Articles de revues : « Dark Matter - Astroparticle Physics »

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BETTINI, A. « ASTROPARTICLE PHYSICS ». International Journal of Modern Physics A 22, n^o 30 (10 décembre 2007) : 5550–60. http://dx.doi.org/10.1142/s0217751x07038815.

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Astroparticle is a very wide, expanding, sector of Physics; this report covers only a fraction of it complementing the plenary reports of Y. Takahashi and K. Inoue. I will focus, in particular, on the experimental evidence of new physics, beyond the Standard Model. Astroparticle and accelerator experiments will give complementary tools in the search of new particles, like those of the dark matter, and new fundamental fields, like the inflaton.

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Palanque-Delabrouille, Nathalie. « Overview of astroparticle physics and dark matter searches ». International Journal of Modern Physics A 22, n^o 31 (20 décembre 2007) : 5735–46. http://dx.doi.org/10.1142/s0217751x07038979.

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We present a general overview of recent results in the searches for dark matter and dark energy. We discuss the observation of the collision between two clusters of galaxies, and the impact this has on the relevance of dark matter. We then present the final results from microlensing experiments, which aimed at detecting dark baryonic objects in the halo of our galaxy, and the status of direct searches for WIMPs. We present the evidence for dark energy which initially comes from experiments dedicated to the study of distant type Ia supernovae. The measure of the baryon acoustic oscillation, an independent probe of the evolution of our universe that has recently brought interesting constraints, is finally described.

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Ko, Pyungwon. « Particle, Astroparticle Physics and Cosmology in Dark Matter Models with Dark Gauge Symmetries ». Journal of the Korean Physical Society 73, n^o 4 (août 2018) : 449–65. http://dx.doi.org/10.3938/jkps.73.449.

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Cho, A. « ASTROPARTICLE PHYSICS : Excess Particles From Space May Hint at Dark Matter ». Science 322, n^o 5905 (21 novembre 2008) : 1173. http://dx.doi.org/10.1126/science.322.5905.1173.

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Tinyakov, Peter, Maxim Pshirkov et Sergei Popov. « Astroparticle Physics with Compact Objects ». Universe 7, n^o 11 (25 octobre 2021) : 401. http://dx.doi.org/10.3390/universe7110401.

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Probing the existence of hypothetical particles beyond the Standard model often deals with extreme parameters: large energies, tiny cross-sections, large time scales, etc. Sometimes, laboratory experiments can test required regions of parameter space, but more often natural limitations lead to poorly restrictive upper limits. In such cases, astrophysical studies can help to expand the range of values significantly. Among astronomical sources, used in interests of fundamental physics, compact objects—neutron stars and white dwarfs—play a leading role. We review several aspects of astroparticle physics studies related to observations and properties of these celestial bodies. Dark matter particles can be collected inside compact objects resulting in additional heating or collapse. We summarize regimes and rates of particle capturing as well as possible astrophysical consequences. Then, we focus on a particular type of hypothetical particles—axions. Their existence can be uncovered due to observations of emission originated due to the Primakoff process in magnetospheres of neutron stars or white dwarfs. Alternatively, they can contribute to the cooling of these compact objects. We present results in these areas, including upper limits based on recent observations.

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Bignell, L. J., E. Barberio, M. B. Froehlich, G. J. Lane, O. Lennon, I. Mahmood, F. Nuti et al. « SABRE and the Stawell Underground Physics Laboratory Dark Matter Research at the Australian National University ». EPJ Web of Conferences 232 (2020) : 01002. http://dx.doi.org/10.1051/epjconf/202023201002.

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The direct detection of dark matter is a key problem in astroparticle physics that generally requires the use of deep-underground laboratories for a low-background environment where the rare signals from dark matter interactions can be observed. This work reports on the Stawell Underground Physics Laboratory – currently under construction and the first such laboratory in the Southern Hemisphere – and the associated research program. A particular focus will be given to ANU’s contribution to SABRE, a NaI:Tl dark matter, direct detection experiment that aims to confirm or refute the long-standing DAMA result. Preliminary measurements of the NaI:Tl quenching factor and characterisation of the SABRE liquid scintillator veto are reported.

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Moulin, Emmanuel. « Astroparticle Physics with H.E.S.S. : recents results and nearfuture prospects ». EPJ Web of Conferences 209 (2019) : 01054. http://dx.doi.org/10.1051/epjconf/201920901054.

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H.E.S.S. is an array of five Imaging Atmospheric Cherenkov Telescopes located in Namibia. It is designed for observations of astrophysical sources emitting very-high-energy (VHE) gamma rays in the energy range from a few ten GeVs to several ten TeVs. The H.E.S.S. instrument consists of four identical 12 m diameter telescopes and a 28 m diameter telescope placed at the center of the array. An ambitious Astroparticle Physics program is being carried out by the H.E.S.S. collaboration searching for New Physics in the VHE gamma-ray sky. The program includes the search for WIMP dark matter and axion-like particles, tests of Lorentz invariance, cosmic-ray electron measurements, and search for intergalactic magnetic fields. I will present the latest results on dark matter search from the observations of the Galactic Centre region, the search for Lorentz invariance violation with the 2014 flare observation of Markarian 501, and the first measurement of the cosmic-ray electron spectrum up to 20 TeV. The future of the H.E.S.S. Astroparticle Physics program will be discussed.

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Edwards, Thomas D. P., et Christoph Weniger. « A fresh approach to forecasting in astroparticle physics and dark matter searches ». Journal of Cosmology and Astroparticle Physics 2018, n^o 02 (12 février 2018) : 021. http://dx.doi.org/10.1088/1475-7516/2018/02/021.

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Jacob, Maurice. « The coming of age of cosmophysics ». Anais da Academia Brasileira de Ciências 75, n^o 2 (juin 2003) : 135–55. http://dx.doi.org/10.1590/s0001-37652003000200002.

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''Cosmophysics'' as reviewed is a multidisciplinary domain which brings together astroparticle physics, fundamental physics in space and topics related to the structure and evolution of the Universe. It represents a growing interface between high-energy particle physics and astro-physics. This paper presents a general overview of the subject, focusing on cosmology, cosmic rays, dark matter searches and the soon-expected observation of gravitational waves.

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Lapi, Andrea, Tommaso Ronconi, Lumen Boco, Francesco Shankar, Nicoletta Krachmalnicoff, Carlo Baccigalupi et Luigi Danese. « Astroparticle Constraints from Cosmic Reionization and Primordial Galaxy Formation ». Universe 8, n^o 9 (10 septembre 2022) : 476. http://dx.doi.org/10.3390/universe8090476.

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We derived astroparticle constraints in different dark matter scenarios that are alternatives to cold dark matter (CDM): thermal relic warm dark matter, WDM; fuzzy dark matter, ψDM; self-interacting dark matter, SIDM; sterile neutrino dark matter, νDM. Our framework is based on updated determinations of the high-redshift UV luminosity functions for primordial galaxies to redshift z∼10, on redshift-dependent halo mass functions in the above DM scenarios from numerical simulations, and on robust constraints on the reionization history of the Universe from recent astrophysical and cosmological datasets. First, we built an empirical model of cosmic reionization characterized by two parameters, namely the escape fraction fesc of ionizing photons from primordial galaxies, and the limiting UV magnitude MUVlim down to which the extrapolated UV luminosity functions steeply increased. Second, we performed standard abundance matching of the UV luminosity function and the halo mass function, obtaining a relationship between UV luminosity and the halo mass, whose shape depends on an astroparticle quantity X specific to each DM scenario (e.g., WDM particle mass); we exploited such a relationship to introduce (in the analysis) a constraint from primordial galaxy formation, in terms of the threshold halo mass above which primordial galaxies can efficiently form stars. Third, we performed Bayesian inference on the three parameters fesc, MUVlim, and X via a standard MCMC technique, and compared the outcomes of different DM scenarios on the reionization history. We also investigated the robustness of our findings against educated variations of still uncertain astrophysical quantities. Finally, we highlight the relevance of our astroparticle estimates in predicting the behavior of the high-redshift UV luminosity function at faint, yet unexplored magnitudes, which may be tested with the advent of the James Webb Space Telescope.

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Votano, Lucia. « Origin and status of the Gran Sasso INFN Laboratory ». Modern Physics Letters A 29, n^o 36 (20 novembre 2014) : 1430040. http://dx.doi.org/10.1142/s0217732314300407.

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The Gran Sasso National Laboratory of INFN (LNGS) is the largest underground laboratory for astroparticle physics in the world. Located in Italy between the cities of L'Aquila and Teramo, 120 km far from Rome, is a research infrastructure mainly dedicated to astroparticle and neutrino physics. It offers the most advanced underground facility in terms of dimensions, complexity and completeness of its infrastructures. LNGS is one of the four national laboratories run by the Istituto Nazionale di Fisica Nucleare (INFN). The scientific program at LNGS is mainly focused on astroparticle, particle and nuclear physics. The laboratory presently hosts many experiments as well as R&D activities, including world-leading research in the fields of solar neutrinos, accelerator neutrinos (CNGS neutrino beam from CERN to Gran Sasso), dark matter (DM), neutrinoless double beta decay (2β0ν) and nuclear cross-section of astrophysical interest. Associate sciences like earth physics, biology and fundamental physics complement the activities. The laboratory is operated as an international science facility and hosts experiments whose scientific merit is assessed by an international advisory Scientific Committee. A review of the main experiments carried out at LNGS will be given, together with the most recent and relevant scientific results achieved.

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Domi, Alba, Simon Bourret et Liam Quinn. « Particle Physics with ORCA ». EPJ Web of Conferences 207 (2019) : 04003. http://dx.doi.org/10.1051/epjconf/201920704003.

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KM3NeT is a Megaton-scale neutrino telescope currently under construction at the bottom of the Mediterranean Sea. When completed, it will consist of two separate detectors: ARCA (Astroparticle Research with Cosmics in the Abyss), optimised for high-energy neutrino astronomy, and ORCA (Oscillation Research with Cosmics in the Abyss) for neutrino oscillation studies of atmospheric neutrinos. The main goal of ORCA is the determination of the neutrino mass ordering (NMO). Nevertheless it is possible to exploit ORCA’s configuration to make other important measurements, such as sterile neutrinos, non standard interactions, tau-neutrino appearance, neutrinos from Supernovae, Dark Matter and Earth Tomography studies. Part of these analyses are summarized here.

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Mavromatos, Nick E. « Small-Scale Cosmology “Crisis” and Self-Interacting Right-Handed Neutrino Warm Dark Matter ». EPJ Web of Conferences 182 (2018) : 01001. http://dx.doi.org/10.1051/epjconf/201818201001.

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In the lecture, I first review the basic problems of the ΔCDM model at small (galactic) scales, also known as “small-scale Cosmology crisis”, namely discrepancies between theoretical simulations and observations. I then argue how systems of righthanded neutrinos (RHN) with masses of order 50 keV in the galaxies can tackle these problems, provided appropriately strong RHN self-interactions are included. Such models may constitute interesting minimal extensions of the Standard Model. Combining galactic phenomenology with other astroparticle physics considerations of such models, one arrives at a narrow range 47 keVc-2 ≤ m ≤ 50 keVc-2 for the allowed mass m of RHN, thereby pointing towards the rôle of such particles as interesteding warm dark matter components.

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Ejiri, H. « Nuclear Spin Responses for Neutrinos in Astroparticle Physics ». International Journal of Modern Physics E 06, n^o 01 (mars 1997) : 1–43. http://dx.doi.org/10.1142/s0218301397000020.

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Nuclear spin responses are of vital importance for studies of neutrinos, weakly interacting particles and of weak interactions in nuclei. The physics objectives are concerned with lepton nuclear physics within and beyond the standard theory. Here nuclei, which consist of elementary particles in good quantum (eigen) states, are used as excellent micro-laboratories for studying fundamental particles and interactions. Subjects discussed include neutrinos(ν) and weak interactions, weakly interacting massive particles as candidates for dark matters (DM), and other related problems. Experimental studies of them are made by investigating ultra rare nuclear processes at low background underground laboratories. Nuclear responses relevant to electroweak processes, neutrinos, and weakly interacting massive particles are discussed. Nuclear spin isospin responses associated with axial charged weak currents are investigated by using charge-exchange spin flip nuclear reactions at the RCNP ring cyclotron laboratory.

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Robens, Tania. « The THDMa Revisited ». Symmetry 13, n^o 12 (6 décembre 2021) : 2341. http://dx.doi.org/10.3390/sym13122341.

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The THDMa is a new physics model that extends the scalar sector of the Standard Model by an additional doublet as well as a pseudoscalar singlet and allows for mixing between all possible scalar states. In the gauge-eigenbasis, the additional pseudoscalar serves as a portal to the dark sector, with a priori any dark matter spins states. The option where dark matter is fermionic is currently one of the standard benchmarks for the experimental collaborations, and several searches at the LHC constrain the corresponding parameter space. However, most current studies constrain regions in parameter space by setting all but 2 of the 12 free parameters to fixed values. In this work, we performed a generic scan on this model, allowing all parameters to float. We applied all current theoretical and experimental constraints, including bounds from current searches, recent results from B-physics, in particular Bs→Xsγ, as well as bounds from astroparticle physics. We identify regions in the parameter space which are still allowed after these were applied and which might be interesting for an investigation of current and future collider machines.

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Gandolfi, Giovanni, Andrea Lapi, Tommaso Ronconi et Luigi Danese. « Astroparticle Constraints from the Cosmic Star Formation Rate Density at High Redshift : Current Status and Forecasts for JWST ». Universe 8, n^o 11 (7 novembre 2022) : 589. http://dx.doi.org/10.3390/universe8110589.

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We exploit the recent determination of the cosmic star formation rate (SFR) density at high redshifts z≳4 to derive astroparticle constraints on three common dark matter (DM) scenarios alternative to standard cold dark matter (CDM): warm dark matter (WDM), fuzzy dark matter (ψDM) and self-interacting dark matter (SIDM). Our analysis relies on the ultraviolet (UV) luminosity functions measured from blank field surveys by the Hubble Space Telescope out to z≲10 and down to UV magnitudes MUV≲−17. We extrapolate these to fainter yet unexplored magnitude ranges and perform abundance matching with the halo mass functions in a given DM scenario, thus, obtaining a redshift-dependent relationship between the UV magnitude and the halo mass. We then computed the cosmic SFR density by integrating the extrapolated UV luminosity functions down to a faint magnitude limit MUVlim, which is determined via the above abundance matching relationship by two free parameters: the minimum threshold halo mass MHGF for galaxy formation, and the astroparticle quantity X characterizing each DM scenario (namely, particle mass for WDM and ψDM, and kinetic temperature at decoupling TX for SIDM). We perform Bayesian inference on such parameters using a Monte Carlo Markov Chain (MCMC) technique by comparing the cosmic SFR density from our approach to the current observational estimates at z≳4, constraining the WDM particle mass to mX≈1.2−0.4(−0.5)+0.3(11.3) keV, the ψDM particle mass to mX≈3.7−0.4(−0.5)+1.8(+12.9.3)×10−22 eV, and the SIDM temperature to TX≈0.21−0.06(−0.07)+0.04(+1.8) keV at 68% (95%) confidence level. Finally, we forecast how such constraints will be strengthened by upcoming refined estimates of the cosmic SFR density if the early data on the UV luminosity function at z≳10 from the James Webb Space Telescope (JWST) will be confirmed down to ultra-faint magnitudes.

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Mohamad, Zulfakri, Koji Ishidoshiro, Yasuhiro Kishimoto, Satoru Mima, Tohru Taino, Keishi Hosokawa, Kosuke Nakamura, Minori Eizuka, Ryota Ito et Hiroki Kawamura. « Progress of Kinetic Inductance Detectors on Calcium Fluoride for Astroparticle physics ». Journal of Physics : Conference Series 2374, n^o 1 (1 novembre 2022) : 012026. http://dx.doi.org/10.1088/1742-6596/2374/1/012026.

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Kinetic Inductance Detector (KID) is an exciting device that promises high sensitivity to photons from submillimeter waves to gamma-rays with large format arrays. The KID consists of a superconductor thin film microwave resonator combined with a transmission line. When energy accumulates, Cooper pairs in the superconductor films are broken. Then quasiparticles are produced. This change increases the kinetic inductance in the resonant circuits and can be monitored by the transmission line. We propose that Lumped Element KID (LEKID) is implemented on Calcium Fluoride (CaF2) substrate for next-generation astroparticle experiments. 48Ca is one of the double-beta decay nuclei, and 19F is sensitive to spin-dependent elastic scattering with dark matter. The LEKID on CaF2 can be cooled to 15mK using a dilution refrigerator. At this stage, the quality factors of the LEKID are about 500×103, and measurement for particle detection using 241Am particle irradiation is also demonstrated at this low temperature.

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Mukhanov, Viatcheslav, et Licia Verde. « JCAP 20th anniversary retrospective : editorial ». Journal of Cosmology and Astroparticle Physics 2023, n^o 06 (1 juin 2023) : 041. http://dx.doi.org/10.1088/1475-7516/2023/06/041.

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Abstract This year the Journal of Cosmology and Astroparticle Physics (JCAP) celebrates its 20th anniversary. “A journal by scientists for scientists” is the motto that has driven JCAP since its inception, which epitomises its philosophy of being an innovative and community-driven journal. Over the past two decades, JCAP has become one of the premier outlets for high-quality research, now publishing circa 800 papers per year, almost all of which are Open Access (either green or gold route), and with submissions originating from more than 60 countries around the world. JCAP encompasses theoretical, observational, and experimental areas as well as computation and simulation, and this special issue represents a testament to the role of the journal and its impact within the fields of cosmology and astroparticle physics. Over the years, JCAP has published influential papers on topics ranging from the early universe and dark matter to large-scale structure, gravitational waves and high-energy astrophysics, all of which are presented in this celebratory collection of the journal’s 20th year of publication.

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COCCIA, E. « UNDERGROUND LABORATORIES AND THEIR PHYSICS REACH ». International Journal of Modern Physics A 27, n^o 08 (30 mars 2012) : 1230008. http://dx.doi.org/10.1142/s0217751x12300086.

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Underground laboratories, shielded by the Earth's crust from the particles that rain down on the surface in the form of cosmic rays, provide the low radioactive background environment necessary to host key experiments in the field of particle and astroparticle physics, nuclear astrophysics and other disciplines that can profit of their characteristics and of their infrastructures. The cosmic silence condition existing in these laboratories allows the search for extremely rare phenomena and the exploration of the highest energy scales that cannot be reached with accelerators. Major fundamental challenges are within the scope of these laboratories, notably, understanding the properties of neutrinos and dark matter, and exploring the unification of the fundamental forces of nature. I will review the physics reach and briefly describe the main underground facilities that are presently in operation around the world.

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McGrath, Conor. « VERITAS Highlights 2022 ». Journal of Physics : Conference Series 2429, n^o 1 (1 février 2023) : 012015. http://dx.doi.org/10.1088/1742-6596/2429/1/012015.

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Abstract The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is an array of four 12 m Imaging Atmospheric Cherenkov Telescopes (IACTs), located at the Fred Lawrence Whipple Observatory in Arizona, USA, that has been in full array operation since 2007. VERITAS conducts research in a variety of areas including galactic science such as supernova remnants, pulsar wind nebulae, binary systems; extra-galactic science including jetted AGN, gamma-ray burst and fast radio burst searches; multimessenger follow-ups and astroparticle physics, including dark matter searches. This paper will cover recent VERITAS highlights and results.

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Settanta, Giulio. « JUNO Non-oscillation Physics ». Journal of Physics : Conference Series 2156, n^o 1 (1 décembre 2021) : 012109. http://dx.doi.org/10.1088/1742-6596/2156/1/012109.

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Abstract The JUNO observatory, a 20 kt liquid scintillator detector to be completed in 2021 in China, belongs to the next-generation of neutrino detectors, which share the common features of having a multi-ton scale and an energy resolution at unprecedented levels. Beside the ambitious goal of neutrino mass ordering determination, the JUNO Collaboration plans also to perform a wide series of other measurements in the neutrino and astroparticle fields, rare processes and searches for new physics. The detector characteristics will allow the detection of neutrinos from many sources, like supernovae, the Sun, atmospheric and geoneutrinos. Other potential studies accessible to JUNO include the search for exotic processes, such as nucleon decays, Dark Matter and magnetic monopoles interactions, light sterile neutrinos production. This work reviews the physics potential of JUNO about non-reactor neutrino sources, highlighting the unique contributions that the experiment will give to the various fields in the forthcoming years.

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Mazde, Kratika, et Luca Visinelli. « The interplay between the dark matter axion and primordial black holes ». Journal of Cosmology and Astroparticle Physics 2023, n^o 01 (1 janvier 2023) : 021. http://dx.doi.org/10.1088/1475-7516/2023/01/021.

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Abstract If primordial black holes (PBHs) had come to dominate the energy density of the early Universe when oscillations in the axion field began, we show that the relic abundance and expected mass range of the QCD axion would be greatly modified. Since the QCD axion is a potential candidate for dark matter (DM), we refer to it as the DM axion. We predominantly explore PBHs in the mass range (106 - 5× 108)g. We investigate the relation between the relic abundance of DM axions and the parameter space of PBHs. We numerically solve the set of Boltzmann equations, that governs the cosmological evolution during both radiation and PBH-dominated epochs, providing the bulk energy content of the early Universe. We further solve the equation of motion of the DM axion field to obtain its present abundance. Alongside non-relativistic production mechanisms, light QCD axions are generated from evaporating PBHs through the Hawking mechanism and could make up a fraction of the dark radiation (DR). If the QCD axion is ever discovered, it will give us insight into the early Universe and probe into the physics of the PBH-dominated era. We estimate the bounds on the model from DR axions produced via PBH evaporation and thermal decoupling, and we account for isocurvature bounds for the period of inflation where the Peccei-Quinn symmetry is broken. We assess the results obtained against the available CMB data and we comment on the forecasts from gravitational wave searches. We briefly state the consequences of PBH accretion and the uncertainties this may further add to cosmology and astroparticle physics modeling.

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Lamanna, Giovanni. « Astrophysics and Particle Physics in Space with the Alpha Magnetic Spectrometer ». Modern Physics Letters A 18, n^o 28 (14 septembre 2003) : 1951–66. http://dx.doi.org/10.1142/s0217732303011939.

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The Alpha Magnetic Spectrometer (AMS) is a high energy particle physics experiment in space scheduled to be installed on the International Space Station (ISS) by 2006 for a three-year mission. After a precursor flight of a prototype detector on board of the NASA Space Shuttle in June 1998, the construction of the detector in its final configuration is started and it will be completed by 2004. The purpose of this experiment is to provide a high statistics measurement of charged particles and nuclei in rigidity range 0.5 GV to few TV and to explore the high-energy (> 1 GeV ) gamma-ray sky. In this paper we describe the detector layout and present an overview of the main scientific goals both in the domain of astrophysics: cosmic-ray origin, age and propagation and the exploration of the most energetic gamma-ray sources; and in the domain of astroparticle: the anti-matter and the dark matter searches.

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Cappella, Fabio, et Antonella Incicchitti. « Techniques for Background Identification in the Search for Rare Processes with Crystal Scintillators ». Physics 3, n^o 2 (9 avril 2021) : 187–206. http://dx.doi.org/10.3390/physics3020015.

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In astroparticle, nuclear and subnuclear physics, low-counting experiments play an increasingly important role in the investigation of rare processes such as dark matter, double beta decay, some neutrino processes and low-background spectrometry. Extremely low-background features are more and more required to produce detectors and apparata of suitable sensitivity. Over time, a great deal of interest and attention in developing experimental techniques suitable to improve, verify and maintain the radiopurity of these detectors has arisen. In this paper, the characterization of inorganic crystal scintillators (such as, e.g., NaI(Tl), ZnWO4 and CdWO4) using α, β and γ radioactive sources and the main experimental techniques applied in the field to quantitatively identify the radioactive contaminants are highlighted; in particular, we focus on inorganic crystal scintillators, widely used in rare processes investigation, considering their applications at noncryogenic temperatures in the framework of the DAMA experiment activities at the Gran Sasso National Laboratory of the INFN (National Institute for Nuclear Physics, INFN).

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Mu, Wei, Xiaonu Xiong et Xiangdong Ji. « Corrigendum to ‘Scintillation efficiency for low energy nuclear recoils in liquid xenon dark matter detectors’ [Astroparticle Physics 61 (2015) 56-61] ». Astroparticle Physics 72 (janvier 2016) : 109. http://dx.doi.org/10.1016/j.astropartphys.2015.06.003.

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Pinfold, James L. « The MoEDAL experiment : a new light on the high-energy frontier ». Philosophical Transactions of the Royal Society A : Mathematical, Physical and Engineering Sciences 377, n^o 2161 (11 novembre 2019) : 20190382. http://dx.doi.org/10.1098/rsta.2019.0382.

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MoEDAL is a pioneering LHC experiment designed to search for anomalously ionizing messengers of new physics, such as the magnetic monopole. After a test run at 8 TeV centre-of-mass energy ( E cm ), it started official data taking at the LHC at an E cm of 13 TeV, in 2015. Its groundbreaking physics program defines a number of scenarios that yield potentially revolutionary insights into such foundational questions as: are there extra dimensions or new symmetries; what is the mechanism for the generation of mass; does magnetic charge exist; do topological particles exist; and what is the nature of dark matter? After a brief introduction, MoEDAL's progress to date will be reported, including its past, current and expected future physics output. Additionally, an upgrade to the MoEDAL detector consisting of two new subdetectors: MAPP (MoEDAL Apparatus for Penetrating Particles) now being prototyped at IP8; and MALL (MoEDAL Apparatus for very long-lived particles), will be presented. Finally, a possible astroparticle extension to MoEDAL, called Cosmic-MoEDAL, will be briefly described. This high altitude detector will allow the search for magnetic monopoles to be continued from the TeV scale to the GUT scale. This article is part of a discussion meeting issue ‘Topological avatars of new physics’.

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Smolyaninov, Igor I. « Oscillating Cosmological Force Modifies Newtonian Dynamics ». Galaxies 8, n^o 2 (22 mai 2020) : 45. http://dx.doi.org/10.3390/galaxies8020045.

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In the Newtonian limit of general relativity a force acting on a test mass in a central gravitational field is conventionally defined by the attractive Newtonian gravity (inverse square) term plus a small repulsive cosmological force, which is proportional to the slow acceleration of the universe expansion. In this paper we considered the cosmological-force correction due to fast quantum oscillations of the universe scale factor as a potential solution of the cosmological constant problem. These fast fluctuations of the cosmological scale factor violate Lorentz invariance at the Planck scale, and they induce strong changes to the current sign and magnitude of the average cosmological force, thus making it one of the potential probable causes for the modification of Newtonian dynamics in galaxy-scale systems. The modified cosmological force may be responsible for the recently discovered “cosmic-clock” behavior of disk galaxies in the low-redshift universe. The obtained results have strong implications for astroparticle physics since they demonstrate that typical galaxy rotation curves may be obtained without (or almost without) dark-matter particles.

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Felizardo, M. « A SIMPLE review ». International Journal of Modern Physics A 35, n^o 09 (30 mars 2020) : 2030005. http://dx.doi.org/10.1142/s0217751x20300057.

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The Superheated Instrument for Massive ParticLe searches (SIMPLE) consists of an astroparticle dark matter search experiment with large active mass superheated droplet detectors (SDDs), that are installed at the underground low noise laboratory in France (LSBB). Several factors made the use of SDDs an attractive approach for the detection of weakly interacting massive particles (WIMPs), namely their intrinsic insensitivity to minimally ionizing particles, high fluorine content, low cost and operation at near ambient pressure and temperature. The signal that arises from the droplet phase transition generates a millimetric-sized gas bubble that is recorded by acoustic means. I describe the SIMPLE detectors, their acoustic instrumentation and signal analysis, which generated several science measurements executed through several phases over the last 20 years: the Pilot Phase with an exposure of 0.19 kgd, Phase I with an exposure of 0.42 kgd, Phase II with an exposure of 18.24 kgd and, an intended Phase III with an expected exposure increasing from 100 to 2500 kgd to be executed with a bubble chamber.

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Asaoka, Y., O. Adriani, Y. Akaike, K. Asano, MG Bagliesi, E. Berti, G. Bigongiari et al. « The CALorimetric Electron Telescope (CALET) on the International Space Station : Results from the First Two Years of Operation ». EPJ Web of Conferences 208 (2019) : 13001. http://dx.doi.org/10.1051/epjconf/201920813001.

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The CALorimetric Electron Telescope (CALET) space experiment, which has been developed by Japan in collaboration with Italy and the United States, is a high-energy astroparticle physics mission on the International Space Station (ISS). The primary goals of the CALET mission include investigation of possible nearby sources of high-energy electrons, detailed study of galactic cosmic-ray acceleration and propagation, and search for dark matter signatures. With a long-term observation onboard the ISS, the CALET experiment measures the flux of cosmic-ray electrons (including positrons) up to 20 TeV, gamma-rays to 10 TeV, and nuclei up to 1,000 TeV based on its charge separation capability from Z = 1 to 40. Since the start of science operation in mid-October, 2015, a continuous observation has been maintained without any major interruptions. The number of triggered events over 10 GeV is nearly 20 million per month. By using the data obtained during the first two-years, here we present a summary of the CALET observations: 1) Electron+positron energy spectrum, 2) Nuclei analysis, 3) Gamma-ray observation with a characterization of the on-orbit performance. The search results for the electromagnetic counterparts of LIGO/Virgo gravitational wave events are also discussed.

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Homola, Piotr, Dmitriy Beznosko, Gopal Bhatta, Łukasz Bibrzycki, Michalina Borczyńska, Łukasz Bratek, Nikolay Budnev et al. « Cosmic-Ray Extremely Distributed Observatory ». Symmetry 12, n^o 11 (5 novembre 2020) : 1835. http://dx.doi.org/10.3390/sym12111835.

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The Cosmic-Ray Extremely Distributed Observatory (CREDO) is a newly formed, global collaboration dedicated to observing and studying cosmic rays (CR) and cosmic-ray ensembles (CRE): groups of at least two CR with a common primary interaction vertex or the same parent particle. The CREDO program embraces testing known CR and CRE scenarios, and preparing to observe unexpected physics, it is also suitable for multi-messenger and multi-mission applications. Perfectly matched to CREDO capabilities, CRE could be formed both within classical models (e.g., as products of photon–photon interactions), and exotic scenarios (e.g., as results of decay of Super-Heavy Dark Matter particles). Their fronts might be significantly extended in space and time, and they might include cosmic rays of energies spanning the whole cosmic-ray energy spectrum, with a footprint composed of at least two extensive air showers with correlated arrival directions and arrival times. As the CRE are predominantly expected to be spread over large areas and, due to the expected wide energy range of the contributing particles, such a CRE detection might only be feasible when using all available cosmic-ray infrastructure collectively, i.e., as a globally extended network of detectors. Thus, with this review article, the CREDO Collaboration invites the astroparticle physics community to actively join or to contribute to the research dedicated to CRE and, in particular, to pool together cosmic-ray data to support specific CRE detection strategies.

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Schroeder, Frank G., Alan Coleman, Johannes Eser, Eric Mayotte, Fred Sarazin, Dennis Soldin et Tonia M. Venters. « The Snowmass UHECR White Paper on Ultra-High-Energy Cosmic Rays ». EPJ Web of Conferences 283 (2023) : 01001. http://dx.doi.org/10.1051/epjconf/202328301001.

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This proceeding summarizes the talk given at the opening of the UHECR 2022 conference in L’Aquila on the whitepaper ‘Ultra-High-Energy Cosmic Rays: The Intersection of the Cosmic and Energy Frontiers’ [Astroparticle Physics 149 (2023) 102819 - arXiv:2205.05845] that has been prepared for the Snowmass survey in the USA. The whitepaper provides an overview of recent progress and open questions regarding the particle physics and astrophysics related to ultra-high-energy cosmic rays (UHECR) and outlines the connections between the particle and astrophysics aspects of cosmic rays. It also discusses what instrumentation is needed to address the major scientific questions in ultra-high-energy cosmic-ray physics. While the upgraded Pierre Auger Observatory and Telescope Array will remain the workhorses at the highest energies in the current decade, new experiments with significantly higher exposure are needed in the coming decade. Ground arrays featuring simultaneous detection of the position of the shower maximum and the size of the muonic component will enable particle astronomy by measuring the rigidity of individual events. They should be complemented by other detectors maximizing the total exposure. This can be achieved by a few next-generation experiments using the latest developments in detection and analysis techniques: GRAND as a ground-based radio array, and POEMMA as a space-borne stereo fluorescence telescope will feature complementary approaches to provide maximum exposure; IceCube-Gen2 with its surface array, and GCOS aim at increased statistics with high accuracy for particle physics and rigidity-based galactic and extra-galactic astrophysics. While designed to discover the astrophysical cosmic-ray sources at the highest energies, the same experiments also contribute to particle physics, e.g., by studying the muon puzzle in cosmic-ray air showers, and by their discovery potential for exciting new physics, such as certain Dark Matter candidates. With the full whitepaper available as a reference, this proceeding will briefly present the science cases of the experiments, highlighting their individual strengths and outlining how they complement each other.

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Bungau, C., B. Camanzi, J. Chamber, Y. Chen, D. B. Cline, R. Luscher, J. D. Lewin, P. F. Smith, N. J. T. Smith et H. Wang. « Erratum to : “Monte Carlo studies of combined shielding and veto techniques for neutron background reduction in underground dark matter experiments based on liquid noble gas targets” [Astroparticle Physics 23 (2005) 97–115] ». Astroparticle Physics 23, n^o 5 (juin 2005) : 535. http://dx.doi.org/10.1016/j.astropartphys.2005.03.002.

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Sushchov, O., P. Homola, N. Dhital, Ł. Bratek, P. Poznański, T. Wibig, J. Zamora-Saa et al. « Cosmic-Ray Extremely Distributed Observatory : a global cosmic ray detection framework ». Advances in Astronomy and Space Physics 7, n^o 1-2 (2017) : 23–29. http://dx.doi.org/10.17721/2227-1481.7.23-29.

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The main objective of the Cosmic-Ray Extremely Distributed Observatory (CREDO) is the detection and analysis of extended cosmic ray phenomena, so-called super-preshowers (SPS), using existing as well as new infrastructure (cosmic-ray observatories, educational detectors, single detectors etc.). The search for ensembles of cosmic ray events initiated by SPS is yet an untouched ground, in contrast to the current state-of-the-art analysis, which is focused on the detection of single cosmic ray events. Theoretical explanation of SPS could be given either within classical (e.g., photon-photon interaction) or exotic (e.g., Super Heavy Dark Matter decay or annihilation) scenarios, thus detection of SPS would provide a better understanding of particle physics, high energy astrophysics and cosmology. The ensembles of cosmic rays can be classified based on the spatial and temporal extent of particles constituting the ensemble. Some classes of SPS are predicted to have huge spatial distribution, a unique signature detectable only with a facility of the global size. Since development and commissioning of a completely new facility with such requirements is economically unwarranted and time-consuming, the global analysis goals are achievable when all types of existing detectors are merged into a worldwide network. The idea to use the instruments in operation is based on a novel trigger algorithm: in parallel to looking for neighbour surface detectors receiving the signal simultaneously, one should also look for spatially isolated stations clustered in a small time window. On the other hand, CREDO strategy is also aimed at an active engagement of a large number of participants, who will contribute to the project by using common electronic devices (e.g., smartphones), capable of detecting cosmic rays. It will help not only in expanding the geographical spread of CREDO, but also in managing a large manpower necessary for a more efficient crowd-sourced pattern recognition scheme to identify and classify SPS. A worldwide network of cosmic-ray detectors could not only become a unique tool to study fundamental physics, it will also provide a number of other opportunities, including space-weather or geophysics studies. Among the latter one has to list the potential to predict earthquakes by monitoring the rate of low energy cosmic-ray events. The diversity of goals motivates us to advertise this concept across the astroparticle physics community.

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Porter, Troy A., Robert P. Johnson et Peter W. Graham. « Dark Matter Searches with Astroparticle Data ». Annual Review of Astronomy and Astrophysics 49, n^o 1 (22 septembre 2011) : 155–94. http://dx.doi.org/10.1146/annurev-astro-081710-102528.

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Bertone, Gianfranco, Nassim Bozorgnia, Jong Soo Kim, Sebastian Liem, Christopher McCabe, Sydney Otten et Roberto Ruiz de Austri. « Identifying WIMP dark matter from particle and astroparticle data ». Journal of Cosmology and Astroparticle Physics 2018, n^o 03 (14 mars 2018) : 026. http://dx.doi.org/10.1088/1475-7516/2018/03/026.

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Ong, Rene A. « Astroparticle physics ». Physica Scripta T158 (1 décembre 2013) : 014022. http://dx.doi.org/10.1088/0031-8949/2013/t158/014022.

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Pérez Bertolli, C., C. Sarmiento-Cano et H. Asorey. « MUON FLUX ESTIMATION IN THE ANDES UNDERGROUND LABORATORY ». Anales AFA 32, n^o 4 (15 janvier 2022) : 106–11. http://dx.doi.org/10.31527/analesafa.2021.32.4.106.

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The ANDES Underground Laboratory is being planned and designed to be one of the largest and most shielded laboratories in the Southern Hemisphere, which will be located in the Andes Range, in the area of the current Paso AguaNegra that connects the provinces of San Juan (Argentina) and Elqui (Chile). The diversity of experiments that are being planned, including experiments for the direct and indirect search of dark matter and neutrino precision physics, requires a precise knowledge of the flux of high-energy atmospheric muons within the laboratory. These are produced during the interaction of astroparticles with energies between 1012and 1018eV denominated of high and ultra-high energy with the Earth’s atmosphere. In the high-energy component, muons with energies of tens of TeV can be found, capable of passing through thousands of meters of rock. Previous estimates made from reasonable assumptions about the type of rock expected in the area showed that the expected muon flux was compatible with other underground laboratories at an equivalent depth. In this work, extensive atmospheric showers flux simulations were performed at the laboratory site. Afterwards, there was a selection of those muons with sufficient energy to reach the laboratory-based on their angle of incidence and the height at which they enter the mountain. Then a transfer function was modeled using the new geological studies currently available that allow us to have a detailed model of the rock distribution inside the mountain. Finally, the interaction of these muons with the different types of rock was calculated numerically along their way to the laboratory using the continuous slowdown approximation, thus obtaining that the expected muon flux within the laboratory is 1,47±0,02 day−1m−2sr−1

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XU, RENXIN. « ASTRO-QUARK MATTER : A CHALLENGE FACING ASTROPARTICLE PHYSICS ». Modern Physics Letters A 23, n^o 17n20 (28 juin 2008) : 1629–42. http://dx.doi.org/10.1142/s021773230802803x.

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Quark matter both in terrestrial experiment and in astrophysics is briefly reviewed. Astrophysical quark matter could appear in the early Universe, in compact stars, and as cosmic rays. Emphasis is put on quark star as the nature of pulsars. Possible astrophysical implications of experiment-discovered sQGP are also concisely discussed.

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DeRocco, William, Marios Galanis et Robert Lasenby. « Dark matter scattering in astrophysical media : collective effects ». Journal of Cosmology and Astroparticle Physics 2022, n^o 05 (1 mai 2022) : 015. http://dx.doi.org/10.1088/1475-7516/2022/05/015.

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Abstract It is well-known that stars have the potential to be excellent dark matter detectors. Infalling dark matter that scatters within stars could lead to a range of observational signatures, including stellar heating, black hole formation, and modified heat transport. To make robust predictions for such phenomena, it is necessary to calculate the scattering rate for dark matter inside the star. As we show in this paper, for small enough momentum transfers, this requires taking into account collective effects within the dense stellar medium. These effects have been neglected in many previous treatments; we demonstrate how to incorporate them systematically, and show that they can parametrically enhance or suppress dark matter scattering rates depending on how dark matter couples to the Standard Model. We show that, as a result, collective effects can significantly modify the potential discovery or exclusion reach for observations of compact objects such as white dwarfs and neutron stars. While the effects are more pronounced for dark matter coupling through a light mediator, we show that even for dark matter coupling via a heavy mediator, scattering rates can differ by orders of magnitude from their naive values for dark matter masses ≲ 100 MeV. We also illustrate how collective effects can be important for dark matter scattering in more dilute media, such as the Solar core. Our results demonstrate the need to systematically incorporate collective effects in a wide range of astroparticle contexts; to facilitate this, we provide expressions for in-medium self-energies for a variety of different media, which are applicable to many other processes of interest (such as particle production).

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Perković, Dalibor, et Hrvoje Štefančić. « Dark sector unifications : Dark matter-phantom energy, dark matter - constant w dark energy, dark matter-dark energy-dark matter ». Physics Letters B 797 (octobre 2019) : 134806. http://dx.doi.org/10.1016/j.physletb.2019.134806.

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Sitenko, Yu A. « Chiral effects in magnetized quantum spinor matter in particle and astroparticle physics ». International Journal of Modern Physics A 33, n^o 34 (10 décembre 2018) : 1845020. http://dx.doi.org/10.1142/s0217751x18450203.

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Quantum spinor matter in extremal conditions (high densities and temperatures, presence of strong magnetic fields) have drawn the attention of researchers in diverse areas of contemporary physics, ranging from cosmology, high-energy and astroparticle physics to condensed matter physics. We study an impact of the confining boundary conditions on the properties of physical systems with hot dense magnetized ultrarelativistic spinor matter and elucidate a significant role of boundaries for such systems.

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FOOT, R., et Z. K. SILAGADZE. « SUPERNOVA EXPLOSIONS, 511 keV PHOTONS, GAMMA RAY BURSTS AND MIRROR MATTER ». International Journal of Modern Physics D 14, n^o 01 (janvier 2005) : 143–51. http://dx.doi.org/10.1142/s0218271805006523.

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There are three astroparticle physics puzzles which fire the imagination: the origin of the "Great Positron Producer" in the galactic bulge, the nature of the gamma-ray bursts central engine and the mechanism of supernova explosions. We show that the mirror matter model has the potential to solve all three of these puzzles in one beautifully simple strike.

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de la Macorra, A. « Dark group : dark energy and dark matter ». Physics Letters B 585, n^o 1-2 (avril 2004) : 17–23. http://dx.doi.org/10.1016/j.physletb.2004.02.006.

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Einasto, Jaan. « Dark Matter ». Brazilian Journal of Physics 43, n^o 5-6 (27 juin 2013) : 369–74. http://dx.doi.org/10.1007/s13538-013-0147-9.

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Ramachers, Yorck. « Dark Matter ». Europhysics News 32, n^o 6 (novembre 2001) : 242–44. http://dx.doi.org/10.1051/epn:2001615.

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Comelli, D., M. Pietroni et A. Riotto. « Dark energy and dark matter ». Physics Letters B 571, n^o 3-4 (octobre 2003) : 115–20. http://dx.doi.org/10.1016/j.physletb.2003.05.006.

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Khuri, Ramzi R. « Dark matter as dark energy ». Physics Letters B 568, n^o 1-2 (août 2003) : 8–10. http://dx.doi.org/10.1016/j.physletb.2003.06.051.

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Spergel, David N. « Dark matter ». Nuclear Physics B - Proceedings Supplements 13 (février 1990) : 66–74. http://dx.doi.org/10.1016/0920-5632(90)90038-v.

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Cheek, Andrew. « Dark Matter Physics in Neutrino Telescopes and Neutrino Physics in Dark Matter Detectors ». Journal of Physics : Conference Series 2156, n^o 1 (1 décembre 2021) : 012215. http://dx.doi.org/10.1088/1742-6596/2156/1/012215.

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Abstract It is often the case that experiments built with a focus on a specific fundamental question are sensitive to a wider range of physical phenomena. In this proceedings I discuss two cases where new insights will come from experiments that have a different primary purpose. First, presents results from Ref. [1], which assesses what simple dark matter models will be uniquely probed by a upcoming Neutrino telescope inspired by KM3NeT. Given the existing constraints from γ-ray telescopes, measurements of the cosmic microwave background and direct dark matter detection, we focus on a secluded U(1)L μ − L γ model as particularly promising. Secondly, I present the results from Ref. [2], which describes how detecting solar neutrinos in direct dark matter detection experiments will be vital for confirming the possible U(1)L μ − L γ explanation of the anomalous magnetic moment of the muon.

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Srednicki, M. « Dark Matter ». European Physical Journal C 15, n^o 1-4 (mars 2000) : 143–44. http://dx.doi.org/10.1007/bf02683414.

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