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1
Choi, Ki-Young, Jinn-Ouk Gong, and Chang Sub Shin. "Small Scale Isocurvature Perturbation of Weakly Interacting Massive Particle." International Journal of Modern Physics: Conference Series 43 (January 2016): 1660202. http://dx.doi.org/10.1142/s2010194516602027.
Повний текст джерелаАнотація:
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.
2
Funk, Stefan. "Indirect detection of dark matter with γ rays". Proceedings of the National Academy of Sciences 112, № 40 (12 травня 2014): 12264–71. http://dx.doi.org/10.1073/pnas.1308728111.
Повний текст джерелаАнотація:
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.
3
the LUX and LZ Collaborations, Vitaly Kudryavtsev for. "Recent Results from LUX and Prospects for Dark Matter Searches with LZ." Universe 5, no. 3 (March 7, 2019): 73. http://dx.doi.org/10.3390/universe5030073.
Повний текст джерелаАнотація:
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.
4
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.
Повний текст джерелаАнотація:
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.
5
Green, Anne M. "WIMP direct detection and halo structure." Symposium - International Astronomical Union 220 (2004): 483–88. http://dx.doi.org/10.1017/s0074180900183871.
Повний текст джерелаАнотація:
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.
6
ULLIO, PIERO. "SEARCHES FOR DARK MATTER PARTICLES THROUGH COSMIC RAY MEASUREMENTS." International Journal of Modern Physics A 17, no. 12n13 (May 20, 2002): 1777–86. http://dx.doi.org/10.1142/s0217751x02011278.
Повний текст джерелаАнотація:
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.
7
SHAN, CHUNG-LIN. "EFFECTS OF RESIDUE BACKGROUND EVENTS IN DIRECT DETECTION EXPERIMENTS ON IDENTIFYING WIMP DARK MATTER." International Journal of Modern Physics D 20, no. 08 (August 15, 2011): 1453–61. http://dx.doi.org/10.1142/s0218271811019633.
Повний текст джерелаАнотація:
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.
8
Sahu, R., V. K. B. Kota, and T. S. Kosmas. "Event Rates for the Scattering of Weakly Interacting Massive Particles from 23Na and 40Ar." Particles 4, no. 1 (February 24, 2021): 75–92. http://dx.doi.org/10.3390/particles4010010.
Повний текст джерелаАнотація:
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.
9
Dutta, Koushik, Avirup Ghosh, Arpan Kar, and Biswarup Mukhopadhyaya. "MeV to multi-TeV thermal WIMPs: most conservative limits." Journal of Cosmology and Astroparticle Physics 2023, no. 08 (August 1, 2023): 071. http://dx.doi.org/10.1088/1475-7516/2023/08/071.
Повний текст джерелаАнотація:
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.
10
Cui, Yanou. "A review of WIMP baryogenesis mechanisms." Modern Physics Letters A 30, no. 37 (November 16, 2015): 1530028. http://dx.doi.org/10.1142/s0217732315300281.
Повний текст джерелаАнотація:
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.
11
Allen, Roland E., and Aritra Saha. "Dark matter candidate with well-defined mass and couplings." Modern Physics Letters A 32, no. 25 (July 31, 2017): 1730022. http://dx.doi.org/10.1142/s0217732317300221.
Повний текст джерелаАнотація:
We propose a Higgs-related but spin-[Formula: see text] dark matter candidate with a mass that is comparable to that of the Higgs. This particle is a weakly interacting massive particle (WIMP) with an R-parity of [Formula: see text], but it can be distinguished from a neutralino by its unconventional couplings to W and Z bosons. Other neutral and charged spin-[Formula: see text] particles of a new kind are also predicted at higher energy.
12
Chen, Shu. "Analysis of Dark Matter Candidates and Detection Scenarios." Highlights in Science, Engineering and Technology 38 (March 16, 2023): 678–84. http://dx.doi.org/10.54097/hset.v38i.5929.
Повний текст джерелаАнотація:
In recent years, the observations collected by the state-of-art detectors have shown that there is considerable amount of invisible matter in our universe, which is named as dark matter. The study of dark matter has become one of the main research directions nowadays. Contemporarily, there are many particle models are considered as candidate of dark matter, including the models of axion, sterile neutrino, and Weakly Interacting Massive Particle (WIMP) e.g., inert Higgs boson, lightest Kaluza-Klein particle and neutralino in supersymmetry. Furthermore, there are also many experiments and measurements of axions and WIMPs, including axion haloscope ADMX, axion helioscope CAST, and WIMP nuclear recoil detection experiments, such as LUX-ZEPLIN and DarkSide-50. In this paper, the basic model of above candidates will be introduced. In addition, discussion about the additional parity-like symmetry for WIMP model building, shortage of the experiments and the future upgraded dark matter experiments will also be presented. Overall, these results shed light on guiding further exploration of dark matter detection and searching.
13
Klapdor-Kleingrothaus, H. V., I. V. Krivosheina, and C. Tomei. "New limits on spin-dependent weakly interacting massive particle (WIMP) nucleon coupling." Physics Letters B 609, no. 3-4 (March 2005): 226–31. http://dx.doi.org/10.1016/j.physletb.2004.12.081.
Повний текст джерела
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Sun, Wenrong. "Demonstration of Models and Detection Scenarios for WIMP And Axion." Highlights in Science, Engineering and Technology 38 (March 16, 2023): 665–71. http://dx.doi.org/10.54097/hset.v38i.5923.
Повний текст джерелаАнотація:
The dark matter physics is a significant part of high energy physics. The model of the dark matter candidate was proposed in last century. In this paper, the analytical models and detection approaches for the WIMPs and axion will be discussed. As one of the candidates, weakly interacting massive particle was proposed to be a good candidate in the past few decades and its model was well established. Many miracles and coincidence of the WIMP properties make it become the most popular candidate for researchers and a lot of detection method was conducted. Direct detection of WIMP is the corner stone of dark matter detection. However, there is no notable progress for WIMP detection until now and the wave dark matter has become popular for researchers. The axion (one of the candidates of dark matter) can resolve the small-scale problem caused by particle dark matter profile. Besides, wave nature of the axion allows researchers to use the pulsar signal to detect them. This paper will give a picture of WIMPs and axion model and detection, inspiring researchers to improve the detection method. These results shed light on guiding further exploration of dark matter searching.
15
CERDEÑO, DAVID G. "DETECTION AND IDENTIFICATION OF DARK MATTER." International Journal of Modern Physics: Conference Series 01 (January 2011): 98–107. http://dx.doi.org/10.1142/s2010194511000134.
Повний текст джерелаАнотація:
Dark matter is an abundant component of our Universe and its detection and identification constitutes one of the most challenging goals in modern Physics. Particle Physics provides well motivated candidates for dark matter, among which a generic weakly-interacting massive particle (WIMP) stands out for its simplicity and the fact that WIMP candidates can be found in many theories proposing new physics at the TeV scale, such as Supersymmetry, models with Universal Extra Dimensions and Little Higgs Theories. I will review the properties of some of the main WIMP candidates and their detectability (with special emphasis on direct detection experiments). I will also address the strategies that can be used to discriminate among them in the case of a future detection.
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Biswas, Anirban, Arpan Kar, Bum-Hoon Lee, Hocheol Lee, Wonwoo Lee, Stefano Scopel, Liliana Velasco-Sevilla, and Lu Yin. "WIMPs in dilatonic Einstein Gauss-Bonnet cosmology." Journal of Cosmology and Astroparticle Physics 2023, no. 08 (August 1, 2023): 024. http://dx.doi.org/10.1088/1475-7516/2023/08/024.
Повний текст джерелаАнотація:
Abstract We use the Weakly Interacting Massive Particle (WIMP) thermal decoupling scenario to probe Cosmologies in dilatonic Einstein Gauss-Bonnet (dEGB) gravity, where the Gauss-Bonnet term is non-minimally coupled to a scalar field with vanishing potential. We put constraints on the model parameters when the ensuing modified cosmological scenario drives the WIMP annihilation cross section beyond the present bounds from DM indirect detection searches. In our analysis we assumed WIMPs that annihilate to Standard Model particles through an s-wave process. For the class of solutions that comply with WIMP indirect detection bounds, we find that dEGB typically plays a mitigating role on the scalar field dynamics at high temperature, slowing down the speed of its evolution and reducing the enhancement of the Hubble constant compared to its standard value. For such solutions, we observe that the corresponding boundary conditions at high temperature correspond asymptotically to a vanishing deceleration parameter q, so that the effect of dEGB is to add an accelerating term that exactly cancels the deceleration predicted by General Relativity. The bounds from WIMP indirect detection are nicely complementary to late-time constraints from compact binary mergers. This suggests that it could be interesting to use other Early Cosmology processes to probe the dEGB scenario.
17
Khlopov, Maxim Yu. "Probes for dark matter physics." International Journal of Modern Physics D 27, no. 06 (April 2018): 1841013. http://dx.doi.org/10.1142/s0218271818410134.
Повний текст джерелаАнотація:
The existence of cosmological dark matter is in the bedrock of the modern cosmology. The dark matter is assumed to be nonbaryonic and consists of new stable particles. Weakly Interacting Massive Particle (WIMP) miracle appeals to search for neutral stable weakly interacting particles in underground experiments by their nuclear recoil and at colliders by missing energy and momentum, which they carry out. However, the lack of WIMP effects in their direct underground searches and at colliders can appeal to other forms of dark matter candidates. These candidates may be weakly interacting slim particles, superweakly interacting particles, or composite dark matter, in which new particles are bound. Their existence should lead to cosmological effects that can find probes in the astrophysical data. However, if composite dark matter contains stable electrically charged leptons and quarks bound by ordinary Coulomb interaction in elusive dark atoms, these charged constituents of dark atoms can be the subject of direct experimental test at the colliders. The models, predicting stable particles with charge [Formula: see text] without stable particles with charges [Formula: see text] and [Formula: see text] can avoid severe constraints on anomalous isotopes of light elements and provide solution for the puzzles of dark matter searches. In such models, the excessive [Formula: see text] charged particles are bound with primordial helium in O-helium atoms, maintaining specific nuclear-interacting form of the dark matter. The successful development of composite dark matter scenarios appeals for experimental search for doubly charged constituents of dark atoms, making experimental search for exotic stable double charged particles experimentum crucis for dark atoms of composite dark matter.
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Kadota, Kenji, and Hiroyuki Tashiro. "Radio bounds on the mixed dark matter scenarios of primordial black holes and WIMPs." Journal of Cosmology and Astroparticle Physics 2022, no. 08 (August 1, 2022): 004. http://dx.doi.org/10.1088/1475-7516/2022/08/004.
Повний текст джерелаАнотація:
Abstract We study the synchrotron radio emission in the mixed dark matter scenarios consisting of the primordial black holes (PBHs) and the self-annihilating WIMPs (weakly interacting massive particles). The WIMPs can form the ultracompact minihalos around PBHs and the annihilation enhancement from these dense halos can lead to the efficient synchrotron radiation at the radio frequency in the presence of galactic magnetic fields. The upper bound of PBH fraction with respect to the total dark matter abundance is of order 10-8 ∼ 10-5 depending on the electroweak scale WIMP mass (mχ = 10 ∼ 1000 GeV) and the WIMP annihilation channel (e.g. a hadronic χχ ⟶ bb̅ or a leptonic χχ ⟶ e + e - channel). The PBH contribution to the total dark matter abundance is hence negligible when the other component of dark matter is composed of the conventional electroweak scale WIMPs.
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Visinelli, Luca. "(Non-)Thermal Production of WIMPs during Kination." Symmetry 10, no. 11 (October 26, 2018): 546. http://dx.doi.org/10.3390/sym10110546.
Повний текст джерелаАнотація:
Understanding the nature of the Dark Matter (DM) is one of the current challenges in modern astrophysics and cosmology. Knowing the properties of the DM particle would shed light on physics beyond the Standard Model and even provide us with details of the early Universe. In fact, the detection of such a relic would bring us information from the pre-Big Bang Nucleosynthesis (BBN) period, an epoch from which we have no direct data, and could even hint at inflation physics. In this work, we assume that the expansion rate of the Universe after inflation is governed by the kinetic energy of a scalar field ϕ , in the so-called “kination” model. Adding to previous work on the subject, we assume that the ϕ field decays into both radiation and DM particles, which we take to be Weakly Interacting Massive Particles (WIMPs). The present abundance of WIMPs is then fixed during the kination period through either a thermal “freeze-out” or “freeze-in” mechanism, or through a non-thermal process governed by the decay of ϕ . We explore the parameter space of this theory with the requirement that the present WIMP abundance provides the correct relic budget. Requiring that BBN occurs during the standard cosmological scenario sets a limit on the temperature at which the kination period ends. Using this limit and assuming the WIMP has a mass m χ = 100 GeV, we obtain that the thermally averaged WIMP annihilation cross section has to satisfy the constraints 4 × 10 − 16 GeV − 2 ≲ ⟨ σ v ⟩ ≲ 2 × 10 − 5 GeV − 2 in order for having at least one of the production mechanism to yield the observed amount of DM. This result shows how the properties of the WIMP particle, if ever measured, can yield information on the pre-BBN content of the Universe.
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Bai, Yu, Weichao Sun, and Chung-Lin Shan. "Effects of threshold energy on reconstructions of properties of low-mass WIMPs in direct dark matter detection experiments." International Journal of Modern Physics A 33, no. 20 (July 20, 2018): 1850120. http://dx.doi.org/10.1142/s0217751x18501208.
Повний текст джерелаАнотація:
In this paper, we revisit our model-independent methods developed for reconstructing properties of Weakly Interacting Massive Particles (WIMPs) by using measured recoil energies from direct Dark Matter detection experiments directly and take into account more realistically non-negligible threshold energy. All expressions for reconstructing the mass and the (ratios between the) spin-independent and the spin-dependent WIMP–nucleon couplings have been modified. We focus on low-mass ([Formula: see text] GeV) WIMPs and present the numerical results obtained by Monte Carlo simulations. Constraints caused by non-negligible threshold energy and technical treatments for improving reconstruction results will also be discussed.
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Acharyya, A., A. Archer, P. Bangale, J. T. Bartkoske, P. Batista, M. Baumgart, W. Benbow, et al. "Search for Ultraheavy Dark Matter from Observations of Dwarf Spheroidal Galaxies with VERITAS." Astrophysical Journal 945, no. 2 (March 1, 2023): 101. http://dx.doi.org/10.3847/1538-4357/acbc7b.
Повний текст джерелаАнотація:
Abstract Dark matter is a key piece of the current cosmological scenario, with weakly interacting massive particles (WIMPs) a leading dark matter candidate. WIMPs have not been detected in their conventional parameter space (100 GeV ≲M χ ≲ 100 TeV), a mass range accessible with current Imaging Atmospheric Cherenkov Telescopes. As ultraheavy dark matter (UHDM; M χ ≳ 100 TeV) has been suggested as an underexplored alternative to the WIMP paradigm, we search for an indirect dark matter annihilation signal in a higher mass range (up to 30 PeV) with the VERITAS γ-ray observatory. With 216 hr of observations of four dwarf spheroidal galaxies, we perform an unbinned likelihood analysis. We find no evidence of a γ-ray signal from UHDM annihilation above the background fluctuation for any individual dwarf galaxy nor for a joint-fit analysis, and consequently constrain the velocity-weighted annihilation cross section of UHDM for dark matter particle masses between 1 TeV and 30 PeV. We additionally set constraints on the allowed radius of a composite UHDM particle.
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Faulkner, John. "Constraints on central solar conditions from helioseismology and neutrino counts." Symposium - International Astronomical Union 123 (1988): 105–9. http://dx.doi.org/10.1017/s0074180900157845.
Повний текст джерелаАнотація:
Interesting joint constraints are placed on central solar conditions by the solar neutrino detection rate and the frequency separations of high-order, low-degree p-modes of pulsation. A new form of diagnostic diagram is introduced that illustrates the difficulty in standard theories of simultaneously satisfying these joint constraints. A model employing WIMPs (= weakly interacting massive particles) appears to be the only model extant capable of fitting both kinds of data. Unambiguous identification and fitting of g-modes can provide a further test of the WIMP model provided a certain caution is exercised.
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Shan, Chung-Lin. "Reconstructing the WIMP velocity distribution from direct dark matter detection data with a nonnegligible threshold energy." International Journal of Modern Physics D 24, no. 11 (September 6, 2015): 1550090. http://dx.doi.org/10.1142/s021827181550090x.
Повний текст джерелаАнотація:
In this paper, we investigate the modification of our expressions developed for the model-independent data analysis procedure of the reconstruction of the (time-averaged) one-dimensional velocity distribution of galactic weakly interacting massive particles (WIMPs) with a nonnegligible experimental threshold energy. Our numerical simulations show that, for a minimal reconstructable velocity of as high as [Formula: see text] km/s, our model-independent modification of the estimator for the normalization constant could provide precise reconstructed velocity distribution points to match the true WIMP velocity distribution with ≲ 10% bias.
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Khlopov, Maxim. "Cosmoparticle physics of dark matter." EPJ Web of Conferences 222 (2019): 01006. http://dx.doi.org/10.1051/epjconf/201922201006.
Повний текст джерелаАнотація:
The lack of confirmation for the existence of supersymmetric particles and Weakly Interacting Massive Particles (WIMPs) appeals to extension of the field of studies of the physical nature of dark matter, involving nonsupersymmetric and non-WIMP solutions. We briefly discuss some examples of such candidates in their relationship with extension of particle symmetry and pattern of symmetry breaking. We specify in the example of axion-like particles nontrivial features of cosmological reflection of the structure and pattern of Peccei-Quinn-like symmetry breaking. The puzzles of direct and indiect dark matter searches can find solution in the approach of composite dark matter. The advantages and open problems of this approach are specified. We note that detailed analysis of cosmological consequences of any extension of particle model that provides candidates for dark matter inevitably leads to nonstandard features in the corresponding cosmological scenario. It makes possible to use methods of cosmoparticle physics to study physical nature of the dark matter in the combination of its physical, astrophysical and cosmological signatures.
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Siripak, J., Y. Yan, U. Sawangwit, and N. Sangungsuk. "Machine learning application for dark matter - background classification in JUNO experiment." Journal of Physics: Conference Series 2431, no. 1 (January 1, 2023): 012094. http://dx.doi.org/10.1088/1742-6596/2431/1/012094.
Повний текст джерелаАнотація:
Abstract Jiangmen underground neutrino observatory (JUNO) has a potential to indirectly detect dark matter (DM), observing neutrino events from annihilations of DM trapped by the gravitational force in the solar core. Weakly interacting massive particle (WIMP) DM candidate with mass > 4 GeV has significant solar capture rate. In this work, we simulate JUNO neutrino events from the most dominated WIMP annihilation channel, τ τ − . Given the high-energy neutrinos from massive WIMPs, we extend the neutrino-nucleon interactions in the detector to include quasi-elastic (QE) and deep inelastic scatterings (DIS). The most challenging background events in the energy range above 100 MeV is the atmospheric neutrinos (atmo). The pulse shape discrimination (PSD) method is usually applied to distinguish between DM and atmo. In this work, we apply machine learning (ML) techniques to distinguish between the background (BG) atmo and DM neutrino events. We found that the random forest algorithm gives the best results. Using ML, the accuracy of DM-atmo events classification is 93.8% while similar f1-score could be achieved. On the other hand, only 78.1 % accuracy is obtained using conventional PSD with linear regression (LR). The upper limit for spin-dependent DM-proton cross-section σ χ p S D with the applied ML is 5.84 × 10−40 cm2 for a 10 GeV WIMP DM which is an improvement over the sensitivity of the LR method of by a factor of ∼ 2.8x.
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Throm, Maxwell, Reagan Thornberry, John Killough, Brian Sun, Gentill Abdulla, and Roland E. Allen. "Two natural scenarios for dark matter particles coexisting with supersymmetry." Modern Physics Letters A 34, no. 02 (January 20, 2019): 1930001. http://dx.doi.org/10.1142/s0217732319300015.
Повний текст джерелаАнотація:
We describe two natural scenarios in which both dark matter, weakly interacting massive particles (WIMPs) and a variety of supersymmetric partners should be discovered in the foreseeable future. In the first scenario, the WIMPs are neutralinos, but they are only one component of the dark matter, which is dominantly composed of other relic particles such as axions. (This is the multicomponent model of Baer, Barger, Sengupta and Tata.) In the second scenario, the WIMPs result from an extended Higgs sector and may be the only dark matter component. In either scenario, both the dark matter WIMP and a plethora of other neutral and charged particles await discovery at many experimental facilities. The new particles in the second scenario have far weaker cross-sections for direct and indirect detection via their gauge interactions, which are either momentum-dependent or second-order. However, as we point out here, they should have much stronger interactions via the Higgs. We estimate that their interactions with fermions will then be comparable to (although not equal to) those of neutralinos with a corresponding Higgs interaction. It follows that these newly proposed dark matter particles should be within the reach of emerging and proposed facilities for direct, indirect and collider-based detection.
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DRUKIER, A. K., and S. NUSSINOV. "TOWARDS DETECTION OF LOW MASS WIMPs (MWIMP<10GeV/c2): MINI-REVIEW." International Journal of Modern Physics A 28, no. 26 (October 20, 2013): 1330033. http://dx.doi.org/10.1142/s0217751x13300330.
Повний текст джерелаАнотація:
Weakly Interacting Massive Particles (WIMPs) may constitute most of the matter in the Universe. There are intriguing results from DAMA/LIBRA, CoGeNT and CRESST-II, and more recently CDMS-Si suggesting a relatively light dark matter candidate of mass <10 GeV /c2. At the same time, experiments using heavy nuclear targets such as CDMS-Ge and XENON detectors suggest that there is no DM candidates with MW>15 GeV /c2. We review the existing experiments and the problems associated with light mass WIMP detection. We find that all six experiments considered (DAMA, CoGeNT, CRESST, CDMS-Si, CDMS-Ge, XENON) are consistent if one assumes that the mass of WIMP is lower than expected: 3.4<MW<6.8 GeV /c2. This is followed by a discussion of the properties of "new" detectors, which may enable more reliable detection of low mass WIMPs.
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HE, XIAO-GANG, TONG LI, XUE-QIAN LI, JUSAK TANDEAN, and HO-CHIN TSAI. "CONSTRAINTS ON SCALAR DARK MATTER FROM DIRECT EXPERIMENTAL SEARCHES." International Journal of Modern Physics: Conference Series 01 (January 2011): 257–65. http://dx.doi.org/10.1142/s2010194511000377.
Повний текст джерелаАнотація:
The standard model (SM) plus a real gauge-singlet scalar field dubbed darkon (SM+D) is the simplest model possessing a weakly interacting massive particle (WIMP) dark-matter candidate. The upper limits for the WIMP-nucleon elastic cross-section as a function of WIMP mass from the recent XENON10 and CDMS II experiments rule out darkon mass ranges from 10 to (50, 70, 75) GeV for Higgs-boson masses of (120, 200, 350) GeV, respectively. This may exclude the possibility of the darkon providing an explanation for the gamma-ray excess observed in the EGRET data. We show that by extending the SM+D to a two-Higgs-doublet model plus a darkon the experimental constraints on the WIMP-nucleon interactions can be circumvented due to suppression occurring at some values of the product tan α tan β, with α being the neutral-Higgs mixing angle and tan β the ratio of vacuum expectation values of the Higgs doublets. We also comment on the implication of the darkon model for Higgs searches at the LHC.
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Renzi, G. "Search for dark matter from the centre of the Earth with 8 years of IceCube data." Journal of Instrumentation 16, no. 11 (November 1, 2021): C11012. http://dx.doi.org/10.1088/1748-0221/16/11/c11012.
Повний текст джерелаАнотація:
Abstract Neutrinos have been proved to be unique messengers in the understanding of fundamental physics processes, and in astrophysical data sets they may provide hints of physics beyond the Standard Model. For example, neutrinos could be the key to discerning between various dark matter models that are based on Weakly Interacting Massive Particles (WIMPs). WIMPs can scatter off standard matter nuclei in the vicinity of massive bodies such as the Sun or the Earth, lose velocity, and be gravitationally trapped in the center of the body. Self-annihilation of dark matter into Standard Model particles may produce an observable flux of neutrinos. For the case of the Earth, an excess of neutrinos coming from the center of the planet could indicate WIMP capture and annihilation at the Earth’s core. The IceCube Neutrino Observatory, located at the geographical South Pole, is sensitive to these excess neutrinos. A search has been conducted on 8 years of IceCube data, probing multiple dark matter channels and masses. With this analysis, we show that IceCube has world-leading sensitivity to the spin-independent dark matter-nucleon scattering cross section above a WIMP mass of 100 GeV.
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Cook, R. H. W., N. Seymour, K. Spekkens, N. Hurley-Walker, P. J. Hancock, M. E. Bell, J. R. Callingham, et al. "Searching for dark matter signals from local dwarf spheroidal galaxies at low radio frequencies in the GLEAM survey." Monthly Notices of the Royal Astronomical Society 494, no. 1 (March 17, 2020): 135–45. http://dx.doi.org/10.1093/mnras/staa726.
Повний текст джерелаАнотація:
ABSTRACT The search for emission from weakly interacting massive particle (WIMP) dark matter annihilation and decay has become a multipronged area of research not only targeting a diverse selection of astrophysical objects, but also taking advantage of the entire electromagnetic spectrum. The decay of WIMP particles into standard model particles has been suggested as a possible channel for synchrotron emission to be detected at low radio frequencies. Here, we present the stacking analysis of a sample of 33 dwarf spheroidal (dSph) galaxies with low-frequency (72–231 MHz) radio images from the GaLactic and Extragalactic All-sky Murchison Widefield Array (GLEAM) survey. We produce radial surface brightness profiles of images centred upon each dSph galaxy with background radio sources masked. We remove 10 fields from the stacking due to contamination from either poorly subtracted, bright radio sources or strong background gradients across the field. The remaining 23 dSph galaxies are stacked in an attempt to obtain a statistical detection of any WIMP-induced synchrotron emission in these systems. We find that the stacked radial brightness profile does not exhibit a statistically significant detection above the 95 per cent confidence level of ∼1.5 mJy beam−1. This novel technique shows the potential of using low-frequency radio images to constrain fundamental properties of particle dark matter.
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Belotsky, K. M., E. A. Esipova, M. Yu Khlopov, and M. N. Laletin. "Dark Coulomb binding of heavy neutrinos of fourth family." International Journal of Modern Physics D 24, no. 13 (November 2015): 1545008. http://dx.doi.org/10.1142/s021827181545008x.
Повний текст джерелаАнотація:
Direct dark matter searches put severe constraints on the weakly interacting massive particles (WIMPs). These constraints cause serious troubles for the model of stable neutrino of fourth generation with mass around 50[Formula: see text]GeV. Though the calculations of primordial abundance of these particles make them in the charge symmetric case a sparse subdominant component of the modern dark matter, their presence in the universe would exceed the current upper limits by several orders of the magnitude. However, if quarks and leptons of fourth generation possess their own Coulomb-like [Formula: see text]-interaction, recombination of pairs of heavy neutrinos and antineutrinos and their annihilation in the “neutrinium” atoms can play important role in their cosmological evolution, reducing their modern abundance far below the experimental upper limits. The model of stable fourth generation assumes that the dominant part of dark matter is explained by excessive [Formula: see text] antiquarks, forming [Formula: see text] charged clusters, bound with primordial helium in nuclear-interacting O-helium (OHe) dark atoms. The [Formula: see text] charge conservation implies generation of the same excess of fourth generation neutrinos, potentially dangerous WIMP component of this scenario. We show that due to [Formula: see text]-interaction recombination of fourth neutrinos with OHe hides these WIMPs from direct WIMP searches, leaving the negligible fraction of free neutrinos, what makes their existence compatible with the experimental constraints.
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Angevaare, J. R., G. Bertone, A. P. Colijn, M. P. Decowski, and B. J. Kavanagh. "Complementarity of direct detection experiments in search of light Dark Matter." Journal of Cosmology and Astroparticle Physics 2022, no. 10 (October 1, 2022): 004. http://dx.doi.org/10.1088/1475-7516/2022/10/004.
Повний текст джерелаАнотація:
Abstract Dark Matter experiments searching for Weakly interacting massive particles (WIMPs) primarily use nuclear recoils (NRs) in their attempt to detect WIMPs. Migdal-induced electronic recoils (ERs) provide additional sensitivity to light Dark Matter with 𝒪(GeV/c 2) masses. In this work, we use Bayesian inference to find the parameter space where future detectors like XENONnT and SuperCDMS SNOLAB will be able to detect WIMP Dark Matter through NRs, Migdal-induced ERs or a combination thereof. We identify regions where each detector is best at constraining the Dark Matter mass and spin independent cross-section and infer where two or more detection configurations are complementary to constraining these Dark Matter parameters through a combined analysis.
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Mahanta, Devabrat, and Debasish Borah. "WIMPy leptogenesis in non-standard cosmologies." Journal of Cosmology and Astroparticle Physics 2023, no. 03 (March 1, 2023): 049. http://dx.doi.org/10.1088/1475-7516/2023/03/049.
Повний текст джерелаАнотація:
Abstract We study the possibility of generating baryon asymmetry of the universe from dark matter (DM) annihilations during non-standard cosmological epochs. Considering the DM to be of weakly interacting massive particle (WIMP) type, the generation of baryon asymmetry via leptogenesis route is studied where WIMP DM annihilation produces a non-zero lepton asymmetry. Adopting a minimal particle physics model to realise this along with non-zero light neutrino masses, we consider three different types of non-standard cosmic history namely, (i) fast expanding universe, (ii) early matter domination and (iii) scalar-tensor theory of gravity. By solving the appropriate Boltzmann equations incorporating such non-standard history, we find that the allowed parameter space consistent with DM relic and observed baryon asymmetry gets enlarged with the possibility of lower DM mass in some scenarios. While such lighter DM can face further scrutiny at direct search experiments, the non-standard epochs offer complementary probes on their own.
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Basu, Arghyadeep, Nirupam Roy, Samir Choudhuri, Kanan K. Datta, and Debajyoti Sarkar. "Stringent constraint on the radio signal from dark matter annihilation in dwarf spheroidal galaxies using the TGSS." Monthly Notices of the Royal Astronomical Society 502, no. 2 (January 16, 2021): 1605–11. http://dx.doi.org/10.1093/mnras/stab120.
Повний текст джерелаАнотація:
ABSTRACT Weakly interacting massive particles (WIMPs) are considered to be one of the favoured dark matter candidates. Searching for any detectable signal due to the annihilation and decay of WIMPs over the entire electromagnetic spectrum has become a matter of interest for the last few decades. WIMP annihilation to Standard Model particles gives rise to a possibility of detection of this signal at low radio frequencies via synchrotron radiation. Dwarf spheroidal (dSphs) galaxies are expected to contain a huge amount of dark matter which makes them promising targets to search for such large scale diffuse radio emission. In this work, we present a stacking analysis of 23 dSph galaxies observed at low frequency (147.5 MHz) as part of the TIFR-GMRT Sky Survey (TGSS). The non-detection of any signal from these stacking exercises put very tight constraints on the dark matter parameters. The best limit comes from the novel method of stacking after scaling the radio images of the individual dSph galaxy fields after scaling them by the respective half-light radius. The constraint on the thermally averaged cross-section is below the thermal relic cross-section value over a range of WIMP mass for reasonable choices of relevant astrophysical parameters. Such analysis, using future deeper observation of individual targets as well as stacking, can potentially reveal more about the WIMP dark matter properties.
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Smith, Peter F. "Status of Experiments for Direct Detection of Galactic Dark Matter Particles." Symposium - International Astronomical Union 201 (2005): 312–21. http://dx.doi.org/10.1017/s0074180900216409.
Повний текст джерелаАнотація:
There is increasing evidence that the majority of dark matter is non-baryonic. Principal candidates are weakly interacting massive particles (WIMPS), axions, and neutrinos. There has been increasing effort on sensitive WIMP searches, motivated in particular by supersymmetry theory, which predicts a stable neutral particle in the mass range 10-1000 GeV. Interactions of these with normal matter would produce low energy nuclear recoils which could be observed by underground detectors capable of discriminating these from background. Current experimental progress is summarised, together with plans for more sensitive experiments. These include gaseous detectors with directional sensitivity, offering the prospect of a ‘dark matter telescope’ which would provide information on the dark matter velocity distribution. Axions could be detected by conversion to microwave photons, and experimental sensitivity is approaching the theoretically-required levels. Relic neutrinos could also form a component of the dark matter if any has a cosmologically significant mass, and the latter could be checked with a new detector able to detect the higher neutrino flavours from a Galactic supernova burst. More distant future possibilities are outlined for direct detection of relic neutrinos by coherent scattering.
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Vollmann, Martin, Volker Heesen, Timothy W. Shimwell, Martin J. Hardcastle, Marcus Brüggen, Günter Sigl, and Huub J. A. Röttgering. "Radio constraints on dark matter annihilation in Canes Venatici I with LOFAR†." Monthly Notices of the Royal Astronomical Society 496, no. 3 (June 13, 2020): 2663–72. http://dx.doi.org/10.1093/mnras/staa1657.
Повний текст джерелаАнотація:
ABSTRACT Dwarf galaxies are dark matter (DM) dominated and therefore promising targets for the search for weakly interacting massive particles (WIMPs), which are well-known candidates for DM. The annihilation of WIMPs produces ultrarelativistic cosmic ray electrons and positrons that emit synchrotron radiation in the presence of magnetic fields. For typical magnetic field strengths (few μG) and $\mathcal {O}$(GeV–TeV) WIMP masses, this emission peaks at hundreds of MHz. Here, we use the non-detection of 150-MHz radio continuum emission from the dwarf spheroidal galaxy Canes Venatici I with the Low-Frequency Array to derive constraints on the annihilation cross-section of WIMPs into primary electron–positron and other fundamental particle–antiparticle pairs. Our main underlying assumption is that the transport of the cosmic rays can be described by the diffusion approximation, thus requiring a non-zero magnetic field strength with small-scale structure. In particular, by adopting magnetic field strengths of $\mathcal {O}(1\, \mu$G) and diffusion coefficients $\sim \!10^{27}~\rm cm^2\, s^{-1}$, we obtain limits that are comparable with those set by the Fermi Large Area Telescope using gamma-ray observations of this particular galaxy. Assuming s-wave annihilation and WIMPs making up 100 per cent of the DM density, our benchmark limits exclude several thermal WIMP realizations in the [2, 20]-GeV mass range. We caution, however, that our limits for the cross-section are subject to enormous uncertainties that we also quantitatively assess. In particular, variations on the propagation parameters or on the DM halo can shift our limits up by several orders of magnitude (in the pessimistic scenario).
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GREEN, ANNE M. "ASTROPHYSICAL UNCERTAINTIES ON DIRECT DETECTION EXPERIMENTS." Modern Physics Letters A 27, no. 03 (January 30, 2012): 1230004. http://dx.doi.org/10.1142/s0217732312300042.
Повний текст джерелаАнотація:
Direct detection experiments are poised to detect dark matter in the form of weakly interacting massive particles (WIMPs). The signals expected in these experiments depend on the ultra-local WIMP density and velocity distribution. Firstly we review methods for modeling the dark matter distribution. We then discuss observational determinations of the local dark matter density, circular speed and escape speed, and the results of numerical simulations of Milky Way-like dark matter halos. In each case we highlight the uncertainties and assumptions made. We then overview the resulting uncertainties in the signals expected in direct detection experiments, specifically the energy, time and direction dependence of the event rate. Finally we conclude by discussing techniques for handling the astrophysical uncertainties when interpreting data from direct detection experiments.
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Lopes, José, and Ilídio Lopes. "Dark matter capture and annihilation in stars: Impact on the red giant branch tip." Astronomy & Astrophysics 651 (July 2021): A101. http://dx.doi.org/10.1051/0004-6361/202140750.
Повний текст джерелаАнотація:
Context. While stars have often been used as laboratories to study dark matter (DM), red giant branch (RGB) stars and all the rich phenomenology they encompass have frequently been overlooked by such endeavors. Aims. We study the capture, evaporation, and annihilation of weakly interacting massive particle (WIMP) DM in low-mass RGB stars (M = 0.8−1.4 M⊙). Methods. We used a modified stellar evolution code to study the effects of DM self-annihilation on the structure and evolution of low-mass RGB stars. Results. We find that the number of DM particles that accumulate inside low-mass RGB stars is not only constant during this phase of evolution, but also mostly independent of the stellar mass and to some extent stellar metallicity. Moreover, we find that the energy injected into the stellar core due to DM annihilation can promote the conditions necessary for helium burning and thus trigger an early end of the RGB phase. The premature end of the RGB, which is most pronounced for DM particles with mχ ≃ 100 GeV, is thus achieved at a lower helium core mass, which results in a lower luminosity at the tip of the red giant branch (TRGB). Although in the current WIMP paradigm, these effects are only relevant if the number of DM particles inside the star is extremely large, we find that for light WIMPs (mχ ≃ 4 GeV), relevant deviations from the standard TRGB luminosity (∼8%) can be achieved with conditions that can be realistic in the inner parsec of the Milky Way.
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Ebadi, Reza, Mason C. Marshall, David F. Phillips, Johannes Cremer, Tao Zhou, Michael Titze, Pauli Kehayias, et al. "Directional detection of dark matter using solid-state quantum sensing." AVS Quantum Science 4, no. 4 (December 2022): 044701. http://dx.doi.org/10.1116/5.0117301.
Повний текст джерелаАнотація:
Next-generation dark matter (DM) detectors searching for weakly interacting massive particles (WIMPs) will be sensitive to coherent scattering from solar neutrinos, demanding an efficient background-signal discrimination tool. Directional detectors improve sensitivity to WIMP DM despite the irreducible neutrino background. Wide-bandgap semiconductors offer a path to directional detection in a high-density target material. A detector of this type operates in a hybrid mode. The WIMP or neutrino-induced nuclear recoil is detected using real-time charge, phonon, or photon collection. The directional signal, however, is imprinted as a durable sub-micron damage track in the lattice structure. This directional signal can be read out by a variety of atomic physics techniques, from point defect quantum sensing to x-ray microscopy. In this Review, we present the detector principle as well as the status of the experimental techniques required for directional readout of nuclear recoil tracks. Specifically, we focus on diamond as a target material; it is both a leading platform for emerging quantum technologies and a promising component of next-generation semiconductor electronics. Based on the development and demonstration of directional readout in diamond over the next decade, a future WIMP detector will leverage or motivate advances in multiple disciplines toward precision dark matter and neutrino physics.
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Mizukoshi, K., T. Maeda, Y. Nakano, S. Higashino, and K. Miuchi. "Scintillation light increase of carbontetrafluoride gas at low temperature." Journal of Instrumentation 16, no. 12 (December 1, 2021): P12033. http://dx.doi.org/10.1088/1748-0221/16/12/p12033.
Повний текст джерелаАнотація:
Abstract Scintillation detector is widely used for the particle detection in the field of particle physics. Particle detectors containing fluorine-19 (19F) are known to have advantages for Weakly Interacting Massive Particles (WIMPs) dark matter search, especially for spin-dependent interactions with WIMPs due to its spin structure. In this study, the scintillation properties of carbontetrafluoride (CF4) gas at low temperature were evaluated because its temperature dependence of light yield has not been measured. We evaluated the light yield by cooling the gas from room temperature (300 K) to 263 K. As a result, the light yield of CF4 was found to increase by (41.0 ± 4.0stat. ± 6.6syst.)% and the energy resolution was also found to improve at low temperature.
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Bernal, Nicolás, and Yong Xu. "WIMPs during reheating." Journal of Cosmology and Astroparticle Physics 2022, no. 12 (December 1, 2022): 017. http://dx.doi.org/10.1088/1475-7516/2022/12/017.
Повний текст джерелаАнотація:
Abstract Weakly Interacting Massive Particles (WIMPs) are among the best-motivated dark matter candidates. In the standard scenario where the freeze-out happens well after the end of inflationary reheating, they are in tension with the severe experimental constraints. Here, we investigate the thermal freeze-out of WIMPs occurring during reheating, while the inflaton ϕ coherently oscillates in a generic potential ∝ ϕn . Depending on the value of n and the spin of the inflaton decaying products, the evolution of the radiation and inflaton energy densities can show distinct features, therefore, having a considerable impact on the freeze-out behavior of WIMPs. As a result of the injection of entropy during reheating, the parameter space compatible with the observed DM relic abundance is enlarged. In particular, the WIMP thermally averaged annihilation cross-section can be several magnitudes lower than that in the standard case. Finally, we discuss the current bounds from dark matter indirect detection experiments, and explore future challenges and opportunities.
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Eldridge, C., N. J. C. Spooner, A. G. McLean, J. Burns, T. Crane, A. C. Ezeribe, R. R. Marcelo Gregorio, and A. Scarff. "Directional dark matter readout with a novel multi-mesh ThGEM for SF6 negative ion operation." Journal of Instrumentation 18, no. 08 (August 1, 2023): P08021. http://dx.doi.org/10.1088/1748-0221/18/08/p08021.
Повний текст джерелаАнотація:
Abstract Direct searches for Weakly Interacting Massive Particle (WIMP) dark matter could greatly benefit from directional measurement of the expected induced nuclear recoils. Gas-based Time Projection Chambers (TPCs) offer potential for this, opening the possibility of measuring WIMP signals below the so-called neutrino floor but also of directional measurement of recoils induced by neutrinos from the Sun, for instance as proposed by the CYGNUS collaboration. Presented here for the first time are results from a Multi-Mesh Thick Gas Electron Multiplier (MM-ThGEM) using negative ion gases for operation with such a directional dark matter TPC. Negative ion drift gases are favoured for directionality due to their low diffusion characteristics. The multiple internal mesh structure is designed to provide a high gain amplification stage when coupled to future large area Micromegas, strip or pixel charge readout planes. Experimental results and simulations are presented of MM-ThGEM gain and functionality using low pressure pure CF4, SF6 and SF6:CF4 mixtures irradiated with alpha particles and 55Fe x-rays. The concept is found to work well, providing stable operation with gains over 103 in pure SF6.
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Cerdeño, D. G., C. Marcos, M. Peiró, M. Fornasa, C. Cuesta, E. García, C. Ginestra, et al. "Scintillating bolometers: A key for determining WIMP parameters." International Journal of Modern Physics A 29, no. 19 (July 30, 2014): 1443009. http://dx.doi.org/10.1142/s0217751x1443009x.
Повний текст джерелаАнотація:
In the last decade direct detection Dark Matter (DM) experiments have increased enormously their sensitivity and ton-scale setups have been proposed, especially using germanium and xenon targets with double readout and background discrimination capabilities. In light of this situation, we study the prospects for determining the parameters of Weakly Interacting Massive Particle (WIMP) DM (mass, spin-dependent (SD) and spin-independent (SI) cross-section off nucleons) by combining the results of such experiments in the case of a hypothetical detection. In general, the degeneracy between the SD and SI components of the scattering cross-section can only be removed using targets with different sensitivities to these components. Scintillating bolometers, with particle discrimination capability, very good energy resolution and threshold and a wide choice of target materials, are an excellent tool for a multitarget complementary DM search. We investigate how the simultaneous use of scintillating targets with different SD-SI sensitivities and/or light isotopes (as the case of CaF 2 and NaI ) significantly improves the determination of the WIMP parameters. In order to make the analysis more realistic we include the effect of uncertainties in the halo model and in the spin-dependent nuclear structure functions, as well as the effect of a thermal quenching different from 1.
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Drukier, A. K., R. L. Fagaly, and R. Bielski. "Nano-booms — A new class of WIMP detectors." International Journal of Modern Physics A 29, no. 19 (July 30, 2014): 1443006. http://dx.doi.org/10.1142/s0217751x14430064.
Повний текст джерелаАнотація:
Weakly Interacting Massive Particles (WIMPs) can constitute a large fraction of the dark matter (DM) in the universe. The importance of coherent scattering and detection of annual modulation effect (AME), diurnal modulation effect (DME) and direction sensitive AME was documented. In particular, DAMA/NaI and DAMA/LIBRA have released data collected during 14 annual cycles, which support in model independent way, the presence of DM particles in the galactic halo. There is a clear evidence of AME signature in DAMA data. Recently, positive hints have also been reported by CoGeNT on AME signature in Ge, while CREST-II and CDMS-Si have published some events in excess of estimated background; these events are compatible with WIMP-like candidates. If these results would be analyzed all together in some WIMP scenario, one could derive: M DM < 10 GeV /c2. Current generation of detectors is far from being optimal or in some cases even reliable when M DM approaches 5 GeV /c2. We propose a detector, which can detect the direction of incoming WIMPs. This paper focus on a particular implementation of the new class of nano-explosive DM detectors. The local heating ignites an explosion, which release chemical energy stored in such a nano-grain. Use of two component nano-explosive permits to amplify the bolometric effect due to WIMP-candidates. The energy available becomes 100,000-fold larger than the energy initially deposited by DM candidate. This leads to a sonic-boom, which can be detected remotely. This new class of nano-explosive detectors may be especially important in detection of WIMPs with very low mass, say M DM = O (5 GeV /c2). We describe a configuration, which leads to explosive-triode, and permits detection of the direction of incoming WIMPs.
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KHLOPOV, MAXIM YU. "PHYSICS OF DARK MATTER IN THE LIGHT OF DARK ATOMS." Modern Physics Letters A 26, no. 38 (December 14, 2011): 2823–39. http://dx.doi.org/10.1142/s0217732311037194.
Повний текст джерелаАнотація:
Direct searches for dark matter lead to serious problems for simple models with stable neutral Weakly Interacting Massive Particles (WIMPs) as candidates for dark matter. A possibility is discussed that new stable quarks and charged leptons exist and are hidden from detection, being bound in neutral dark atoms of composite dark matter. Stable -2 charged particles O -- are bound with primordial helium in O-helium (OHe) atoms, being specific nuclear interacting form of composite Warmer than Cold dark matter. Slowed down in the terrestrial matter, OHe is elusive for direct methods of underground dark matter detection based on the search for effects of nuclear recoil in WIMP-nucleus collisions. The positive results of DAMA experiments can be explained as annual modulation of radiative capture of O-helium by nuclei. In the framework of this approach, test of DAMA results in detectors with other chemical content becomes a nontrivial task, while the experimental search of stable charged particles at LHC or in cosmic rays acquires a meaning of direct test for composite dark matter scenario.
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Sahu, R., and V. K. B. Kota. "Deformed shell model study of event rates for WIMP-73Ge scattering." Modern Physics Letters A 32, no. 38 (December 14, 2017): 1750210. http://dx.doi.org/10.1142/s0217732317502108.
Повний текст джерелаАнотація:
The event detection rates for the Weakly Interacting Massive Particles (WIMP) (a dark matter candidate) are calculated with [Formula: see text]Ge as the detector. The calculations are performed within the deformed shell model (DSM) based on Hartree–Fock states. First, the energy levels and magnetic moment for the ground state and two low-lying positive parity states for this nucleus are calculated and compared with experiment. The agreement is quite satisfactory. Then the nuclear wave functions are used to investigate the elastic and inelastic scattering of WIMP from [Formula: see text]Ge; inelastic scattering, especially for the [Formula: see text] transition, is studied for the first time. The nuclear structure factors which are independent of supersymmetric model are also calculated as a function of WIMP mass. The event rates are calculated for a given set of nucleonic current parameters. The calculation shows that [Formula: see text]Ge is a good detector for detecting dark matter.
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MUÑOZ, CARLOS. "DARK MATTER DETECTION IN THE LIGHT OF RECENT EXPERIMENTAL RESULTS." International Journal of Modern Physics A 19, no. 19 (July 30, 2004): 3093–169. http://dx.doi.org/10.1142/s0217751x04018154.
Повний текст джерелаАнотація:
The existence of dark matter was suggested, using simple gravitational arguments, seventy years ago. Although we are now convinced that most of the mass in the Universe is indeed some nonluminous matter, we still do not know its composition. The problem of the dark matter in the Universe is reviewed here. Particle candidates for dark matter are discussed with particular emphasis on Weakly Interacting Massive Particles (WIMP's). Experiments searching for these relic particles, carried out by many groups around the world, are also reviewed, paying special attention to their direct detection by observing the elastic scattering on target nuclei through nuclear recoils. Finally, we concentrate on the theoretical models predicting WIMP's, and in particular on supersymmetric extensions of the standard model, where the leading candidate for WIMP, the neutralino, is present. There, we compute the cross-section for the direct detection of neutralinos, and compare it with the sensitivity of detectors. We mainly discuss supergravity, superstring and M theory scenarios.
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Carr, Bernard, Florian Kühnel, and Luca Visinelli. "Black holes and WIMPs: all or nothing or something else." Monthly Notices of the Royal Astronomical Society 506, no. 3 (July 8, 2021): 3648–61. http://dx.doi.org/10.1093/mnras/stab1930.
Повний текст джерелаАнотація:
ABSTRACT We consider constraints on primordial black holes (PBHs) in the mass range $(10^{-18}\!-\!10^{15})\, \mathrm{M}_{\odot }$ if the dark matter (DM) comprises weakly interacting massive particles (WIMPs) that form haloes around them and generate γ-rays by annihilations. We first study the formation of the haloes and find that their density profile prior to WIMP annihilations evolves to a characteristic power-law form. Because of the wide range of PBH masses considered, our analysis forges an interesting link between previous approaches to this problem. We then consider the effect of the WIMP annihilations on the halo profile and the associated generation of γ-rays. The observed extragalactic γ-ray background implies that the PBH DM fraction is $f^{}_{\rm PBH} \lesssim 2 \times 10^{-9}\, (m_{\chi } / {\rm TeV})^{1.1}$ in the mass range $2 \times 10^{-12}\, \mathrm{M}_{\odot }\, (m_{\chi } / {\rm TeV})^{-3.2} \lesssim M \lesssim 5 \times 10^{12}\, \mathrm{M}_{\odot }\, (m_{\chi } / {\rm TeV})^{1.1}$, where mχ and M are the WIMP and PBH masses, respectively. This limit is independent of M and therefore applies for any PBH mass function. For $M \lesssim 2\times 10^{-12}\, \mathrm{M}_{\odot }\, (m_{\chi }/ {\rm TeV})^{-3.2}$, the constraint on $f^{}_{\rm PBH}$ is a decreasing function of M and PBHs could still make a significant DM contribution at very low masses. We also consider constraints on WIMPs if the DM is mostly PBHs. If the merging black holes recently discovered by LIGO/Virgo are of primordial origin, this would rule out the standard WIMP DM scenario. More generally, the WIMP DM fraction cannot exceed 10−4 for $M \gt 10^{-9}\, \mathrm{M}_{\odot }$ and $m_{\chi } \gt 10\,$ GeV. There is a region of parameter space, with $M \lesssim 10^{-11}\, \mathrm{M}_{\odot }$ and $m_{\chi } \lesssim 100\,$ GeV, in which WIMPs and PBHs can both provide some but not all of the DM, so that one requires a third DM candidate.
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Alfaro, R., C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, et al. "Searching for TeV Dark Matter in Irregular Dwarf Galaxies with HAWC Observatory." Astrophysical Journal 945, no. 1 (March 1, 2023): 25. http://dx.doi.org/10.3847/1538-4357/acb5f1.
Повний текст джерелаАнотація:
Abstract We present the results of dark matter (DM) searches in a sample of 31 dwarf irregular (dIrr) galaxies within the field of view of the HAWC Observatory. dIrr galaxies are DM-dominated objects in which astrophysical gamma-ray emission is estimated to be negligible with respect to the secondary gamma-ray flux expected by annihilation or decay of weakly interacting massive particles (WIMPs). While we do not see any statistically significant DM signal in dIrr galaxies, we present the exclusion limits (95% C.L.) for annihilation cross section and decay lifetime for WIMP candidates with masses between 1 and 100 TeV. Exclusion limits from dIrr galaxies are relevant and complementary to benchmark dwarf Spheroidal (dSph) galaxies. In fact, dIrr galaxies are targets kinematically different from benchmark dSph, preserving the footprints of different evolution histories. We compare the limits from dIrr galaxies to those from ultrafaint and classical dSph galaxies previously observed with HAWC. We find that the constraints are comparable to the limits from classical dSph galaxies and ∼2 orders of magnitude weaker than the ultrafaint dSph limits.
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Regis, Marco. "A Novel Approach in the WIMP Quest: Cross-Correlation of Gamma-Ray Anisotropies and Cosmic Shear." Acta Polytechnica CTU Proceedings 1, no. 1 (December 4, 2014): 34–37. http://dx.doi.org/10.14311/app.2014.01.0034.
Повний текст джерелаАнотація:
We present the cross-correlation angular power spectrum of cosmic shear and gamma-rays produced by the annihilation/decay of Weakly Interacting Massive Particle (WIMP) dark matter (DM), and by astrophysical sources. We show that this observable can provide novel information on the composition of the Extra-galactic Gamma-ray Background (EGB), since the amplitude and shape of the cross-correlation signal depend on which class of sources is responsible for the gamma-ray emission. If the DM contribution to the EGB is significant (at least in a definite energy range), although compatible with current observational bounds, its strong correlation with the cosmic shear (since both signals peak at large halo masses) makes such signature potentially detectable by combining Fermi-LAT data with forthcoming galaxy surveys, like Dark Energy Survey and Euclid.