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Gotowe bibliografie tematyczne / Weakly Interacting Massive Particle (WIMP)

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Gotowa bibliografia na temat „Weakly Interacting Massive Particle (WIMP)”

Autor: Grafiati

Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Weakly Interacting Massive Particle (WIMP)"

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Choi, Ki-Young, Jinn-Ouk Gong i Chang Sub Shin. "Small Scale Isocurvature Perturbation of Weakly Interacting Massive Particle". International Journal of Modern Physics: Conference Series 43 (styczeń 2016): 1660202. http://dx.doi.org/10.1142/s2010194516602027.

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It is known that the smallest size of the structures of the Universe with the weakly interacting massive dark matter is determined by the scale that enters the Hubble horizon at the time of kinetic decoupling of WIMP. This comes from the fact that the perturbation at smaller scales is erased due to the collisional damping during the kinetic decoupling. However the isocurvature mode is not affected and continue to be constant. We discuss about the generation of the isocurvature mode of WIMP dark matter at small scales recently found by Choi, Gong, and Shin1 and its implications for the indirect detection of dark matter through the formation of the small size of halos.

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Funk, Stefan. "Indirect detection of dark matter with γ rays". Proceedings of the National Academy of Sciences 112, nr 40 (12.05.2014): 12264–71. http://dx.doi.org/10.1073/pnas.1308728111.

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The details of what constitutes the majority of the mass that makes up dark matter in the Universe remains one of the prime puzzles of cosmology and particle physics today—80 y after the first observational indications. Today, it is widely accepted that dark matter exists and that it is very likely composed of elementary particles, which are weakly interacting and massive [weakly interacting massive particles (WIMPs)]. As important as dark matter is in our understanding of cosmology, the detection of these particles has thus far been elusive. Their primary properties such as mass and interaction cross sections are still unknown. Indirect detection searches for the products of WIMP annihilation or decay. This is generally done through observations of γ-ray photons or cosmic rays. Instruments such as the Fermi large-area telescope, high-energy stereoscopic system, major atmospheric gamma-ray imaging Cherenkov, and very energetic radiation imaging telescope array, combined with the future Cherenkov telescope array, will provide important complementarity to other search techniques. Given the expected sensitivities of all search techniques, we are at a stage where the WIMP scenario is facing stringent tests, and it can be expected that WIMPs will be either be detected or the scenario will be so severely constrained that it will have to be rethought. In this sense, we are on the threshold of discovery. In this article, I will give a general overview of the current status and future expectations for indirect searches of dark matter (WIMP) particles.

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the LUX and LZ Collaborations, Vitaly Kudryavtsev for. "Recent Results from LUX and Prospects for Dark Matter Searches with LZ". Universe 5, nr 3 (7.03.2019): 73. http://dx.doi.org/10.3390/universe5030073.

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Weakly Interacting Massive Particle (WIMP) remains one of the most promising dark matter candidates. Many experiments around the world are searching for WIMPs and the best current sensitivity to WIMP-nucleon spin-independent cross-section is about 10 − 10 pb. LUX has been one of the world-leading experiments in the search for dark matter WIMPs. Results from the LUX experiment on WIMP searches for different WIMP masses are summarised in this paper. The LUX detector will be replaced by its successor, the LUX-ZEPLIN (LZ) detector. With 50 times larger fiducial mass and an increased background rejection power due to specially-designed veto systems, the LZ experiment (due to take first data in 2020) will achieve a sensitivity to WIMPs exceeding the current best limits by more than an order of magnitude (for spin-independent interactions and for WIMP masses exceeding a few GeV). An overview of the LZ experiment is presented and LZ sensitivity is discussed based on the accurately modelled background and the high-sensitivity material screening campaign.

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Jagemann, Thomas. "CRESST Detectors for Nonbaryonic Cold Dark Matter Particles". Symposium - International Astronomical Union 220 (2004): 493–94. http://dx.doi.org/10.1017/s0074180900183901.

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The CRESST experiment is set up for the direct detection of Weakly Interacting Massive Particles (WIMPs) which our Galactic dark matter halo possibly consists of. the employed detection method is elastic scattering by nuclei. the recoiling nucleus deposits most of its energy in the form of lattice vibrations in the detector. Cooling the detector to very low temperatures (mK) enhances the temperature rise due to the energy deposition. the crucial parameter for direct WIMP searches is the sensitivity to the WIMP interaction cross section in a certain range of possible WIMP masses. CRESST is now sensitive enough to explore the parameter space predicted by supersymmetric models.

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Green, Anne M. "WIMP direct detection and halo structure". Symposium - International Astronomical Union 220 (2004): 483–88. http://dx.doi.org/10.1017/s0074180900183871.

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Weakly Interacting Massive Particle (WIMP) direct detection experiments are just reaching the sensitivity required to detect Galactic dark matter in the form of neutralinos (or indeed any stable weakly interacting particle). Detection strategies and data analyses are often based on the simplifying assumption of a standard spherical, isothermal halo model, but observations and numerical simulations indicate that galaxy halos are in fact triaxial and anisotropic, and contain substructure. the annual modulation and direction dependence of the event rate (due to the motion of the Earth) provide the best prospects of distinguishing WIMP scattering from background events, however these signals depend sensitively on the local WIMP velocity distribution. I briefly review the status of WIMP direct detection experiments before discussing the dependence of the annual modulation signal on astrophysical input, in particular the structure of the Milky Way halo, and the possibility that the local WIMP distribution is not smooth.

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ULLIO, PIERO. "SEARCHES FOR DARK MATTER PARTICLES THROUGH COSMIC RAY MEASUREMENTS". International Journal of Modern Physics A 17, nr 12n13 (20.05.2002): 1777–86. http://dx.doi.org/10.1142/s0217751x02011278.

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We consider the hypothesis that dark matter is made of weakly interacting massive particles (WIMPs) and describe how their pair annihilation in the galactic halo generates exotic cosmic ray fluxes. Features for generic WIMP models are reviewed, pointing out cases in which clear signatures arise. Implications from available and upcoming measurements are discussed.

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SHAN, CHUNG-LIN. "EFFECTS OF RESIDUE BACKGROUND EVENTS IN DIRECT DETECTION EXPERIMENTS ON IDENTIFYING WIMP DARK MATTER". International Journal of Modern Physics D 20, nr 08 (15.08.2011): 1453–61. http://dx.doi.org/10.1142/s0218271811019633.

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We reexamine the model-independent data analysis methods for extracting properties of Weakly Interacting Massive Particles (WIMPs) by using data (measured recoil energies) from direct Dark Matter detection experiments directly and, as a more realistic study, consider a small fraction of residue background events, which pass all discrimination criteria and then mix with other real WIMP-induced signals in the analyzed data sets. In this talk, the effects of residue backgrounds on the determination of the WIMP mass as well as the spin-independent WIMP coupling on nucleons will be discussed.

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Sahu, R., V. K. B. Kota i T. S. Kosmas. "Event Rates for the Scattering of Weakly Interacting Massive Particles from 23Na and 40Ar". Particles 4, nr 1 (24.02.2021): 75–92. http://dx.doi.org/10.3390/particles4010010.

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Detection rates for the elastic and inelastic scattering of weakly interacting massive particles (WIMPs) off 23Na are calculated within the framework of Deformed Shell Model (DSM) based on Hartree-Fock states. At first, the spectroscopic properties of the detector nucleus, like energy spectra and magnetic moments, are evaluated and compared with experimental data. Following the good agreement of these results, DSM wave functions are used for obtaining elastic and inelastic spin structure functions, nuclear structure coefficients and so forth for the WIMP-23Na scattering. Then, the event rates are also computed with a given set of supersymmetric parameters. In the same manner, using DSM wavefunctions, nuclear structure coefficients and event rates for elastic scattering of WIMPs from 40Ar are also obtained. These results for event rates and also for annual modulation will be useful for the ongoing and future WIMP detection experiments involving detector materials with 23Na and 40Ar nuclei.

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Dutta, Koushik, Avirup Ghosh, Arpan Kar i Biswarup Mukhopadhyaya. "MeV to multi-TeV thermal WIMPs: most conservative limits". Journal of Cosmology and Astroparticle Physics 2023, nr 08 (1.08.2023): 071. http://dx.doi.org/10.1088/1475-7516/2023/08/071.

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Abstract We consider a weakly interacting massive particle (WIMP) dark matter (DM) annihilating into all possible Standard Model (SM) particle pairs, including the SM neutrinos, via s-wave processes and derive the branching ratio independent upper limit on the total annihilation cross-section 〈σv〉 using the data of CMB, gamma-ray, cosmic-ray and several neutrino observations. For conservative choices of all relevant astrophysical parameters, we obtain upper limits of 10-23–10-25 cm3 s-1 on the total 〈σv〉 for the WIMP mass range 10 MeV–100 TeV, thus making the entire mass range consistent with the observed relic density. An important input that goes into our analysis is the assumption that thermal WIMPs can have significant coupling to the SM neutrinos.

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Cui, Yanou. "A review of WIMP baryogenesis mechanisms". Modern Physics Letters A 30, nr 37 (16.11.2015): 1530028. http://dx.doi.org/10.1142/s0217732315300281.

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It was recently proposed that weakly interacting massive particles (WIMP) may provide new ways of generating the observed baryon asymmetry in the early universe, as well as addressing the cosmic coincidence between dark matter (DM) and baryon abundances. This suggests a new possible connection between weak scale new particle physics and modern cosmology. This review summarizes the general ideas and simple model examples of the two recently proposed WIMP baryogenesis mechanisms: baryogenesis from WIMP DM annihilation during thermal freeze-out, and baryogenesis from metastable WIMP decay after thermal freeze-out. This review also discusses the interesting phenomenology of these models, in particular, the experimental signals that can be probed in the intensity frontier experiments and the large hadron collider (LHC) experiments.

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Rozprawy doktorskie na temat "Weakly Interacting Massive Particle (WIMP)"

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Shaul, Diana Naomi April. "Searching for WIMPs and axion-like particles". Thesis, Imperial College London, 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.244125.

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Części książek na temat "Weakly Interacting Massive Particle (WIMP)"

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Jackson Kimball, Derek F., i Dmitry Budker. "Introduction to Dark Matter". W The Search for Ultralight Bosonic Dark Matter, 1–30. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-030-95852-7_1.

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AbstractTo set the stage for our study of ultralight bosonic dark matter (UBDM), we review the evidence for the existence of dark matter: galactic and stellar dynamics, gravitational lensing studies, measurements of the cosmic microwave background radiation (CMB), surveys of the large-scale structure of the universe, and the observed abundance of light elements. This diverse array of observational evidence informs what we know about dark matter: its universal abundance, its spatial and velocity distribution, and that its explanation involves physics beyond the Standard Model. But what we know about dark matter is far outweighed by what we do not know. We examine UBDM in the context of several of the most prominent alternative hypotheses for the nature of dark matter: weakly interacting massive particles (WIMPs), sterile neutrinos, massive astrophysical compact halo objects (MACHOs), and primordial black holes (PBHs). Finally we examine some of the key general characteristics of UBDM, including its wavelike nature, coherence properties, and couplings to Standard Model particles and fields.

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Hisano, Junji. "Effective Theory Approach to Direct Detection of Dark Matter". W Effective Field Theory in Particle Physics and Cosmology, 650–88. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780198855743.003.0011.

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It is now certain that dark matter exists in the Universe. However, we do not know its nature, nor are there dark matter candidates in the standard model of particle physics or astronomy However, weakly interacting massive particles (WIMPs) in models beyond the standard model are one of the leading candidates available to provide explanation. The dark matter direct detection experiments, in which the nuclei recoiled by WIMPs are sought, are one of the methods to elucidate the nature of dark matter. This chapter introduces an effective field theory (EFT) approach in order to evaluate the nucleon–WIMP elastic scattering cross section.

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Fisher, Peter. "Introduction: The Dark Matter Problem". W What Is Dark Matter?, 1–4. Princeton University Press, 2022. http://dx.doi.org/10.23943/princeton/9780691148342.003.0001.

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This chapter provides a background of the specters that represent dark matter, which explains how astronomers came to know about it. It mentions how theoreticians uncovered how dark matter shaped the largest structures in our universe through gravity and how physicists and astronomers are navigating the complex, frustrating hunt to understand more about dark matter. It also uses the terms visible matter or normal or luminous matter, which refer to matter that forms stars and generates the light observed through telescopes. The chapter focuses on two hypothesized new particles: Weakly Interacting Massive Particles (WIMPs) and axions. It introduces the weak, strong, and electromagnetic forces, which are variants of quantum field theory and collectively make up the Standard Model of particle physics.

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Oliveira, Firmin, i Michael L. Smith. "Dark Matter in Spiral Galaxies as the Gravitational Redshift of Gravitons". W Dark Matter - Recent Observations and Theoretical Advances [Working Title]. IntechOpen, 2022. http://dx.doi.org/10.5772/intechopen.101130.

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Several recent attempts to observe dark matter with characteristics similar to atomic or subatomic particles as Weakly Interacting Massive Particles (WIMPs) have failed to detect anything real over a wide energy range. Likewise, considerations of large, non-emitting objects as the source of most dark matter fall short of expectations. Here we consider the possibility that massless gravitons suffering slow redshift may be responsible for the properties of spiral galaxies attributed to dark matter. Particles such as gravitons will be extremely difficult to directly detect; the best we can envision is measuring this influence on stellar and galactic motions. Since the motions of stars and galaxies are non-relativistic, we can apply our idea to describe the expected large-scale motions using only Newtonian mechanics. Using our assumption about the importance of the graviton, we here describe the well-known Tully-Fisher relationship of spiral galaxies without resorting to hypothesizing exotic WIMPs or invoking modifications of Newtonian dynamics (MoND).

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Streszczenia konferencji na temat "Weakly Interacting Massive Particle (WIMP)"

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Stockwell, Walter, D. Akerib, E. Aubourg, P. D. Barnes, Jr., A. Cummings, Angela Da Silva, J. Emes i in. "Cryogenic germanium detectors for a weakly interactive massive particle (WIMP) dark-matter search". W SPIE's 1994 International Symposium on Optics, Imaging, and Instrumentation, redaktorzy Oswald H. W. Siegmund i John V. Vallerga. SPIE, 1994. http://dx.doi.org/10.1117/12.186825.

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Vallicelli, Elia A., Luca Gelmi, Roberto Bertoni, Walter Fulgione, Mattia Tambaro, Andrea Baschirotto i Marcello De Matteis. "A 0.3nV/√ Hz Input-Referred-Noise Analog Front-End for Weakly-Interacting-Massive-Particles (WIMPs) Acoustic Sensing in Bubbles-Chamber Detectors". W 2019 15th Conference on Ph.D Research in Microelectronics and Electronics (PRIME). IEEE, 2019. http://dx.doi.org/10.1109/prime.2019.8787765.

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