Thematische Bibliographien / Dark Matter Models / Zeitschriftenartikel
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Zeitschriftenartikel zum Thema „Dark Matter Models“

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Veröffentlicht am 18. Mai 2024

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1

Takibayev, N. „Models of dark particle interactions with ordinary matter“. Physical Sciences and Technology 2, Nr. 2 (2015): 58–69. http://dx.doi.org/10.26577/2409-6121-2015-2-2-58-69.

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2

Morgante, Enrico. „Simplified Dark Matter Models“. Advances in High Energy Physics 2018 (17.12.2018): 1–13. http://dx.doi.org/10.1155/2018/5012043.

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I review the construction of simplified models for dark matter searches. After discussing the philosophy and some simple examples, I turn the attention to the aspect of the theoretical consistency and to the implications of the necessary extensions of these models.
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3

Arnowitt, R., B. Dutta und Y. Santoso. „Dark matter in Susy models“. Physics of Atomic Nuclei 65, Nr. 12 (Dezember 2002): 2218–24. http://dx.doi.org/10.1134/1.1530303.

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4

Arnowitt, R., und Pran Nath. „Models of particle dark matter“. Nuclear Physics B - Proceedings Supplements 51, Nr. 2 (November 1996): 171–77. http://dx.doi.org/10.1016/s0920-5632(96)00501-4.

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5

Blinnikov, Sergei I. „Mirror matter and other dark matter models“. Uspekhi Fizicheskih Nauk 184, Nr. 2 (2014): 194–99. http://dx.doi.org/10.3367/ufnr.0184.201402h.0194.

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6

Blinnikov, S. I. „Mirror matter and other dark matter models“. Physics-Uspekhi 57, Nr. 2 (28.02.2014): 183–88. http://dx.doi.org/10.3367/ufne.0184.201402h.0194.

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7

Feng, Haoyang. „Integrated study of dark matter and dark energy models“. Theoretical and Natural Science 34, Nr. 1 (29.04.2024): 162–71. http://dx.doi.org/10.54254/2753-8818/34/20241173.

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Dark matter and dark energy are used as two important concepts in cosmology to explain some of the observed phenomena in the universe. Dark matter is one of the most dominant constituents of the Universe, and it influences the structural formation of the Universe through gravity, including the formation and evolution of galaxies, clusters, and the large-scale structure of the Universe. Dark energy is believed to be one of the causes of the accelerated expansion of the Universe, and its presence explains the observed phenomenon of the accelerating rate of expansion of the Universe. Although their existence has not been directly observed, people understand through the study of the structure and evolution of the universe that they play an important role in the universe. This paper first introduces the background knowledge of dark matter and its related properties and explains the reasons why three types of models, namely WIMP, axion, and sterile neutrino, are candidates for dark matter in the light of existing observations. The paper then discusses the relevant properties of dark energy and analyses the mainstream dark energy models. For the cosmological constant mode, the fine-tuning problem and cosmic coincidence problem it faces are analysed in detail. The evolution of the dark energy equation of state from the past >-1 to the present <-1 is then explained, and this is used to introduce the scalar field model involving dynamic, the Chaplygin gas model, the holographic dark energy model, and the interacting dark energy model.
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8

Bertacca, Daniele, Nicola Bartolo und Sabino Matarrese. „Unified Dark Matter Scalar Field Models“. Advances in Astronomy 2010 (2010): 1–29. http://dx.doi.org/10.1155/2010/904379.

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We analyze and review cosmological models in which the dynamics of a single scalar field accounts for a unified description of the Dark Matter and Dark Energy sectors, dubbed Unified Dark Matter (UDM) models. In this framework, we consider the general Lagrangian of -essence, which allows to find solutions around which the scalar field describes the desired mixture of Dark Matter and Dark Energy. We also discuss static and spherically symmetric solutions of Einstein's equations for a scalar field with noncanonical kinetic term, in connection with galactic halo rotation curves.
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9

Boyle, Latham A., Robert R. Caldwell und Marc Kamionkowski. „Spintessence! New models for dark matter and dark energy“. Physics Letters B 545, Nr. 1-2 (Oktober 2002): 17–22. http://dx.doi.org/10.1016/s0370-2693(02)02590-x.

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10

Sussman, Roberto A., Israel Quiros und Osmel Martín González. „Inhomogeneous models of interacting dark matter and dark energy“. General Relativity and Gravitation 37, Nr. 12 (23.11.2005): 2117–43. http://dx.doi.org/10.1007/s10714-005-0199-4.

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11

Arun, Kenath, S. B. Gudennavar und C. Sivaram. „Dark matter, dark energy, and alternate models: A review“. Advances in Space Research 60, Nr. 1 (Juli 2017): 166–86. http://dx.doi.org/10.1016/j.asr.2017.03.043.

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12

Tuominen, Kimmo. „Cold Particle Dark Matter“. Symmetry 13, Nr. 10 (15.10.2021): 1945. http://dx.doi.org/10.3390/sym13101945.

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Possible dark matter candidates in particle physics span a mass range extending over fifty orders of magnitude. In this review, we consider the range of masses from a few keV to a few hundred TeV, which is relevant for cold particle dark matter. We will consider models where dark matter arises as weakly coupled elementary fields and models where dark matter is a composite state bound by a new strong interaction. Different production mechanisms for dark matter in these models will be described. The landscape of direct and indirect searches for dark matter and some of the resulting constraints on models will be briefly discussed.
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13

Abe, Tomohiro, Yoav Afik, Andreas Albert, Christopher R. Anelli, Liron Barak, Martin Bauer, J. Katharina Behr et al. „LHC Dark Matter Working Group: Next-generation spin-0 dark matter models“. Physics of the Dark Universe 27 (Januar 2020): 100351. http://dx.doi.org/10.1016/j.dark.2019.100351.

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14

Liddle, A. R., und D. H. Lyth. „Inflation and mixed dark matter models“. Monthly Notices of the Royal Astronomical Society 265, Nr. 2 (15.11.1993): 379–84. http://dx.doi.org/10.1093/mnras/265.2.379.

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15

Muñoz, Carlos. „Models of Supersymmetry for Dark Matter“. EPJ Web of Conferences 136 (2017): 01002. http://dx.doi.org/10.1051/epjconf/201713601002.

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16

Campos, A., G. Yepes, A. Klypin, G. Murante, A. Provenzale und S. Borgani. „Mass Segregation in Dark Matter Models“. Astrophysical Journal 446 (Juni 1995): 54. http://dx.doi.org/10.1086/175766.

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17

Olive, Keith A. „Dark Matter in SuperGUT Unification Models“. Journal of Physics: Conference Series 315 (19.08.2011): 012021. http://dx.doi.org/10.1088/1742-6596/315/1/012021.

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18

Muñoz, Carlos. „Indirect dark matter searches and models“. Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 692 (November 2012): 13–19. http://dx.doi.org/10.1016/j.nima.2012.01.053.

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19

Suematsu, Daijiro. „Neutrino mass models and dark matter“. Progress in Particle and Nuclear Physics 64, Nr. 2 (April 2010): 454–56. http://dx.doi.org/10.1016/j.ppnp.2009.12.074.

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20

Bergström, Lars. „Dark matter: Models and detection methods“. Nuclear Physics B - Proceedings Supplements 118 (April 2003): 329–40. http://dx.doi.org/10.1016/s0920-5632(03)01326-4.

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21

LI, TianJun, ZhaoFeng KANG und Xin GAO. „Introduction to the dark matter models“. SCIENTIA SINICA Physica, Mechanica & Astronomica 41, Nr. 12 (01.11.2011): 1396–401. http://dx.doi.org/10.1360/132011-976.

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22

Cheung, Clifford, und David Sanford. „Simplified models of mixed dark matter“. Journal of Cosmology and Astroparticle Physics 2014, Nr. 02 (06.02.2014): 011. http://dx.doi.org/10.1088/1475-7516/2014/02/011.

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23

MURANTE, G., A. PROVENZALE, S. BORGANI, A. CAMPOS und G. YEPES. „Scaling analysis of dark matter models“. Astroparticle Physics 5, Nr. 1 (Juni 1996): 53–68. http://dx.doi.org/10.1016/0927-6505(96)00005-9.

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24

Heinemeyer, Sven, und Carlos Muñoz. „Dark Matter in Supersymmetry“. Universe 8, Nr. 8 (18.08.2022): 427. http://dx.doi.org/10.3390/universe8080427.

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Supersymmetry is a well-motivated theory for physics beyond the Standard Model. In particular, supersymmetric models can naturally possess dark matter candidates that can give rise to the measured dark matter content of the universe. We review several models that have been analyzed with regard to dark matter by groups based in Spain in recent years. These models include, in particular, the Minimal Supersymmetric Standard Model (MSSM) and the ‘μ from ν’ Supersymmetric Standard Model (μνSSM) in various versions.
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25

Dil, Emre. „Couplingq-Deformed Dark Energy to Dark Matter“. Advances in High Energy Physics 2016 (2016): 1–20. http://dx.doi.org/10.1155/2016/9753208.

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We propose a novel coupled dark energy model which is assumed to occur as aq-deformed scalar field and investigate whether it will provide an expanding universe phase. We consider theq-deformed dark energy as coupled to dark matter inhomogeneities. We perform the phase-space analysis of the model by numerical methods and find the late-time accelerated attractor solutions. The attractor solutions imply that the coupledq-deformed dark energy model is consistent with the conventional dark energy models satisfying an acceleration phase of universe. At the end, we compare the cosmological parameters of deformed and standard dark energy models and interpret the implications.
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Borzou, Ahmad. „Assessment of Dark Matter Models Using Dark Matter Correlations across Dwarf Spheroidal Galaxies“. Universe 8, Nr. 7 (21.07.2022): 386. http://dx.doi.org/10.3390/universe8070386.

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The predicted size of dark matter substructures in kilo-parsec scales is model-dependent. Therefore, if the correlations between dark matter mass densities as a function of the distances between them are measured via observations, we can scrutinize dark matter scenarios. In this paper, we present an assessment procedure of dark matter scenarios. First, we use Gaia’s data to infer the single-body phase-space density of the stars in the Fornax dwarf spheroidal galaxy. The latter, together with the Jeans equation, after eliminating the gravitational potential using the Poisson equation, reveals the mass density of dark matter as a function of its position in the galaxy. We derive the correlations between dark matter mass densities as a function of distances between them. No statistically significant correlation is observed. Second, for the sake of comparison with the standard cold dark matter, we also compute the correlations between dark matter mass densities in a small halo of the Eagle hydrodynamics simulation. We show that the correlations from the simulation and from Gaia are in agreement. Third, we show that Gaia observations can be used to limit the parameter space of the Ginzburg–Landau statistical field theory of dark matter mass densities and subsequently shrink the parameter space of any dark matter model. As two examples, we show how to leave limitations on (i) a classic gas dark matter and (ii) a superfluid dark matter.
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27

Mena, Olga. „Low redshift probes and coupled dark matter-dark energy models“. Journal of Physics: Conference Series 259 (01.11.2010): 012084. http://dx.doi.org/10.1088/1742-6596/259/1/012084.

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28

DEL NOBILE, EUGENIO, CHRIS KOUVARIS, FRANCESCO SANNINO und JUSSI VIRKAJÄRVI. „DARK MATTER INTERFERENCE“. Modern Physics Letters A 27, Nr. 19 (21.06.2012): 1250108. http://dx.doi.org/10.1142/s0217732312501088.

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We study different patterns of interference in WIMP-nuclei elastic scattering that can accommodate the DAMA and CoGeNT experiments via an isospin violating ratio fn/fp = -0.71. We study interference between the following pairs of mediators: Z and Z′, Z′ and Higgs, and two Higgs fields. We show under what conditions interference works. We also demonstrate that in the case of the two Higgs interference, an explanation of the DAMA/CoGeNT is consistent with electroweak baryogenesis scenarios based on two Higgs doublet models proposed in the past.
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29

KIM, SUNG-WON, und YURI KANG. „DARK ENERGY AND DARK MATTER ACCRETION ONTO A BLACK HOLE IN EXPANDING UNIVERSE“. International Journal of Modern Physics: Conference Series 12 (Januar 2012): 320–29. http://dx.doi.org/10.1142/s2010194512006526.

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In this paper, we considered the multi-component accretion onto the black hole in the expanding universe. The accreted matters are dark energy, dark matter, and the interaction terms. We found the black hole mass change rates and their behaviors according to the models of interaction and dark energy.
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30

Lee, Jae-Weon. „Brief History of Ultra-light Scalar Dark Matter Models“. EPJ Web of Conferences 168 (2018): 06005. http://dx.doi.org/10.1051/epjconf/201816806005.

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This is a review on the brief history of the scalar field dark matter model also known as fuzzy dark matter, BEC dark matter, wave dark matter, or ultra-light axion. In this model ultra-light scalar dark matter particles with mass m = O(10-22)eV condense in a single Bose-Einstein condensate state and behave collectively like a classical wave. Galactic dark matter halos can be described as a self-gravitating coherent scalar field configuration called boson stars. At the scale larger than galaxies the dark matter acts like cold dark matter, while below the scale quantum pressure from the uncertainty principle suppresses the smaller structure formation so that it can resolve the small scale crisis of the conventional cold dark matter model.
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31

Rahimi, Elham, Evan Vienneau, Nassim Bozorgnia und Andrew Robertson. „The local dark matter distribution in self-interacting dark matter halos“. Journal of Cosmology and Astroparticle Physics 2023, Nr. 02 (01.02.2023): 040. http://dx.doi.org/10.1088/1475-7516/2023/02/040.

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Abstract We study the effects of dark matter self-interactions on the local dark matter distribution in selected Milky Way-like galaxies in the EAGLE hydrodynamical simulations. The simulations were run with two different self-interacting dark matter models, a constant and velocity-dependent self-interaction cross-section. We find that the local dark matter velocity distribution of the Milky Way-like halos in the simulations with dark matter self-interactions and baryons are generally similar to those extracted from cold collisionless dark matter simulations with baryons. In both cases, the local dark matter speed distributions agree well with their best fit Maxwellian distributions. Including baryons in the simulations with or without dark matter self-interactions increases the local dark matter density and shifts the dark matter speed distributions to higher speeds. To study the implications for direct detection, we compute the dark matter halo integrals obtained directly from the simulations and compare them to those obtained from the best fit Maxwellian velocity distribution. We find that a Maxwellian distribution provides a good fit to the halo integrals of most halos, without any significant difference between the results of different dark matter self-interaction models.
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32

Edmonds, Douglas, Djordje Minic und Tatsu Takeuchi. „Dark matter, dark energy and fundamental acceleration“. International Journal of Modern Physics D 29, Nr. 14 (Oktober 2020): 2043030. http://dx.doi.org/10.1142/s0218271820430300.

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We discuss the existence of an acceleration scale in galaxies and galaxy clusters and its relevance for the nature of dark matter. The presence of the same acceleration scale found at very different length scales, and in very different astrophysical objects, strongly supports the existence of a fundamental acceleration scale governing the observed gravitational physics. We comment on the implications of such a fundamental acceleration scale for constraining cold dark matter models as well as its relevance for structure formation to be explored in future numerical simulations.
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33

Nagata, Natsumi, Keith A. Olive und Jiaming Zheng. „Asymmetric dark matter models in SO(10)“. Journal of Cosmology and Astroparticle Physics 2017, Nr. 02 (09.02.2017): 016. http://dx.doi.org/10.1088/1475-7516/2017/02/016.

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34

Cerdeño, D. G., A. Cheek, E. Reid und H. Schulz. „Surrogate models for direct dark matter detection“. Journal of Cosmology and Astroparticle Physics 2018, Nr. 08 (09.08.2018): 011. http://dx.doi.org/10.1088/1475-7516/2018/08/011.

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35

Bode, Paul, Jeremiah P. Ostriker und Neil Turok. „Halo Formation in Warm Dark Matter Models“. Astrophysical Journal 556, Nr. 1 (20.07.2001): 93–107. http://dx.doi.org/10.1086/321541.

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36

Wilkinson, M. I., J. Kleyna, N. W. Evans und G. Gilmore. „Dark matter in dwarf spheroidals I. Models“. Monthly Notices of the Royal Astronomical Society 330, Nr. 4 (März 2002): 778–91. http://dx.doi.org/10.1046/j.1365-8711.2002.05154.x.

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37

von Buddenbrock, Stefan. „Hypothesising Dark Matter Models in pp Collisions“. Journal of Physics: Conference Series 645 (15.10.2015): 012017. http://dx.doi.org/10.1088/1742-6596/645/1/012017.

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38

Gratsias, John, Robert J. Scherrer, Gary Steigman und Jens V. Villumsen. „Seeded hot dark matter models with inflation“. Astrophysical Journal 405 (März 1993): 30. http://dx.doi.org/10.1086/172339.

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39

Kane, G. L. „Realistic models of supersymmetric particle dark matter“. Nuclear Physics B - Proceedings Supplements 51, Nr. 2 (November 1996): 178–82. http://dx.doi.org/10.1016/s0920-5632(96)00503-8.

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40

Zhang, Yi, und Yue Zhao. „Unconventional dark matter models: a brief review“. Science Bulletin 60, Nr. 11 (Juni 2015): 986–94. http://dx.doi.org/10.1007/s11434-015-0804-1.

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41

Piattella, Oliver F., Daniele Bertacca, Marco Bruni und Davide Pietrobon. „Unified Dark Matter models with fast transition“. Journal of Cosmology and Astroparticle Physics 2010, Nr. 01 (07.01.2010): 014. http://dx.doi.org/10.1088/1475-7516/2010/01/014.

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42

Valentim, R., und J. F. Jesus. „Entropy and creation cold dark matter models“. Astronomische Nachrichten 340, Nr. 1-3 (Januar 2019): 105–7. http://dx.doi.org/10.1002/asna.201913570.

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43

Pace, Francesco, und Carlo Schimd. „Tidal virialization of dark matter haloes with clustering dark energy“. Journal of Cosmology and Astroparticle Physics 2022, Nr. 03 (01.03.2022): 014. http://dx.doi.org/10.1088/1475-7516/2022/03/014.

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Abstract We extend the analysis of Pace et al. [1] by considering the virialization process in the extended spherical collapse model for clustering dark-energy models, i.e., accounting for dark-energy fluctuations. Differently from the standard approach, here virialization is naturally achieved by properly modelling deviations from sphericity due to shear and rotation induced by tidal interactions. We investigate the time evolution of the virial overdensity Δvir in seven clustering dynamical dark energy models and compare the results to the ΛCDM model and to the corresponding smooth dark-energy models. Taking into account all the appropriate corrections, we deduce the abundance of convergence peaks for Rubin Observatory-LSST and Euclid-like weak-lensing surveys, of Sunyaev-Zel'dovich peaks for a Simon Observatory-like CMB survey, and of X-ray peaks for an eROSITA-like survey. Despite the tiny differences in Δvir between clustering and smooth dark-energy models, owing to the large volumes covered by these surveys, five out of seven clustering dark-energy models can be statistically distinguished from ΛCDM. The contribution of dark-energy fluctuation cannot be neglected, especially for the Chevallier-Polarski-Limber and Albrecht-Skordis models, provided the instrumental configurations provide high signal-to-noise ratio. These results are almost independent of the tidal virialization model.
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44

Bolotin, Yuri L., Alexander Kostenko, Oleg A. Lemets und Danylo A. Yerokhin. „Cosmological evolution with interaction between dark energy and dark matter“. International Journal of Modern Physics D 24, Nr. 03 (23.02.2015): 1530007. http://dx.doi.org/10.1142/s0218271815300074.

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In this review we consider in detail different theoretical topics associated with interaction in the dark sector. We study linear and nonlinear interactions which depend on the dark matter and dark energy densities. We consider a number of different models (including the holographic dark energy and dark energy in a fractal universe), with interacting dark energy and dark matter, have done a thorough analysis of these models. The main task of this review was not only to give an idea about the modern set of different models of dark energy, but to show how much can be diverse dynamics of the universe in these models. We find that the dynamics of a universe that contains interaction in the dark sector can differ significantly from the Standard Cosmological Model.
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45

SUN, CHENG-YI, und YU SONG. „INCONSISTENCES IN INTERACTING AGEGRAPHIC DARK ENERGY MODELS“. Modern Physics Letters A 26, Nr. 40 (28.12.2011): 3055–66. http://dx.doi.org/10.1142/s0217732311037285.

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It is found that the origin agegraphic dark energy tracks the matter in the matter-dominated epoch and then the subsequent dark-energy-dominated epoch becomes impossible. It is argued that the difficulty can be removed when the interaction between the agegraphic dark energy and dark matter is considered. In the note, by discussing three different interacting models, we find that the difficulty still stands even in the interacting models. Furthermore, we find that in the interacting models, there exists the other serious inconsistence that the existence of the radiation/matter-dominated epoch contradicts the ability of agegraphic dark energy in driving the accelerated expansion. The contradiction can be avoided in one of the three models if some constraints on the parameters hold.
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46

ARAKI, TAKESHI, C. Q. GENG und KEIKO I. NAGAO. „SIGNATURES OF DARK MATTER IN INERT TRIPLET MODELS“. International Journal of Modern Physics D 20, Nr. 08 (15.08.2011): 1433–40. http://dx.doi.org/10.1142/s021827181101961x.

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In this talk, we will review the signatures of dark matter in two inert triplet models. For the first model with the hypercharge Y = 0, the dark matter mass around 5.5 TeV is favored by both the WMAP data and the direct detection. In contrast, for the second model of Y = 2, it is excluded by the direct detection experiments although dark matter with its mass around 2.8 TeV is allowed by WMAP.
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47

KILE, JENNIFER. „FLAVORED DARK MATTER: A REVIEW“. Modern Physics Letters A 28, Nr. 34 (17.10.2013): 1330031. http://dx.doi.org/10.1142/s0217732313300310.

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The current status of flavored dark matter (DM) is reviewed. We discuss the main experimental constraints on models of flavored DM and survey some possible considerations which are relevant for the constructions of models. We then review the application of existing flavor principles to DM, with an emphasis on minimal flavor violation, and discuss implications of flavored DM on collider phenomenology.
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48

Delort, Thierry. „Theory of Dark Matter and Dark Energy“. Applied Physics Research 10, Nr. 5 (27.09.2018): 1. http://dx.doi.org/10.5539/apr.v10n5p1.

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In this article, we propose a new model of dark matter. According to this new model, dark matter is a substance, that is a new physical element not constituted of classical particles, called dark substance and filling the Universe. Assuming some very simple physical properties to this dark substance, we theoretically justify the flat rotation curve of galaxies and the baryonic Tully-Fisher&rsquo;s law. We then study according to our new theory of dark matter&nbsp; the different possible distributions of dark matter in galaxies and in galaxy clusters, and the velocities of galaxies in galaxy clusters. Then using the new model of dark matter we are naturally led to propose a new geometrical model of Universe, finite, that is different from all geometrical models proposed by the Standard Cosmological Model (SCM). Despite that our Theory of dark matter is compatible with the SCM, we then expose a new Cosmological model based on this new geometrical form of the Universe and on the interpretation of the CMB Rest Frame (CRF), that has not physical interpretation on the SCM and that we will call local Cosmological frame. We then propose 2 possible mathematical models of expansion inside the new Cosmological model. The 1st mathematical model is based on General Relativity as the SCM and gives the same theoretical predictions of distances and of the Hubble&rsquo;s constant as the SCM. The 2nd mathematical model of expansion of the Universe is mathematically much simpler than the mathematical model of expansion used in the SCM, but we will see that its theoretical predictions are in agreement with astronomical observations. Moreover, this 2nd mathematical model of expansion does not need to introduce the existence of a dark energy contrary to the mathematical model of expansion of the SCM. To end we study the evolution of the temperature of dark substance in the Universe and we make appear the existence of a dark energy, due to our model of dark matter.
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49

Eingorn, Maxim, und Claus Kiefer. „Scalar perturbations in cosmological models with dark energy-dark matter interaction“. Journal of Cosmology and Astroparticle Physics 2015, Nr. 07 (22.07.2015): 036. http://dx.doi.org/10.1088/1475-7516/2015/07/036.

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50

Chimento, Luis P., Ruth Lazkoz und Irene Sendra. „DBI models for the unification of dark matter and dark energy“. General Relativity and Gravitation 42, Nr. 5 (30.10.2009): 1189–209. http://dx.doi.org/10.1007/s10714-009-0901-z.

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