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Artículos de revistas sobre el tema "Cosmic rays Measurement"

Autor: Grafiati

Publicado: 4 de junio de 2021

Última modificación: 19 de febrero de 2022

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1

Rossetto, L., S. Buitink, A. Corstanje, J. E. Enriquez, H. Falcke, J. R. Hörandel, A. Nelles, et al. "Measurement of cosmic rays with LOFAR." Journal of Physics: Conference Series 718 (May 2016): 052035. http://dx.doi.org/10.1088/1742-6596/718/5/052035.

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2

Mockler, Daniela. "Measurement of the cosmic ray spectrum with the Pierre Auger Observatory." EPJ Web of Conferences 209 (2019): 01029. http://dx.doi.org/10.1051/epjconf/201920901029.

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The flux of ultra-high energy cosmic rays above 3×1017 eV has been measured with unprecedented precision at the Pierre Auger Observatory. The flux of the cosmic rays is determined by four different measurements. The surface detector array provides three data sets, two formed by dividing the data into two zenith angle ranges, and one obtained from a nested, denser detector array. The fourth measurement is obtained with the fluorescence detector. By combing all four data sets, the all-sky flux of cosmic rays is determined. The spectral features are discussed in detail and systematic uncertainties are addressed.

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3

Norman, Colin A. "The Highest Energy Cosmic Rays." Symposium - International Astronomical Union 175 (1996): 291–96. http://dx.doi.org/10.1017/s0074180900080864.

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The current data on the highest energy cosmic rays (UHECRs) is discussed and an understanding of the origin of these particles is reviewed. New and proposed facilities for measurement of UHECRs, neutrinos and γ-rays can interestingly and significantly constrain the physics of the source origin. Cosmic magnetic field strengths are the most uncertain physical parameter.

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4

Nozzoli, Francesco, and Cinzia Cernetti. "Beryllium Radioactive Isotopes as a Probe to Measure the Residence Time of Cosmic Rays in the Galaxy and Halo Thickness: A “Data-Driven” Approach." Universe 7, no. 6 (June 4, 2021): 183. http://dx.doi.org/10.3390/universe7060183.

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Cosmic rays are a powerful tool for the investigation of the structure of the magnetic fields in the Galactic halo and the properties of the inter-stellar medium. Two parameters of the cosmic ray propagation models, the Galactic halo (half) thickness, H, and the diffusion coefficient, D, are loosely constrained by current cosmic ray flux measurements; in particular, a large degeneracy exists, with only H/D being well measured. The 10Be/9Be isotopic flux ratio (thanks to the 2 My lifetime of 10Be) can be used as a radioactive clock providing the measurement of cosmic ray residence time in a galaxy. This is an important probe with which to solve the H/D degeneracy. Past measurements of 10Be/9Be isotopic flux ratios in cosmic rays are scarce, and were limited to low energy and affected by large uncertainties. Here a new technique to measure 10Be/9Be isotopic flux ratio, with a data-driven approach in magnetic spectrometers is presented. As an example, by applying the method to beryllium events published via PAMELA experiment, it is now possible to determine the important 10Be/9Be measurement while avoiding the prohibitive uncertainties coming from Monte Carlo simulations. It is shown how the accuracy of PAMELA data strengthens the experimental indication for the relativistic time dilation of 10Be decay in cosmic rays; this should improve the knowledge of the H parameter.

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5

HARARI, DIEGO. "MEASUREMENTS OF COSMIC RAYS AT THE HIGHEST ENERGIES WITH THE PIERRE AUGER OBSERVATORY." International Journal of Modern Physics D 20, no. 05 (May 20, 2011): 685–96. http://dx.doi.org/10.1142/s0218271811019037.

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Measurements with the Pierre Auger Observatory indicate with unprecedented statistics that the flux of cosmic rays is strongly suppressed above 4 × 1019 eV. The suppression is consistent with the prediction that cosmic rays with larger energies can only arrive from nearby sources due to their interaction with the cosmic microwave background, but could also be related to the efficiency of the acceleration processes at the sources. The Observatory has found independent evidence of the nearby extragalactic origin of cosmic rays with energy above ~6×1019 eV with a measurement of the fraction of arrival directions that correlate with the positions of active galactic nuclei within ~100 Mpc. This correlation does not identify active galaxies as the sites of origin, since their distribution traces the overall local matter distribution. We review recent measurements made with the Pierre Auger Observatory of the flux, anisotropy and composition of CRs.

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6

An, Q., R. Asfandiyarov, P. Azzarello, P. Bernardini, X. J. Bi, M. S. Cai, J. Chang, et al. "Measurement of the cosmic ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite." Science Advances 5, no. 9 (September 2019): eaax3793. http://dx.doi.org/10.1126/sciadv.aax3793.

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The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with 2 1/2 years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time that an experiment directly measures the cosmic ray protons up to ~100 TeV with high statistics. The measured spectrum confirms the spectral hardening at ~300 GeV found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee and sheds new light on the origin of Galactic cosmic rays.

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7

Kostunin, D., P. A. Bezyazeekov, N. M. Budnev, D. Chernykh, O. Fedorov, O. A. Gress, A. Haungs, et al. "Present status and prospects of the Tunka Radio Extension." EPJ Web of Conferences 216 (2019): 01005. http://dx.doi.org/10.1051/epjconf/201921601005.

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The Tunka Radio Extension (Tunka-Rex) is a digital radio array operating in the frequency band of 30-80 MHz and detecting radio emission from air-showers produced by cosmic rays with energies above 100 PeV. The experimentis installed at the site of the TAIGA (Tunka Advanced Instrument for cosmic rays and Gamma Astronomy) observatory and performs joint measurements with the co-located particle and air-Cherenkov detectors in passive mode receiving a trigger from the latter. Tunka-Rex collects data since 2012, and during the last five years went throughseveral upgrades. As a result the density of the antenna field was increased by three times since its commission. In this contribution we present the latest results of Tunka-Rex experiment, particularly an updated analysis and efficiency study, which have been applied to the measurement of the mean shower maximum as a function of energy for cosmic rays of energies up to EeV. The future plans are also discussed: investigations towards an energy spectrum of cosmic rays with Tunka-Rex and their mass composition using a combination of Tunka-Rex data with muon measurements by the particle detector Tunka-Grande.

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8

Mariazzi, Analisa. "Highest energy particle physics with the Pierre Auger Observatory." International Journal of Modern Physics: Conference Series 31 (January 2014): 1460301. http://dx.doi.org/10.1142/s2010194514603019.

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Astroparticles offer a new path for research in the field of particle physics, allowing investigations at energies above those accesible with accelerators. Ultra-high energy cosmic rays can be studied via the observation of the showers they generate in the atmosphere. The Pierre Auger Observatory is a hybrid detector for ultra-high energy cosmic rays, combining two complementary measurement techniques used by previous experiments, to get the best possible measurements of these air showers. Shower observations enable one to not only estimate the energy, direction and most probable mass of the primary cosmic particles but also to obtain some information about the properties of their hadronic interactions. Results that are most relevant in the context of determining hadronic interaction characteristics at ultra-high energies will be presented.

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9

Oschlies, K., R. Beaujean, and W. Enge. "Measurement of low energy cosmic rays aboard Spacelab-1." International Journal of Radiation Applications and Instrumentation. Part D. Nuclear Tracks and Radiation Measurements 12, no. 1-6 (January 1986): 407–9. http://dx.doi.org/10.1016/1359-0189(86)90620-5.

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10

DE MELLO NETO, J. R. T. "ULTRA HIGH ENERGY COSMIC RAYS WITH THE PIERRE AUGER OBSERVATORY." International Journal of Modern Physics: Conference Series 18 (January 2012): 221–29. http://dx.doi.org/10.1142/s2010194512008495.

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We present the status and the recent measurements from the Pierre Auger Observatory. The energy spectrum is described and its features discussed. We report searches for anisotropy of cosmic rays arrival directions in large scales and through correlation with catalogues of celestial objects. The measurement of the cross section proton-air is discussed. Finally, the mass composition is addressed with the measurements of the variation of the depth of shower maximum with energy and with the muon density at ground.

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11

Fichtel, Carl E., Mehmet E. Ozel, and Robert G. Stone. "Cosmic Rays and the Dynamic Balance in the Large Magellanic Cloud." International Astronomical Union Colloquium 123 (1990): 537–41. http://dx.doi.org/10.1017/s0252921100077630.

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AbstractPresent and future measurement of the Large Magellanic Cloud (LMC) particularly in the radio and high energy gamma ray range offer the possibility of understanding the density and distribution of the cosmic rays in a galaxy other than our own and the role that they play in galactic dynamic balance. After a study of the consistency of the measurements and interpretation of the synchrotron radiation from our own galaxy, the cosmic ray distribution for the LMC is calculated under the assumption that the cosmic ray nucleon to electron ratio is the same and the relation to the magnetic fields are the same, although the implications of alternatives are discussed. It is seen that the cosmic ray density level appears to be similar to that in our own galaxy, but varying in position in a manner generally consistent with the concept of correlation with the matter on a broad scale.

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12

Martineau-Huynh, Olivier. "The GRAND project and GRANDProto300 experiment." EPJ Web of Conferences 210 (2019): 06007. http://dx.doi.org/10.1051/epjconf/201921006007.

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The Giant Array for Neutrino Detection (GRAND) is a proposal for a giant observatory of ultra-high energy cosmic particles (neutrinos, cosmic rays and gamma rays). It will be composed of twenty subarrays of 10 000 antennas each, totaling a detection area of 200 000 km2. GRAND will reach unprecedented sensitivity to neutrinos allowing to detect cosmogenic neutrinos while its sub-degree angular resolution will also make it possible to hunt for point sources and possibly start neutrino astronomy. Combined with its gigantic exposure to ultra-high energy cosmic rays and gamma rays, GRAND will be a powerful tool to solve the century-long mistery of the nature and origin of the particles with highest energy in the Universe. On the path to GRAND, the GRANDProto300 experiment will be deployed in 2020 over a total area of 200 km2. It primarly aims at validating the detection concept of GRAND, but also proposes a rich science program centered on a precise and complete measurement of the air showers initiated by cosmic rays with energies between 1016.5 and 1018 eV, a range where we expect to observe the transition between the Galactic and extra-galactic origin of cosmic rays.

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13

DI SCIASCIO, G. "MEASUREMENT OF COSMIC RAY SPECTRUM AND ANISOTROPY WITH ARGO-YBJ." International Journal of Modern Physics: Conference Series 23 (January 2013): 314–18. http://dx.doi.org/10.1142/s2010194513011549.

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In this paper we report on the observation of the anisotropy of cosmic ray arrival direction at different angular scales with ARGO-YBJ. Evidence of new few-degree excesses throughout the sky region 195° ≤ R.A. ≤ 315° is presented for the first time. We report also on the measurement of the light-component (p+He) spectrum of primary cosmic rays in the range 5–200 TeV.

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14

Bongi, M., O. Adriani, M. Ambriola, A. Bakaldin, G. C. Barbarino, A. Basili, G. Bazilevskaja, et al. "PAMELA: a satellite experiment for antiparticles measurement in cosmic rays." IEEE Transactions on Nuclear Science 51, no. 3 (June 2004): 854–59. http://dx.doi.org/10.1109/tns.2004.829504.

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15

Schröder, Frank G. "Physics Potential of a Radio Surface Array at the South Pole." EPJ Web of Conferences 216 (2019): 01007. http://dx.doi.org/10.1051/epjconf/201921601007.

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A surface array of radio antennas will enhance the performance of the IceTop array and enable new, complementary science goals. First, the accuracy for cosmic-ray air showers will be increased since the radio array provides a calorimetric measurement of the electromagnetic component and is sensitive to the position of the shower maximum. This enhanced accuracy can be used to better measure the mass composition, to search for possible mass-dependent anisotropies in the arrival directions of cosmic rays, and for more thorough tests of hadronic interaction models. Second, the sensitivity of the radio array to inclined showers will increase the sky coverage for cosmic-ray measurements. Third, the radio array can be used to search for PeV photons from the Galactic Center. Since IceTop is planned to be enhanced by a scintillator array in the near future, a radio extension sharing the same infrastructure can be installed with minimal additional effort and excellent scientific prospects. The combination of ice-Cherenkov, scintillation, and radio detectors at IceCube will provide unprecedented accuracy for the study of highenergy Galactic cosmic rays.

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16

Oka, Takeshi. "H 3 + , the ideal probe for in situ measurement of the Galactic cosmic rays." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 377, no. 2154 (August 5, 2019): 20180402. http://dx.doi.org/10.1098/rsta.2018.0402.

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The reason why H 3 + is an ideal probe for in situ measurement of cosmic ray energy density in the Galaxy is discussed. The variation of measured values of cosmic ray ionization rate ζ of H 2 since the theoretical prediction by Spitzer & Tomasko (Spitzer & Tomasko 1968 Astrophys. J. 152 , 971–986) is reviewed. How the measurements by H 3 + established ζ as of the order of 10 −17 s −1 for dense clouds, 10 −16 s −1 for diffuse clouds in the Galactic disc, and 10 −14 s −1 for warm and diffuse gas in the Galactic centre is discussed. This article is part of a discussion meeting issue ‘Advances in hydrogen molecular ions: H 3 + , H 5 + and beyond’.

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17

Petrera, Sergio. "Recent results from the Pierre Auger Observatory." EPJ Web of Conferences 208 (2019): 08001. http://dx.doi.org/10.1051/epjconf/201920808001.

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In this paper some recent results from the Pierre Auger Collaboration are presented. These are the measurement of the energy spectrum of cosmic rays over a wide range of energies (1017.5 to above 1020 eV), studies of the cosmic-ray mass composition with the fluorescence and surface detector of the Observatory, the observation of a large-scale anisotropy in the arrival direction of cosmic rays above 8 × 1018 eV and indications of anisotropy at intermediate angular scales above 4 × 1019 eV. The astrophysical implications of the spectrum and composition results are also discussed. Finally the progress of the upgrade of the Observatory, AugerPrime is presented.

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18

Timofeev, Lev, and Anatoly Ivanov. "EAS detection by wide-angle cherenkov telescopes at the Yakutsk array." EPJ Web of Conferences 208 (2019): 08015. http://dx.doi.org/10.1051/epjconf/201920808015.

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A proposed new method for measuring the Cherenkov light from extensive air showers (EAS) of cosmic rays (CR), which allows to determine not only the primary particle energy and angle of arrival, but also the parameters of the shower in the atmosphere - the maximum depth and “age”. For measurements, it is proposed to use Cherenkov light produced by EAS in a ground network of wide-angle telescopes, which are separated from each other by a distance 100-300 m depending on the total number of telescopes operating in coincidence, acting autonomously, or includes a detector of the charged components, radio waves, etc. as part of the EAS. The energy measurement and CR angle of arrival, data on the depth of the maximum and the associated mass of the primary particle generating the EAS is particularly important in the study of galactic cosmic rays for E> 1014 eV, where currently there are no direct measurements of the maximum depth of the EAS.

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19

Weinmann-Smith, R., M. T. Swinhoe, and J. Hendricks. "Measurement and simulation of cosmic rays effects on neutron multiplicity counting." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 814 (April 2016): 50–55. http://dx.doi.org/10.1016/j.nima.2016.01.012.

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20

Nobukawa, Kumiko K., Shigetaka Saji, Arisa Hirayama, Masayoshi Nobukawa, Shigeo Yamauchi, Hironori Matsumoto, and Katsuji Koyama. "Measurement of Low-Energy Cosmic Rays via the Neutral Iron Line." Journal of Physics: Conference Series 1181 (February 2019): 012040. http://dx.doi.org/10.1088/1742-6596/1181/1/012040.

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21

Lyu Qi-Wen, Zheng Yang-Heng, Tai Cai-Xing, Liu Fu-Hu, Cai Xiao, Fang Jian, Gao Long, et al. "The study of time-resolved measurement using ICCD positioning cosmic rays." Acta Physica Sinica 61, no. 7 (2012): 072904. http://dx.doi.org/10.7498/aps.61.072904.

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22

Kawai, H., S. Yoshida, J. H. Kim, S. Roh, Dongsu Ryu, H. Yoshii, S. Nam, et al. "Measurement of Ultra-High Energy Cosmic Rays by Telescope Array (TA)." Journal of the Physical Society of Japan 78, Suppl.A (January 2009): 108–13. http://dx.doi.org/10.1143/jpsjs.78sa.108.

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23

Xiong, Zhaohua, Hesheng Chen, Changgen Yang, Min Yang, Guomeng Chen, Gang Chen, Yusheng Lü, Honglin Zhuang, and Xiaowei Tang. "Measurement of3He/4He ratio in cosmic rays with the AMS experiment." Journal of High Energy Physics 2003, no. 11 (November 21, 2003): 048. http://dx.doi.org/10.1088/1126-6708/2003/11/048.

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24

Glaser, Christian. "ARIANNA: Measurement of cosmic rays with a radio neutrino detector in Antarctica." EPJ Web of Conferences 216 (2019): 02008. http://dx.doi.org/10.1051/epjconf/201921602008.

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The ARIANNA detector aims to detect neutrinos with energies above 1016 eV by instrumenting 0.5 Teratons of ice with a surface array of a thousand independent radio detector stations in Antarctica. The Antarctic ice is transparent to the radio signals caused by the Askaryan effect which allows for a cost-effective instrumentation of large volumes. Several pilot stations are currently operating successfully at the Moore’s Bay site (Ross Ice Shelf) and at the South Pole. As the ARIANNA detector stations are positioned at the surface, the more abundant cosmic-ray air showers are also measured and serve as a direct way to prove the capabilities of the detector. We will present measured cosmic rays and will show how the incoming direction, polarization and electric field of the cosmicray pulse can be reconstructed from single detector stations comprising 4 upward and 4 downward facing LPDA antennas.

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25

BERTUCCI, BRUNA. "REVIEW OF PRECISION MEASUREMENTS OF HIGH ENERGY ELECTRONS." International Journal of Modern Physics A 17, no. 12n13 (May 20, 2002): 1613–24. http://dx.doi.org/10.1142/s0217751x02011114.

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An accurate measurement of the intensity and energy spectra of Cosmic Ray electrons and positrons represents a major experimental challenge. Long exposure times and excellent particle identification capabilities are needed in order to cope with the low intensity of the electron and positron fluxes and the overwhelming background from protons and nuclei in cosmic rays. The motivations for such an experimental effort will be briefly discussed and the most recent results revieweved together with the perspectives of future experiments.

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26

Curceanu, Catalina, Diana Sirghi, Florin Sirghi, Sergio Bartalucci, Massimiliano Bazzi, Alberto Clozza, Luca De Paolis, et al. "Quantum mechanics under X-rays in the Gran Sasso underground laboratory." International Journal of Quantum Information 15, no. 08 (December 2017): 1740004. http://dx.doi.org/10.1142/s0219749917400044.

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By performing X-ray measurements in the “cosmic silence” of the underground laboratory of Gran Sasso, LNGS-INFN, we test a basic principle of quantum mechanics: the Pauli Exclusion Principle (PEP) for electrons. We present the achieved results of the VIP experiment and the ongoing VIP2 measurement aiming to gain two orders of magnitude improvement in testing PEP. X-ray emission can also be used to put strong constraints on the parameters of the Continuous Spontaneous Localization Model, which was introduced as a possible solution to the measurement problem in Quantum Mechanics. A Bayesian analysis of the data collected by IGEX will be presented, which allows to exclude a broad region of the parameter space which characterizes this model.

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27

Takeishi, Ryuji. "Observation of ultra-high energy cosmic rays with the Telescope Array experiment." EPJ Web of Conferences 182 (2018): 02122. http://dx.doi.org/10.1051/epjconf/201818202122.

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The origin of ultra-high energy cosmic rays (UHECRs) has been a longstanding mystery. The Telescope Array (TA) is the largest experiment in the northern hemisphere observing UHECR in Utah, USA. It aims to reveal the origin of UHECR by studying the energy spectrum, mass composition and anisotropy of cosmic rays. TA is a hybrid detector comprised of three air fluorescence stations which measure the fluorescence light induced from cosmic ray extensive air showers, and 507 surface scintillator counters which sample charged particles from air showers on the ground. We present the cosmic ray spectrum observed with the TA experiment. We also discuss our results from measurement of the mass composition. In addition, we present the results from the analysis of anisotropy, including the excess of observed events in a region of the northern sky at the highest energy. Finally, we introduce the TAx4 experiment which quadruples TA, and the TA low energy extension (TALE) experiment.

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28

Goto, Yuji. "Cross Section and Asymmetry Measurement of Very Forward Neutral Particle Production at RHIC." International Journal of Modern Physics: Conference Series 40 (January 2016): 1660110. http://dx.doi.org/10.1142/s2010194516601101.

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Although air shower observations at the surface of the earth have been developed in order to understand the origin of the ultra high energy cosmic rays, the observations have uncertainties in interpretation of the observed data from the present phenomenological nuclear collision models. Precision measurements of the very forward particle production in the collider experiments improve understanding of particle production processes in the nuclear collisions, and provide large influences on interpretation of the observed data and the origin of the cosmic rays. On the other hand, a large 10% single transverse-spin asymmetry in neutron production from transversely polarized proton collisions was found at the RHIC collider at BNL. It has provided a valuable input for understanding particle production processes in the polarized proton collisions. We will have a new collider experiment at RHIC which has a high resolution and a wide coverage of transverse momentum measurements in order to figure out elementary processes of the air shower generation.

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29

CASOLINO, MARCO. "LOW ENERGY SOLAR AND GALACTIC COSMIC RAYS AT 1 AU." International Journal of Modern Physics A 17, no. 12n13 (May 20, 2002): 1685–94. http://dx.doi.org/10.1142/s0217751x02011187.

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In this work we present some of the recent results obtained with the satellite missions NINA-1 and NINA-2 and the experiments on board MIR space station Sileye-1 and 2. The aim is the study of the low energy (10 MeV - 2 GeV) cosmic ray component and different periods of the solar cycle and during Solar Energetic Particle events. Other items of physics include the measurement of the secondary cosmic ray component, produced in the interaction with the upper layers of Earth's atmosphere and the evaluation of the absorbed and equivalent doses inside MIR.

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30

SCHIFFER, PETER. "ENERGY ORDERING EFFECTS IN THE ARRIVAL DIRECTIONS OF ULTRA-HIGH ENERGY COSMIC RAYS MEASURED BY THE PIERRE AUGER OBSERVATORY." International Journal of Modern Physics E 20, supp02 (December 2011): 50–56. http://dx.doi.org/10.1142/s021830131104058x.

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The Pierre Auger Observatory is the world's largest experiment for the measurement of ultra-high energy cosmic rays (UHECRs). These UHECRs are assumed to be to be charged particles, and thus are deflected in cosmic magnetic fields. Recent results of the Pierre Auger Observatory addressing the complex of energy ordering of the UHECRs arrival directions are reviewed in this contribution. So far no significant energy ordering has been observed.

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31

Cao, Z., L. L. Ma, S. S. Zhang, C. Wang, L. Q. Yin, and B. Y. Bi. "Measurement of knees of the spectra of heavy nuclei above 10 PeV with LHAASO." EPJ Web of Conferences 208 (2019): 14002. http://dx.doi.org/10.1051/epjconf/201920814002.

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Measuring the knees of the cosmic ray spectra for individual species is a very important approach to solve the problem of the origin of ultra high energy galactic cosmic rays. The knee of the iron spectrum is implied to be above 10 PeV from previous experiments, such as ARGO-YBJ and LHAASO-WFCTA. LHAASO is a suitable size for measurements with the required precision. The key is to separate iron nuclei from all cosmic ray samples. In this paper, we identify a couple of variables that are sensitive to the composition of showers recorded by the detector arrays in LHAASO. A multi variate analysis is proposed for the separation. The efficiency and purity of the selection for demanded species are optimized by well configuring the LHAASO array using the LHAASO simulation tools.

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32

Guardincerri, E., J. D. Bacon, N. Barros, C. Blasi, L. Bonechi, A. Chen, R. D'Alessandro, et al. "Imaging the dome of Santa Maria del Fiore using cosmic rays." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 377, no. 2137 (December 10, 2018): 20180136. http://dx.doi.org/10.1098/rsta.2018.0136.

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The dome of Santa Maria del Fiore, Florence Cathedral, was built between 1420 and 1436 by architect Filippo Brunelleschi and it is now cracking under its own weight. Engineering efforts are under way to model the dome's structure and reinforce it against further deterioration. According to some scholars, Brunelleschi might have built reinforcement structures into the dome itself; however, the only known reinforcement is a wood chain 7.75 m above the springing of the Cupola. Multiple scattering muon radiography is a non-destructive imaging method that can be used to image the interior of the dome's wall and therefore ascertain the layout and status of any iron substructure in it. A demonstration measurement was performed at the Los Alamos National Laboratory on a mock-up wall to show the feasibility of the work proposed, and a lightweight and modular imaging system is currently under construction. We will discuss here the results of the demonstration measurement and the potential of the proposed technique, describe the imaging system under construction and outline the plans for the measurement. This article is part of the Theo Murphy meeting issue ‘Cosmic-ray muography’.

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33

KODAIRA, S., M. HAREYAMA, N. HASEBE, T. MIYACHI, K. SAKURAI, W. R. BINNS, J. R. CUMMINGS, et al. "THE ATTENUATION LENGTH OF COSMIC RAY IRON IN THE ATMOSPHERE OBTAINED BY TIGER EXPERIMENT." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6702–4. http://dx.doi.org/10.1142/s0217751x05029861.

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A precise measurement of elemental abundances of galactic cosmic rays from charges Z = 20 to 34 was made by TIGER balloon experiment. Using the various path lengths in the atmosphere between 4 and 16 g/cm2 from the TIGER flight data, we derived the attenuation length of iron nuclei with the energy above 2.5 GeV/n in the atmosphere. As the result, we obtained the attenuation length of 15.5 ± 0.6 g/cm 2 which is consistent with previous results of balloon measurements.

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34

Garzón, Juan A. "TRASGOS: Towards a New Standard for the Regular Measurement of Cosmic Rays." Physics of Atomic Nuclei 83, no. 3 (May 2020): 453–62. http://dx.doi.org/10.1134/s1063778820030084.

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35

Fukushima, M. "Measurement of ultra-high energy cosmic rays: An experimental summary and prospects." EPJ Web of Conferences 53 (2013): 02002. http://dx.doi.org/10.1051/epjconf/20135302002.

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36

Prado, Raul R. "Tests of hadronic interactions with measurements by Pierre Auger Observatory." EPJ Web of Conferences 208 (2019): 08003. http://dx.doi.org/10.1051/epjconf/201920808003.

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The hybrid design of the Pierre Auger Observatory allows for the measurement of a number of properties of extensive air showers initiated by ultra-high energy cosmic rays. By comparing these measurements to predictions from air shower simulations, it is possible to both infer the cosmic ray mass composition and test hadronic interactions beyond the energies reached by accelerators. In this paper, we will present a compilation of results of air shower measurements by the Pierre Auger Observatory which are sensitive to the properties of hadronic interactions and can be used to constrain the hadronic interaction models. The inconsistencies found between the interpretation of different observables with regard to primary composition and between their measurements and simulations show that none of the currently used hadronic interaction models can provide a proper description of air showers and, in particular, of the muon production.

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37

Castellina, Antonella. "Auger Highlights." Acta Polytechnica CTU Proceedings 1, no. 1 (December 4, 2014): 132–38. http://dx.doi.org/10.14311/app.2014.01.0132.

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The Pierre Auger Observatory has been designed to investigate the origin and nature of the ultra high energy cosmic rays using a hybrid detection technique. A review of selected results is presented, with the emphasis given to the measurement of energy spectrum, mass composition and arrival directions.

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38

Abdalla, H., F. Aharonian, F. Ait Benkhali, E. O. Angüner, M. Arakawa, C. Arcaro, C. Armand, et al. "The starburst galaxy NGC 253 revisited by H.E.S.S. and Fermi-LAT." Astronomy & Astrophysics 617 (September 2018): A73. http://dx.doi.org/10.1051/0004-6361/201833202.

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Context. NGC 253 is one of only two starburst galaxies found to emit γ-rays from hundreds of MeV to multi-TeV energies. Accurate measurements of the very-high-energy (VHE; E > 100 GeV) and high-energy (HE; E > 60 MeV) spectra are crucial to study the underlying particle accelerators, probe the dominant emission mechanism(s) and to study cosmic-ray interaction and transport. Aims. The measurement of the VHE γ-ray emission of NGC 253 published in 2012 by H.E.S.S. was limited by large systematic uncertainties. Here, the most up to date measurement of the γ-ray spectrum of NGC 253 is investigated in both HE and VHE γ-rays. Assuming a hadronic origin of the γ-ray emission, the measurement uncertainties are propagated into the interpretation of the accelerated particle population. Methods. The data of H.E.S.S. observations are reanalysed using an updated calibration and analysis chain. The improved Fermi–LAT analysis employs more than 8 yr of data processed using pass 8. The cosmic-ray particle population is evaluated from the combined HE–VHE γ-ray spectrum using NAIMA in the optically thin case. Results. The VHE γ-ray energy spectrum is best fit by a power-law distribution with a flux normalisation of (1.34 ± 0.14stat ± 0.27sys) × 10−13 cm−2 s−1 TeV1 at 1 TeV – about 40% above, but compatible with the value obtained in Abramowski et al. (2012). The spectral index Γ = 2.39 ± 0.14stat ± 0.25sys is slightly softer than but consistent with the previous measurement within systematic errors. In the Fermi energy range an integral flux of F(E > 60 MeV) = (1.56 ± 0.28stat ± 0.15sys) × 10−8 cm−2 s−1 is obtained. At energies above ∼3 GeV the HE spectrum is consistent with a power-law ranging into the VHE part of the spectrum measured by H.E.S.S. with an overall spectral index Γ = 2.22 ± 0.06stat. Conclusions. Two scenarios for the starburst nucleus are tested, in which the gas in the starburst nucleus acts as either a thin or a thick target for hadronic cosmic rays accelerated by the individual sources in the nucleus. In these two models, the level to which NGC 253 acts as a calorimeter is estimated to a range of fcal = 0.1 to 1 while accounting for the measurement uncertainties. The presented spectrum is likely to remain the most accurate measurements until the Cherenkov Telescope Array (CTA) has collected a substantial set of data towards NGC 253.

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39

Roth, M. "Measurement of the energy spectrum of cosmic rays from the Pierre Auger Observatory." Nuclear Physics B - Proceedings Supplements 190 (May 2009): 12–19. http://dx.doi.org/10.1016/j.nuclphysbps.2009.03.062.

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40

Binns, W. R., R. G. Bose, D. L. Braun, T. J. Brandt, W. M. Daniels, P. F. Dowkontt, S. P. Fitzsimmons, et al. "THE SUPERTIGER INSTRUMENT: MEASUREMENT OF ELEMENTAL ABUNDANCES OF ULTRA-HEAVY GALACTIC COSMIC RAYS." Astrophysical Journal 788, no. 1 (May 16, 2014): 18. http://dx.doi.org/10.1088/0004-637x/788/1/18.

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41

Adriani, O., G. C. Barbarino, G. A. Bazilevskaya, R. Bellotti, M. Boezio, E. A. Bogomolov, M. Bongi, et al. "MEASUREMENT OF BORON AND CARBON FLUXES IN COSMIC RAYS WITH THE PAMELA EXPERIMENT." Astrophysical Journal 791, no. 2 (July 31, 2014): 93. http://dx.doi.org/10.1088/0004-637x/791/2/93.

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42

Karelin, A. V., O. Adriani, G. C. Barbarino, G. A. Bazilevskaya, R. Bellotti, M. Boezio, E. A. Bogomolov, et al. "Measurement of the large-scale anisotropy of cosmic rays in the PAMELA experiment." JETP Letters 101, no. 5 (March 2015): 295–98. http://dx.doi.org/10.1134/s0021364015050136.

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43

Pacini, Lorenzo, and Nicola Mori. "CaloCube and “Tracker In Calorimeter” projects for the direct measurement of high energy charged astro-particles and gamma rays." EPJ Web of Conferences 209 (2019): 01039. http://dx.doi.org/10.1051/epjconf/201920901039.

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Measurements of high energy cosmic rays in the “knee” region (about 1015 eV) are currently available only with ground detectors: new observations of cosmic particles up to these energies with direct measurements are one of the main goals of the next generation space experiments. To achieve those aims, a large acceptance, good energy resolution and particle identification are needed. CaloCube is the design of a space borne calorimeter which is capable to accept particles coming from any direction, increasing the acceptance with respect to traditional telescopes. A good performance for both hadronic and electromagnetic showers is achieved with a 3-D sampling capability: the basic picture of CaloCube is a cubic homogeneous calorimeter which consists of cubic scintillating crystals. MC simulations, concerning different materials and geometrical configurations, and several beam tests with different versions of the CaloCube prototype have been employed to optimize both the detector design and the data analysis method. Taking advantage of the CaloCube project, the space experiment HERD (“High Energy Cosmic Radiation Detection”) will include a large acceptance cubic calorimeter with cubic LYSO crystals. It will be installed on-board of the Chinese space station around 2025. Beside the charged particle observations, high energy gamma-rays provide direct information about the galactic cosmic ray sources. A new project named “Tracker In Calorimeter” (TIC) was approved by INFN in 2017 with the main purpose of the optimization of the calorimeter design for the reconstruction of the gamma-ray direction, without the requirement of additional not homogeneous pre-shower detector. A TIC prototype was recently assembled and tested at the PS-CERN and SPS-CERN accelerators.

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44

Sofue, Yoshiaki, Yasuhiro Murata, and Wolfgang Reich. "Spectral Turn-Over of Radio Arc Filaments at 43 GHz: Magnetic Tubes of 4000-yr Old in the Galactic Center." International Astronomical Union Colloquium 140 (1994): 166–67. http://dx.doi.org/10.1017/s0252921100019382.

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The origin of the straight magnetic filaments in the Radio Arc near the Galactic Center is still controversial: either if they are permanent structure of constant configuration for a galactic-time scale, or they are temporary structure of short life time such as due to a sudden injection of cosmic rays or to sudden shock compression. Measurement of life time of the radio emitting cosmic ray electrons consisting the filaments is one of the crucial methods besides a time variation measurement of the fine structure of the filaments.In order to investigate possible spatial variation of spectral index at higher frequencies in the filaments, which might give information about the life time of cosmic ray electrons, we have performed high-resolution radio continuum observations at 43 GHz of the GO.18-0.04 region of the radio Arc near the galactic center using the Nobeyama Millimeter-wave Array. A detailed description of this work is given in Sofue et al. (1992).

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45

Sanguineti, Matteo, and Tommaso Chiarusi. "Measurement of the cosmic ray Moon shadow with the ANTARES detector." EPJ Web of Conferences 209 (2019): 01037. http://dx.doi.org/10.1051/epjconf/201920901037.

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The ANTARES detector is the largest neutrino telescope currently in operation in Mediterranean sea. One of the main goals of the ANTARES telescope is the search for point-like neutrino sources, so both the pointing accuracy and the angular resolution of the detector need a proper direct estimation. One possibility to evaluate the pointing performance of the detector is to analyse the shadow of the Moon, i.e. the deficit in the atmospheric muon flux in the direction of the Moon induced by absorption of cosmic rays. The ANTARES data taken between 2007 and 2016 shows aMoon shadow evidence of 3.5σ significance. This is the first measurement of the ANTARES angular resolution and absolute pointing for atmospheric muons using a celestial calibration source. The presented results confirm the good pointing performance of the detector as well as the predicted angular resolution.

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46

Cernetti, Cinzia, and Francesco Nozzoli. "A Data Driven Approach to the Measurement of 10Be/9Be in Cosmic Rays with Magnetic Spectrometers." Physical Sciences Forum 2, no. 1 (February 22, 2021): 13. http://dx.doi.org/10.3390/ecu2021-09273.

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Cosmic Rays (CRs) are powerful tools for the investigation of the structure of the magnetic fields in the galactic halo and the properties of the Inter-Stellar Medium. There are two parameters of CR propagation models: The galactic halo (half-) thickness, H, and the diffusion coefficient, D, are loosely constrained by current CR flux measurements; in particular, a large degeneracy exists, as only H/D is well measured. The 10Be/9Be isotopic flux ratio (thanks to the 2 My lifetime of 10Be) can be used as a radioactive clock that provides the measurement of the residence time of CRs in the galaxy. This is an important tool for solving the degeneracy of H/D. Past measurements of the 10Be/9Be isotopic flux ratios in CRs are scarce, limited to low energy, and affected by large uncertainties. Here, a new technique for measuring the 10Be/9Be isotopic flux ratio in magnetic spectrometers with a data-driven approach is presented. As an example, by applying the method to beryllium events that were published by the PAMELA experiment, it is now possible to determine the important 10Be/9Be measurements while avoiding the prohibitive uncertainties coming from Monte Carlo simulations. It is shown how the accuracy of the PAMELA data permits one to infer a value of the halo thickness with a precision of up to 25%.

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47

Gorham, P. W., P. Allison, O. Banerjee, J. J. Beatty, K. Belov, D. Z. Besson, W. R. Binns, et al. "Antarctic Surface Reflectivity Measurements from the ANITA-3 and HiCal-1 Experiments." Journal of Astronomical Instrumentation 06, no. 02 (April 3, 2017): 1740002. http://dx.doi.org/10.1142/s2251171717400025.

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The primary science goal of the NASA-sponsored ANITA project is measurement of ultra-high energy neutrinos and cosmic rays, observed via radio-frequency signals resulting from a neutrino or cosmic ray interaction with terrestrial matter (e.g. atmospheric or ice molecules). Accurate inference of the energies of these cosmic rays requires understanding the transmission/reflection of radio wave signals across the ice–air boundary. Satellite-based measurements of Antarctic surface reflectivity, using a co-located transmitter and receiver, have been performed more-or-less continuously for the last few decades. Our comparison of four different reflectivity surveys, at frequencies ranging from 2 to 45[Formula: see text]GHz and at near-normal incidence, yield generally consistent maps of high versus low reflectivity, as a function of location, across Antarctica. Using the Sun as an RF source, and the ANITA-3 balloon borne radio-frequency antenna array as the RF receiver, we have also measured the surface reflectivity over the interval 200–1000[Formula: see text]MHz, at elevation angles of 12–30[Formula: see text]. Consistent with our previous measurement using ANITA-2, we find good agreement, within systematic errors (dominated by antenna beam width uncertainties) and across Antarctica, with the expected reflectivity as prescribed by the Fresnel equations. To probe low incidence angles, inaccessible to the Antarctic Solar technique and not probed by previous satellite surveys, a novel experimental approach (“HiCal-1”) was devised. Unlike previous measurements, HiCal-ANITA constitute a bi-static transmitter–receiver pair separated by hundreds of kilometers. Data taken with HiCal, between 200 and 600[Formula: see text]MHz shows a significant departure from the Fresnel equations, constant with frequency over that band, with the deficit increasing with obliquity of incidence, which we attribute to the combined effects of possible surface roughness, surface grain effects, radar clutter and/or shadowing of the reflection zone due to Earth curvature effects. We discuss the science implications of the HiCal results, as well as improvements planned for HiCal-2, preparing for launch in December 2016.

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48

Dimiccoli, F., L. Basara, K. Kanishchev, F. Nozzoli, and P. Zuccon. "Measurement of the D/p ratio in Cosmic rays with the AMS-02 experiment." Nuclear and Particle Physics Proceedings 306-308 (September 2019): 80–84. http://dx.doi.org/10.1016/j.nuclphysbps.2019.07.012.

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49

Panico, B., and G. Di Sciascio. "Measurement of the cosmic rays light component (p+He) primary spectrum with ARGO-YBJ." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 692 (November 2012): 155–59. http://dx.doi.org/10.1016/j.nima.2011.12.116.

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50

Bourrion, O., C. Bernard, D. Bondoux, J. L. Bouly, J. Bouvier, B. Boyer, M. Brinet, et al. "Design and construction of a Cherenkov imager for charge measurement of nuclear cosmic rays." Journal of Instrumentation 6, no. 06 (June 8, 2011): P06004. http://dx.doi.org/10.1088/1748-0221/6/06/p06004.

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