISW effect signal can be detected. We can use the ISW effect together with standard cosmological model (in this case the Universe is dominated by the cosmological constant and Cold Dark Matter, ΛCDM) plus numerical algorithms to constrain the parameters in a cosmological model with dark energy. For cases different with a single free parameter of a parameterised Quintessence model, 'w ind. 0' < 0 and 2,0 < 'w ind. a' <−2,0, we can find bins of width [−1,926,−0,323] in 'w ind. 0' and [−0,855, 1,190] in wa. In these intervals, we obtain one sigma level by taking the 68% of the sample which best fit the standard cosmological model
Mestre
Pavlov, Anatoly. "Constraining competing models of dark energy with cosmological observations". Diss., Kansas State University, 2015. http://hdl.handle.net/2097/20345.
Pełny tekst źródłaDepartment of Physics
Bharat Ratra
The last decade of the 20th century was marked by the discovery of the accelerated expansion of the universe. This discovery puzzles physicists and has yet to be fully understood. It contradicts the conventional theory of gravity, i.e. Einstein’s General Relativity (GR). According to GR, a universe filled with dark matter and ordinary matter, i.e. baryons, leptons, and photons, can only expand with deceleration. Two approaches have been developed to study this phenomenon. One attempt is to assume that GR might not be the correct description of gravity, hence a modified theory of gravity has to be developed to account for the observed acceleration of the universe’s expansion. This approach is known as the ”Modified Gravity Theory”. The other way is to assume that the energy budget of the universe has one more component which causes expansion of space with acceleration on large scales. Dark Energy (DE) was introduced as a hypothetical type of energy homogeneously filling the entire universe and very weakly or not at all interacting with ordinary and dark matter. Observational data suggest that if DE is assumed then its contribution to the energy budget of the universe at the current epoch should be about 70% of the total energy density of the universe. In the standard cosmological model a DE term is introduced into the Einstein GR equations through the cosmological constant, a constant in time and space, and proportional to the metric tensor g[subscript]mu[subscript]nu. While this model so far fits most available observational data, it has some significant conceptual shortcomings. Hence there are a number of alternative cosmological models of DE in which the dark energy density is allowed to vary in time and space.
Weller, Joel Martin. "Models of onflation and dark energy with coupled scalar fields". Thesis, University of Sheffield, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.538088.
Pełny tekst źródłaKsiążki na temat "Dark energy models"
Prime elements of ordinary matter, dark matter & dark energy: Beyond standard model & string theory. Wyd. 2. Boca Raton, FL: Universal Publishers, 2007.
Znajdź pełny tekst źródłaFrom quantum to cosmos: Fundamental physics research in space. Hackensack, N.J: World Scientific, 2009.
Znajdź pełny tekst źródłaE'kov, Evgeniy. The origin and evolution of the Universe. ru: INFRA-M Academic Publishing LLC., 2022. http://dx.doi.org/10.12737/1852616.
Pełny tekst źródłaBlaha, Stephen. The origin of the standard model: The genesis of four quark and lepton species, parity violation, the electro weak sector, color SU(3), three visible generations of fermions, and one generation of dark matter with dark energy ; Quantum theory of the third kind : a new type of divergence-free quantum field theory supporting a unified standard model of elementary particles and quantum gravity based on a new method in the calculus of variations. Auburn, NH: Pingree-Hill Publishing, 2006.
Znajdź pełny tekst źródłaStern, Steffen. Dynamical dark energy and variation of fundamental'constants': A study of experimental probes and theoretical models. Südwestdeutscher Verlag für Hochschulschriften AG & Company KG, 2009.
Znajdź pełny tekst źródłaSaha, Prasenjit, i Paul A. Taylor. The Expanding Universe. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198816461.003.0008.
Pełny tekst źródłaGinzburg, Vladimir. Prime Elements Of Ordinary Matter, Dark Matter & Dark Energy - Beyond Standard Model & String Theory. Lulu.com, 2007.
Znajdź pełny tekst źródłaGinzburg, Vladimir B. Prime Elements of Ordinary Matter, Dark Matter & Dark Energy: Beyond Standard Model & String Theory. Universal Publishers, 2007.
Znajdź pełny tekst źródłaTatum, Eugene Terry, i U. V. S. Seshavatharam. Flat Space Cosmology: A New Model of the Universe Incorporating Astronomical Observations of Black Holes, Dark Energy and Dark Matter. Universal Publishers, 2021.
Znajdź pełny tekst źródłaLander, Enrique. Integral Theory of the Universe: New Model of the Universe, Without Energy or Dark Matter. Independently Published, 2020.
Znajdź pełny tekst źródłaCzęści książek na temat "Dark energy models"
Tsujikawa, S. "Modified Gravity Models of Dark Energy". W Lectures on Cosmology, 99–145. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-10598-2_3.
Pełny tekst źródłaDimopoulos, Konstantinos. "Models of Inflation". W Introduction to Cosmic Inflation and Dark Energy, 137–70. First edition. | Boca Raton : CRC Press, 2020. | Series: Series in astronomy and astrophysics: CRC Press, 2020. http://dx.doi.org/10.1201/9781351174862-7.
Pełny tekst źródłaTsujikawa, Shinji. "Dark Energy: Observational Status and Theoretical Models". W Quantum Gravity and Quantum Cosmology, 289–331. Berlin, Heidelberg: Springer Berlin Heidelberg, 2013. http://dx.doi.org/10.1007/978-3-642-33036-0_11.
Pełny tekst źródłaMacció, A. V., S. A. Bonometto, R. Mainini i A. Klypin. "Structure Formation in Dynamical Dark Energy Models". W Multiwavelength Cosmology, 199–202. Dordrecht: Springer Netherlands, 2004. http://dx.doi.org/10.1007/0-306-48570-2_41.
Pełny tekst źródłaGuendelman, Eduardo, Emil Nissimov i Svetlana Pacheva. "Wheeler–DeWitt Quantization of Gravity Models of Unified Dark Energy and Dark Matter". W Quantum Theory and Symmetries with Lie Theory and Its Applications in Physics Volume 2, 99–113. Singapore: Springer Singapore, 2018. http://dx.doi.org/10.1007/978-981-13-2179-5_7.
Pełny tekst źródłaZakharov, A. F., S. Capozziello, F. De Paolis, G. Ingrosso i A. A. Nucita. "The Role of Dark Matter and Dark Energy in Cosmological Models: Theoretical Overview". W Probing The Nature of Gravity, 353–65. New York, NY: Springer New York, 2009. http://dx.doi.org/10.1007/978-1-4419-1362-3_22.
Pełny tekst źródłaArnowitt, R., B. Dutta i Y. Santoso. "Neutralino Proton Cross Sections for Dark Matter in SUGRA and D-BRANE Models". W Sources and Detection of Dark Matter and Dark Energy in the Universe, 222–35. Berlin, Heidelberg: Springer Berlin Heidelberg, 2001. http://dx.doi.org/10.1007/978-3-662-04587-9_23.
Pełny tekst źródłaStaicova, Denitsa, i Michail Stoilov. "Cosmological Solutions from Models with Unified Dark Energy and Dark Matter and with Inflaton Field". W Quantum Theory and Symmetries with Lie Theory and Its Applications in Physics Volume 2, 251–60. Singapore: Springer Singapore, 2018. http://dx.doi.org/10.1007/978-981-13-2179-5_19.
Pełny tekst źródłaChattopadhyay, Surajit, i Antonio Pasqua. "Consequences of Holographic Scalar Field Dark Energy Models in Chameleon Brans-Dicke Cosmology". W Springer Proceedings in Physics, 487–92. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-25619-1_74.
Pełny tekst źródłaCunillera, Francesc. "Obstructions to Quintessence Model Building". W Dark Energy, 131–70. Cham: Springer Nature Switzerland, 2023. http://dx.doi.org/10.1007/978-3-031-21468-4_8.
Pełny tekst źródłaStreszczenia konferencji na temat "Dark energy models"
Caldwell, Robert R. "Dark Energy Models". W Proceedings of the 2012 Theoretical Advanced Study Institute in Elementary Particle Physics. WORLD SCIENTIFIC, 2013. http://dx.doi.org/10.1142/9789814525220_0001.
Pełny tekst źródłaBesprosvany, Jaime, Germán Izquierdo, Alfredo Macias i Marco Maceda. "Dark-energy thermodynamic models". W RECENT DEVELOPMENTS IN GRAVITATION AND BEC’S PHENOMENOLOGY: IV Mexican Meeting on Experimental and Theoretical Physics: Symposium on Gravitation BEC’s Phenomenology. AIP, 2010. http://dx.doi.org/10.1063/1.3531619.
Pełny tekst źródłaCopeland, Edmund J., Jean-Michel Alimi i André Fuözfa. "Models of Dark Energy". W INVISIBLE UNIVERSE: Proceedings of the Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3462965.
Pełny tekst źródłaGANNOUJI, R., D. POLARSKI, A. RANQUET i A. A. STAROBINSKY. "SCALAR-TENSOR DARK ENERGY MODELS". W Proceedings of the MG11 Meeting on General Relativity. World Scientific Publishing Company, 2008. http://dx.doi.org/10.1142/9789812834300_0259.
Pełny tekst źródłaZimdahl, W. "Models of interacting dark energy". W I COSMOSUL: COSMOLOGY AND GRAVITATION IN THE SOUTHERN CONE. AIP, 2012. http://dx.doi.org/10.1063/1.4756811.
Pełny tekst źródłaChan, R., M. A. F. da Silva, Jaime F. Villas da Rocha, Jean-Michel Alimi i André Fuözfa. "Star Models with Dark Energy". W INVISIBLE UNIVERSE: Proceedings of the Conference. AIP, 2010. http://dx.doi.org/10.1063/1.3462618.
Pełny tekst źródłaGao, Changjun, Yan Gong, Xuelei Chen, Carlo Luciano Bianco i She-Sheng Xue. "Phenomenological Models of dark Energy". W RELATIVISTIC ASTROPHYSICS: 4th Italian-Sino Workshop. AIP, 2008. http://dx.doi.org/10.1063/1.2836987.
Pełny tekst źródłaLazkoz, Ruth, Mauricio Carbajal, Luis Manuel Montaño, Oscar Rosas-Ortiz, Sergio A. Tomas Velazquez i Omar Miranda. "Geometrical Constraints on Dark Energy Models". W Advanced Summer School in Physics 2007. AIP, 2007. http://dx.doi.org/10.1063/1.2825127.
Pełny tekst źródłaChimento, Luis P. "Exactly solved models of interacting dark matter and dark energy". W I COSMOSUL: COSMOLOGY AND GRAVITATION IN THE SOUTHERN CONE. AIP, 2012. http://dx.doi.org/10.1063/1.4756808.
Pełny tekst źródłaKumar, Jason. "WIMPless Dark Matter: Models and Signatures". W 35th International Conference of High Energy Physics. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.120.0438.
Pełny tekst źródłaRaporty organizacyjne na temat "Dark energy models"
Abdallah, Jalal, Adi Ashkenazi, Antonio Boveia, Giorgio Busoni, Andrea De Simone, Caterina Doglioni, Aielet Efrati i in. Simplified Models for Dark Matter and Missing Energy Searches at the LHC. Office of Scientific and Technical Information (OSTI), październik 2014. http://dx.doi.org/10.2172/1304777.
Pełny tekst źródłaBoveia, Antonio, Oliver Buchmueller, Giorgio Busoni, Francesco D' Eramo, Albert De Roeck, Andrea De Simone, Caterina Doglioni i in. Recommendations on presenting LHC searches for missing transverse energy signals using simplified s-channel models of dark matter. Office of Scientific and Technical Information (OSTI), marzec 2016. http://dx.doi.org/10.2172/1255141.
Pełny tekst źródłaFarbin, Amir. DoE Early Career Research Program: Final Report: Model-Independent Dark-Matter Searches at the ATLAS Experiment and Applications of Many-core Computing to High Energy Physics. Office of Scientific and Technical Information (OSTI), lipiec 2015. http://dx.doi.org/10.2172/1193786.
Pełny tekst źródłaVieitez Martínez, Daniel. Introducción a las mejores prácticas de los modelos internacionales de asociaciones público-privadas. Inter-American Development Bank, styczeń 2010. http://dx.doi.org/10.18235/0007604.
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