Journal articles: 'Cosmic ray; detector; anisotropy'

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Янчуковский, Валерий, Valery Yanchukovsky, Владислав Григорьев, Vladislav Grigoryev, Гермоген Крымский, Germogen Krymsky, Василий Кузьменко, Vasiliy Kuzmenko, Антон Молчанов, and Anton Molchanov. "Receiving vectors of muon telescope of cosmic ray station Novosibirsk." Solar-Terrestrial Physics 2, no. 1 (June 1, 2016): 103–19. http://dx.doi.org/10.12737/19883.

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The method of receiving vectors allows us to determine cosmic ray anisotropy at every moment of time. Also, the method makes it possible to study fast anisotropy fluctuations related to the interplanetary medium dynamics. Receiving vectors have been calculated earlier for neutron monitors and muon telescopes. However, most muon telescopes of the network of cosmic ray stations for which calculations were made does not operate now. In recent years, new, improved detectors have been developed. Unfortunately, the use of them is limited because of the absence of receiving coefficients. These detectors include a matrix telescope in Novosibirsk. Therefore, receiving vector components for muon telescopes of observation cosmic ray station Novosibirsk have been defined. Besides, design features of the facility, its orientation, and directional diagram depending on zenith and azimuth angles were taken into account. Also, for the system of telescopes, we allowed for coupling coefficients found experimentally by the test detector.

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Kawata, K., A. di Matteo, T. Fujii, D. Ivanov, C. C. H. Jui, J. P. Lundquist, J. N. Matthews, et al. "TA Anisotropy Summary." EPJ Web of Conferences 210 (2019): 01004. http://dx.doi.org/10.1051/epjconf/201921001004.

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The Telescope Array (TA) is the largest ultra-high-energy cosmic-ray (UHECR) detector in the northern hemisphere. It consists of an array of 507 surface detectors (SD) covering a total 700 km2 and three fluorescence detector stations overlooking the SD array. In this proceedings, we summarize recent results on the search for directional anisotropy of UHECRs using the latest dataset collected by the TA SD array. We obtained hints of the anisotropy of the UHECRs in the northern sky from the various analyses.

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Янчуковский, Валерий, Valery Yanchukovsky, Владислав Григорьев, Vladislav Grigoryev, Гермоген Крымский, Germogen Krymsky, Василий Кузьменко, Vasiliy Kuzmenko, Антон Молчанов, and Anton Molchanov. "Receiving vectors of muon telescope of cosmic ray station “Novosibirsk”." Solnechno-Zemnaya Fizika 2, no. 1 (March 17, 2016): 76–87. http://dx.doi.org/10.12737/16762.

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The method of receiving vectors allows us to determine cosmic ray anisotropy at each moment. Also, the method makes it possible to study fast anisotropy fluctuations related to the interplanetary medium dynamics. Receiving vectors have been calculated earlier for neutron monitors and muon telescopes. However, the most of muon telescopes of the network of cosmic ray stations for which calculations were made does not operate now. In recent years, new improved detectors appeared. Unfortunately, the use of them is limited because of absence of receiving coefficients. These detectors include the matrix telescope in Novosibirsk. Therefore, components of receiving vector for muon telescopes of observation cosmic ray station “Novosibirsk” have been defined. Besides, design features of the facility, its orientation, and directional diagram depending on zenith and azimuth angles were taken into account. Also, for the system of telescopes, we allowed for coupling coefficients found experimentally using the test detector.

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Hall, D. L., M. L. Duldig, and J. E. Humble. "The North–South Anisotropy and the Radial Density Gradient of Galactic Cosmic Rays at 1 AU." Publications of the Astronomical Society of Australia 12, no. 2 (August 1995): 153–58. http://dx.doi.org/10.1017/s1323358000020191.

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AbstractThe radial density gradient (Gr) of Galactic cosmic rays in the ecliptic plane points outward from the Sun. This indicates an increasing density of cosmic ray particles beyond the Earth’s orbit. Due to this gradient and the direction of the Sun’s interplanetary magnetic field (IMF) above and below the IMF wavy neutral sheet, there exists an anisotropic flow of cosmic ray particles approximately perpendicular to the ecliptic plane (i.e. in the direction parallel to BIMF × Gr). This effect is called the north–south anisotropy (ξNS) and manifests as a diurnal variation in sidereal time in the particle intensity recorded by a cosmic ray detector. By analysing the yearly averaged sidereal diurnal variation recorded by five neutron monitors and six muon telescopes from 1957 to 1990, we have deduced probable values of the average rigidity spectrum and magnitude of ξNS. Furthermore, we have used determined yearly amplitudes of ξNS to infer the magnitude of Gr for particles with rigidities in excess of 10 GV.

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Munakata, Kazuoki. "Probing the heliosphere with the directional anisotropy of galactic cosmic-ray intensity." Proceedings of the International Astronomical Union 7, S286 (October 2011): 185–94. http://dx.doi.org/10.1017/s1743921312004826.

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AbstractBecause of the large detector volume that can be deployed, ground-based detectors remain state-of-the-art instrumentation for measuring high-energy galactic cosmic-rays (GCRs). This paper demonstrates how useful information can be derived from observations of the directional anisotropy of the high-energy GCR intensity, introducing the most recent results obtained from the ground-based observations. The anisotropy observed with the global muon detector network (GMDN) provides us with a unique information of the spatial gradient of the GCR density which reflects the large-scale magnetic structure in the heliosphere. The solar cycle variation of the gradient gives an important information on the GCR transport in the heliosphere, while the short-term variation of the gradient enables us to deduce the large-scale geometry of the magnetic flux rope and the interplanetary coronal mass ejection (ICME). Real-time monitoring of the precursory anisotropy which has often been observed at the Earth preceding the arrival of the ICME accompanied by a strong shock may provide us with useful tools for forecasting the space weather with a long lead time. The solar cycle variation of the Sun's shadow observed in the TeV GCR intensity is also useful for probing the large-scale magnetic structure of the solar corona.

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Munakata, K., M. Kozai, C. Kato, Y. Hayashi, R. Kataoka, A. Kadokura, M. Tokumaru, et al. "Large-amplitude Bidirectional Anisotropy of Cosmic-Ray Intensity Observed with Worldwide Networks of Ground-based Neutron Monitors and Muon Detectors in 2021 November." Astrophysical Journal 938, no. 1 (October 1, 2022): 30. http://dx.doi.org/10.3847/1538-4357/ac91c5.

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Abstract We analyze the cosmic-ray variations during a significant Forbush decrease observed with worldwide networks of ground-based neutron monitors and muon detectors during 2021 November 3–5. Utilizing the difference between primary cosmic-ray rigidities monitored by neutron monitors and muon detectors, we deduce the rigidity spectra of the cosmic-ray density (or omnidirectional intensity) and the first- and second-order anisotropies separately for each hour of data. A clear two-step decrease is seen in the cosmic-ray density with the first ∼2% decrease after the interplanetary shock arrival followed by the second ∼5% decrease inside the magnetic flux rope (MFR) at 15 GV. Most strikingly, a large bidirectional streaming along the magnetic field is observed in the MFR with a peak amplitude of ∼5% at 15 GV, which is comparable to the total density decrease inside the MFR. The bidirectional streaming could be explained by adiabatic deceleration and/or focusing in the expanding MFR, which have stronger effects for pitch angles near 90°, or by selective entry of GCRs along a leg of the MFR. The peak anisotropy and density depression in the flux rope both decrease with increasing rigidity. The spectra vary dynamically, indicating that the temporal variations of density and anisotropy appear different in neutron monitor and muon detector data.

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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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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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TAMBURRO, ALESSIO. "MEASUREMENTS OF COSMIC RAYS WITH ICETOP/ICECUBE: STATUS AND RESULTS." Modern Physics Letters A 27, no. 39 (December 13, 2012): 1230038. http://dx.doi.org/10.1142/s0217732312300388.

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The IceCube Observatory at the South Pole is composed of a cubic kilometer scale neutrino telescope buried beneath the icecap and a square-kilometer surface water Cherenkov tank detector array known as IceTop. The combination of the surface array with the in-ice detector allows the dominantly electromagnetic signal of air showers at the surface and their high-energy muon signal in the ice to be measured in coincidence. This ratio is known to carry information about the nuclear composition of the primary cosmic rays. This paper reviews the recent results from cosmic-ray measurements performed with IceTop/IceCube: energy spectrum, mass composition, anisotropy, search for PeV γ sources, detection of high energy muons to probe the initial stages of the air shower development, and study of transient events using IceTop in scaler mode.

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Kyratzis, Dimitrios. "Overview of the HERD space mission." Physica Scripta 97, no. 5 (April 12, 2022): 054010. http://dx.doi.org/10.1088/1402-4896/ac63fc.

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Abstract The High Energy cosmic Radiation Detector (HERD) is a prominent space-borne instrument to be installed on-board the Chinese Space Station (CSS) around 2027, resulting from a collaboration among Chinese and European institutions. Primary scientific goals of HERD include: precise measurements of the cosmic ray (CR) energy spectra and mass composition at energies up to few PeV, electron/positron spectra up to tens of TeV, CR anisotropy, gamma ray astronomy and transient studies, along with indirect searches for Dark Matter candidates. The detector is configured to accept incident particles from both its top and four lateral sides. Owing to its pioneering design, more than one order of magnitude increase in geometric acceptance is foreseen, with respect to previous and ongoing experiments. HERD is conceived around a deep (∼55 X 0, 3 λ I ) 3D cubic calorimeter (CALO), forming an octagonal prism. Fiber Trackers (FiTs) are instrumented on all active sides, with a Plastic Scintillator Detector (PSD) covering the calorimeter and tracker. Ultimately, a Silicon Charge Detector (SCD) envelops the above-stated sub-detectors, while a Transition Radiation Detector (TRD) is instrumented on one of its lateral faces, for energy calibration in the TeV scale. This work illustrates HERD’s latest advancements and scientific objectives along with an overview of upcoming activities.

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Munakata, K., T. Kuwabara, J. W. Bieber, P. Evenson, R. Pyle, S. Yasue, C. Kato, et al. "CME-geometry and cosmic-ray anisotropy observed by a prototype muon detector network." Advances in Space Research 36, no. 12 (January 2005): 2357–62. http://dx.doi.org/10.1016/j.asr.2003.05.064.

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Ogio, Shoichi. "Telescope Array Experiment." EPJ Web of Conferences 208 (2019): 08002. http://dx.doi.org/10.1051/epjconf/201920808002.

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The Telescope Array is the largest hybrid cosmic ray detector in the Northern hemisphere designed to measure primary particles in 4 PeV to 100 EeV range. The main TA detector consists of an air shower array of 507 plastic scintillation counters on a 1.2 km square grid and fluorescence detectors at three stations overlooking the sky above the air shower array. The experiment and its recent measurements - spectrum, composition, and anisotropy - is reviewed. Recently the construction of the TA Low energy Extension (TALE) detector, which consists of an additional fluorescence detector and an infill array, was finished. TALE lowers the energy threshold of TA down to 4 PeV. We are also constructing the TAx4 detector to increase statistics in particular at the highest energies. The current status and the future prospects of these new TAx4 experiments is reported.

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SOKOLSKY, PIERRE. "ULTRA-HIGH ENERGY COSMIC RAYS." Modern Physics Letters A 19, no. 13n16 (May 30, 2004): 959–66. http://dx.doi.org/10.1142/s0217732304014240.

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We describe the current status of the High Resolution Fly's Eye detector. Recent results indicate that the UHE cosmic ray spectrum exhibits significant structure near 1019 eV. A few events are seen beyond 1020 eV in contradiction to the AGASA ground array claim of no cut-off. The composition of the cosmic rays is found to change from a predominantly heavy to a predominantly light mixture between and 1017 and 1018 eV. No evidence for anisotropy, on either small scales or large scales is found, in contradiction to AGASA. Systematic errors and absolute energy scale issues are now being carefully considered to see how to partially resolve this discrepancy. A new experiment(FLASH) at the Stanford Linear Accelerator Center (SLAC) to measure the Nitrogen fluorescence efficiency more precisely is described.

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Cutler, D. J., and D. E. Groom. "Mayflower Mine 1500 GV detector - Cosmic-ray anisotropy and search for Cygnus X-3." Astrophysical Journal 376 (July 1991): 322. http://dx.doi.org/10.1086/170282.

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Grigoryev, Vladislav, Sardaana Gerasimova, Peter Gololobov, Sergei Starodubtsev, and Anton Zverev. "Peculiarities of sporadic variations in density and anisotropy of galactic cosmic rays in solar cycle 24." Solar-Terrestrial Physics 8, no. 1 (March 25, 2022): 34–38. http://dx.doi.org/10.12737/stp-81202204.

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In this work, we have processed data from the global network of neutron monitors and muon telescopes by the global survey method to study variations in the density and anisotropy of galactic cosmic rays during Forbush decreases observed in solar cycle 24. The simultaneous use of two different type detectors made it possible to examine the temporal dynamics of the angular distribution of cosmic rays in two different energy intervals. Besides, we have used measurements of the Yakutsk cosmic ray spectrograph after A.I. Kuzmin to assess the energy spectrum index during large disturbances of the interplanetary medium in this cycle. Analysis of the results obtained confirms our early statements that solar activity cycle 24 features an increased level of turbulence in the interplanetary magnetic field.

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Desiati, Paolo. "ICECUBE OBSERVATORY: NEUTRINOS AND THE ORIGIN OF COSMIC RAYS." Acta Polytechnica 53, A (December 18, 2013): 770–75. http://dx.doi.org/10.14311/ap.2013.53.0770.

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The completed IceCube Observatory, the first km<sup>3</sup> neutrino telescope, is already providing the most stringent limits on the flux of high energy cosmic neutrinos from point-like and diffuse galactic and extra-galactic sources. The non-detection of extra-terrestrial neutrinos has important consequences on the origin of the cosmic rays. Here the current status of astrophysical neutrino searches, and of the observation of a persistent cosmic ray anisotropy above 100TeV, are reviewed.

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Góra, Dariusz. "The Pierre Auger Observatory: Review of Latest Results and Perspectives." Universe 4, no. 11 (November 17, 2018): 128. http://dx.doi.org/10.3390/universe4110128.

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The Pierre Auger Observatory is the world’s largest operating detection system for the observation of ultra high energy cosmic rays (UHECRs), with energies above 10 17 eV. The detector allows detailed measurements of the energy spectrum, mass composition and arrival directions of primary cosmic rays in the energy range above 10 17 eV. The data collected at the Auger Observatory over the last decade show the suppression of the cosmic ray flux at energies above 4 × 10 19 eV. However, it is still unclear if this suppression is caused by the energy limitation of their sources or by the Greisen–Zatsepin–Kuzmin (GZK) cut-off. In such a case, UHECRs would interact with the microwave background (CMB), so that particles traveling long intergalactic distances could not have energies greater than 5 × 10 19 eV. The other puzzle is the origin of UHECRs. Some clues can be drawn from studying the distribution of their arrival directions. The recently observed dipole anisotropy has an orientation that indicates an extragalactic origin of UHECRs. The Auger surface detector array is also sensitive to showers due to ultra high energy neutrinos of all flavors and photons, and recent neutrino and photon limits provided by the Auger Observatory can constrain models of the cosmogenic neutrino production and exotic scenarios of the UHECRs origin, such as the decays of super heavy, non-standard-model particles. In this paper, the recent results on measurements of the energy spectrum, mass composition and arrival directions of cosmic rays, as well as future prospects are presented.

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Belov, A., E. Eroshenko, H. Mavromichalaki, C. Plainaki, and V. Yanke. "Solar cosmic rays during the extremely high ground level enhancement on 23 February 1956." Annales Geophysicae 23, no. 6 (September 15, 2005): 2281–91. http://dx.doi.org/10.5194/angeo-23-2281-2005.

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Abstract. The 23 February 1956 ground level enhancement of the solar cosmic ray intensity (GLE05) is the most famous among the proton events observed since 1942. But we do not have a great deal of information on this event due to the absence of solar wind and interplanetary magnetic field measurements at that time. Furthermore, there were no X-Ray or gamma observations and the information on the associated flare is limited. Cosmic ray data was obtained exclusively by ground level detectors of small size and in some cases of a non-standard design. In the present work all available data from neutron monitors operating in 1956 were analyzed, in order to develop a model of the solar cosmic ray behavior during the event. The time-dependent characteristics of the cosmic ray energy spectrum, cosmic ray anisotropy, and differential and integral fluxes have been evaluated utilizing different isotropic and anisotropic models. It is shown that the most outstanding features of this proton enhancement were a narrow and extremely intense beam of ultra-relativistic particles arriving at Earth just after the onset and the unusually high maximum solar particle energy. However, the contribution of this beam to the overall solar particle density and fluency was not significant because of its very short duration and small width. Our estimate of the integral flux for particles with energies over 100 MeV places this event above all subsequent. Perhaps the number of accelerated low energy particles was closer to a record value, but these particles passed mainly to the west of Earth. Many features of this GLE are apparently explained by the peculiarity of the particle interplanetary propagation from a remote (near the limb) source. The quality of the available neutron monitor data does not allow us to be certain of some details; these may be cleared up by the incorporation into the analysis of data from muonic telescopes and ionization chambers operating at that time. Keywords. Interplanatary physics (Cosmic rays; Energetic particles) – Solar physics, astrophysics and astronomy (Flares and mass injections)

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Nikoukar, Romina, Matthew E. Hill, Lawrence Brown, Jozsef Kota, Robert B. Decker, Konstantinos Dialynas, Douglas C. Hamilton, et al. "On the Energy Dependence of Galactic Cosmic Ray Anisotropies in the Very Local Interstellar Medium." Astrophysical Journal 934, no. 1 (July 1, 2022): 41. http://dx.doi.org/10.3847/1538-4357/ac6fe5.

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Abstract We report on the energy dependence of Galactic cosmic rays (GCRs) in the very local interstellar medium (VLISM) as measured by the Low Energy Charged Particle (LECP) instrument on the Voyager 1 spacecraft. The LECP instrument includes a dual-ended solid-state detector particle telescope mechanically scanning through 360° across eight equally spaced angular sectors. As reported previously, LECP measurements showed a dramatic increase in GCR intensities for all sectors of the ≥211 MeV count rate (CH31) at the Voyager 1 heliopause (HP) crossing in 2012; however, since then the count rate data have demonstrated systematic episodes of intensity decrease for particles around 90° pitch angle. To shed light on the energy dependence of these GCR anisotropies over a wide range of energies, we use Voyager 1 LECP count rate and pulse height analyzer (PHA) data from ≥211 MeV channel together with lower-energy LECP channels. Our analysis shows that, while GCR anisotropies are present over a wide range of energies, there is a decreasing trend in the amplitude of second-order anisotropy with increasing energy during anisotropy episodes. A stronger pitch angle scattering at higher velocities is argued as a potential cause for this energy dependence. A possible cause for this velocity dependence arising from weak rigidity dependence of the scattering mean free path and resulting velocity-dominated scattering rate is discussed. This interpretation is consistent with a recently reported lack of corresponding GCR electron anisotropies.

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Buatthaisong, Nutthawara, David Ruffolo, Alejandro Sáiz, Chanoknan Banglieng, Warit Mitthumsiri, Tanin Nutaro, and Waraporn Nuntiyakul. "Extended Cosmic Ray Decreases with Strong Anisotropy after Passage of Interplanetary Shocks." Astrophysical Journal 939, no. 2 (November 1, 2022): 99. http://dx.doi.org/10.3847/1538-4357/ac96ea.

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Abstract The passage of an interplanetary shock and/or interplanetary coronal mass ejection often causes a rapid decrease in the Galactic cosmic-ray (GCR) flux, known as a Forbush decrease, followed by a recovery of the flux over some days. These local effects are of short duration and strongly rigidity dependent, with higher-rigidity particles exhibiting much weaker effects. In contrast, we present data for two events in which the cosmic-ray flux gradually decreased for about 1 week after shock passage, then recovering over the following week, with the highest anisotropy levels observed throughout Solar Cycle 24. These extended decreases have a weak rigidity dependence and are much more prominent in observations at higher cutoff rigidity, where the initial Forbush decrease is not clearly detected and other variations are generally weak, as we demonstrate using data from the Princess Sirindhorn Neutron Monitor at Doi Inthanon, Thailand with a cutoff rigidity of about 17 GV. We propose that these extended decrease events were initiated upon the passage of an interplanetary shock that inhibited the inflow of GCRs along the interplanetary magnetic field, possibly due to magnetic mirroring at the shock. We also discuss the general behavior of GCR anisotropy as observed at this high cutoff rigidity.

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Qiao, Bing-Qiang, Qing Luo, Qiang Yuan, and Yi-Qing Guo. "Understanding the Phase Reversals of Galactic Cosmic-Ray Anisotropies." Astrophysical Journal 942, no. 1 (December 29, 2022): 13. http://dx.doi.org/10.3847/1538-4357/aca7fc.

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Abstract Energy spectra and anisotropies are very important probes of the origin of cosmic rays. Recent measurements show that complicated but very interesting structures exist at similar energies in both the spectra and energy-dependent anisotropies, indicating a common origin of these structures. A particularly interesting phenomenon is that there is a reversal of the phase of the dipole anisotropies, which challenges theoretical modeling. In this work, for the first time, we identify that there might be an additional phase reversal at ∼100 GeV energies of the dipole anisotropies as indicated by a few underground muon detectors and the first direct measurement by the Fermi satellite, coincident with the hundreds of GV hardening of the spectra. We propose that these two phase reversals, together with the energy evolution of the amplitudes and spectra, can be naturally explained with a nearby source overlapping onto the diffuse background. As a consequence, the spectra and anisotropies can be understood as the scalar and vector components of this model, and the two reversals of the phases characterize just the competition of the cosmic-ray streamings between the nearby source and the background. The alignment of the cosmic-ray streamings along the local large-scale magnetic field may play an important but subdominant role in regulating the cosmic-ray propagation. More precise measurements of the anisotropy evolution at both low energies by space detectors and high energies by air shower experiments for individual species will be essential to further test this scenario.

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de la Fuente, Eduardo, Juan Carlos Díaz–Vélez, Paolo Desiati, Jose Luis García–Luna, Janet Torrealba, and Ricardo Gúzman–Alcála. "Information Technologies on High-Energy Astrophysics: Cosmic Ray Anisotropy using HAWC Observatory." EPJ Web of Conferences 208 (2019): 03005. http://dx.doi.org/10.1051/epjconf/201920803005.

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The detection of astroparticles, specially at high energies (>100 GeV), requires special techniques and instruments (telescopes or observatories), for example, those that use the Water Cherenkov radiation technique. In this paper we show an example of how Information Technologies can be used to perform maps and produce high impact results. The latter case is illustrated in the summary of the generation of a high statistics map of cosmic rays at 10 TeV in the northern sky with data collected by the High Altitude Water Cherenkov (HAWC) observatory.

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Grigoryev, Vladislav, Sardaana Gerasimova, Peter Gololobov, Sergei Starodubtsev, and Anton Zverev. "Peculiarities of sporadic variations in density and anisotropy of galactic cosmic rays in solar cycle 24." Solnechno-Zemnaya Fizika 8, no. 1 (March 25, 2022): 34–38. http://dx.doi.org/10.12737/szf-81202204.

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In this work, we have processed data from the global network of neutron monitors and muon telescopes by the global survey method to study variations in the density and anisotropy of galactic cosmic rays during Forbush decreases observed in solar cycle 24. The simultaneous use of two different type detectors made it possible to examine the temporal dynamics of the angular distribution of cosmic rays in two different energy intervals. Besides, we have used measurements of the Yakutsk cosmic ray spectrograph after A.I. Kuzmin to assess the energy spectrum index during large disturbances of the interplanetary medium in this cycle. Analysis of the results obtained confirms our early statements that solar activity cycle 24 features an increased level of turbulence in the interplanetary magnetic field.

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CHILINGARIAN, A., V. BABAYAN, N. BOSTANJYAN, and G. KARAPETYAN. "CORRELATED MEASUREMENTS OF THE SECONDARY COSMIC RAY FLUXES BY THE NEUTRON MONITORS AND MUON TELESCOPES." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6642–45. http://dx.doi.org/10.1142/s0217751x0502968x.

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Radiation and Geomagnetic storms, which are elements of Space Weather, are part of the major obstacles for Space Operations. Reliable forecasting of the arrival of these dangerous elements is of vital importance for the orbiting flights and electric power distribution in near polar regions. In addition to the fleet of space-born instruments, worldwide networks of particle detectors spread along different latitudes and longitudes, provide valuable information on the intensity and anisotropy of the variable cosmic ray fluxes. Aragats Space-Environmental Center provides monitoring of the different species of secondary cosmic rays at two altitudes and with different energy thresholds. 1-minute data is available on-line from URL 〈〉. We demonstrated the sensitivity of the different species of secondary cosmic ray flux to geophysical conditions, taking as examples extremely violent events of end of October – November 2003. Also we introduce the correlation analysis of the different components of registered time-series as a new tool for the classification of the geoeffective events.

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Aartsen, M. G., K. Abraham, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, et al. "ANISOTROPY IN COSMIC-RAY ARRIVAL DIRECTIONS IN THE SOUTHERN HEMISPHERE BASED ON SIX YEARS OF DATA FROM THE ICECUBE DETECTOR." Astrophysical Journal 826, no. 2 (August 2, 2016): 220. http://dx.doi.org/10.3847/0004-637x/826/2/220.

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Amelchakov, M. B., V. S. Vorobyev, Z. T. Izhbulyakova, A. A. Kovylyaeva, and S. S. Khokhlov. "Investigation of Ultrahigh-Energy Cosmic-Ray Anisotropy Using the Data on Muon Bundles Recorded with the DECOR Coordinate-Tracking Detector." Physics of Atomic Nuclei 81, no. 9 (December 2018): 1362–69. http://dx.doi.org/10.1134/s1063778818090016.

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Munakata, K., Y. Mizoguchi, C. Kato, S. Yasue, S. Mori, M. Takita, and J. Kóta. "SOLAR CYCLE DEPENDENCE OF THE DIURNAL ANISOTROPY OF 0.6 TeV COSMIC-RAY INTENSITY OBSERVED WITH THE MATSUSHIRO UNDERGROUND MUON DETECTOR." Astrophysical Journal 712, no. 2 (March 10, 2010): 1100–1106. http://dx.doi.org/10.1088/0004-637x/712/2/1100.

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Takeishi, R. "Study of muons from ultrahigh energy cosmic ray air showers measured with the Telescope Array experiment." EPJ Web of Conferences 210 (2019): 02012. http://dx.doi.org/10.1051/epjconf/201921002012.

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One of the uncertainties in ultrahigh energy cosmic ray (UHECR) observation derives from the hadronic interaction model used for air shower Monte-Carlo (MC) simulations. One may test the hadronic interaction models by comparing the measured number of muons observed at the ground from UHECR induced air showers with the MC prediction. The Telescope Array (TA) is the largest experiment in the northern hemisphere observing UHECR in Utah, USA. It aims to reveal the origin of UHECRs by studying the energy spectrum, mass composition and anisotropy of cosmic rays by utilizing an array of surface detectors (SDs) and fluorescence detectors. We studied muon densities in the UHE extensive air showers by analyzing the signal of TA SD stations for highly inclined showers. On condition that the muons contribute about 65% of the total signal, the number of particles from air showers is typically 1.88 ± 0.08 (stat.) ± 0.42 (syst.) times larger than the MC prediction with the QGSJET II-03 model for proton-induced showers. The same feature was also obtained for other hadronic interaction models, such as QGSJET II-04.

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PAOLIS, F. DE, G. INGROSSO, PH JETZER, and M. RONCADELLI. "BARYONIC DARK CLUSTERS IN GALACTIC HALOS." International Journal of Modern Physics D 05, no. 02 (April 1996): 151–77. http://dx.doi.org/10.1142/s0218271896000114.

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Besides MACHOs (Massive Astrophysical Compact Halo Objects) discovered by microlensing, cold molecular clouds (mainly of H 2) may well contribute substantially to the galactic halo dark matter. We describe a model for the formation and evolution of proto globular clusters towards either globular clusters or dark clusters of MACHOs and molecular clouds, depending on the distance from the galactic centre. Moreover, we discuss various methods to test this scenario, which rely upon observations in several bands of the electromagnetic spectrum. In particular, we estimate the γ-ray flux arising from halo molecular clouds through the interaction with high-energy cosmic-ray protons. Molecular clouds can also be detected via the absorption lines they would produce in the spectrum of stars located in the Large Magellanic Cloud and via the anisotropy they would introduce in the Cosmic Background Radiation when looking at the halo of M31 galaxy. Finally, we address the possibility of discovering MACHOs by infrared searches.

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Krivonos, Roman, Daniel Wik, Brian Grefenstette, Kristin Madsen, Kerstin Perez, Steven Rossland, Sergey Sazonov, and Andreas Zoglauer. "NuSTAR measurement of the cosmic X-ray background in the 3–20 keV energy band." Monthly Notices of the Royal Astronomical Society 502, no. 3 (February 4, 2021): 3966–75. http://dx.doi.org/10.1093/mnras/stab209.

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ABSTRACT We present measurements of the intensity of the cosmic X-ray background (CXB) with the Nuclear Spectroscopic Telescope Array (NuSTAR) telescope in the 3–20 keV energy range. Our method uses spatial modulation of the CXB signal on the NuSTAR detectors through the telescope’s side aperture. Based on the NuSTAR observations of selected extragalactic fields with a total exposure of 7 Ms, we have estimated the CXB 3–20 keV flux to be 2.8 × 10−11 erg s−1 cm−2 deg−2, which is $\sim \! 8{{\ \rm per\ cent}}$ higher than that measured with HEAO-1 and consistent with the INTEGRAL measurement. The inferred CXB spectral shape in the 3–20 keV energy band is consistent with the canonical model of Gruber et al. We demonstrate that the spatially modulated CXB signal measured by NuSTAR is not contaminated by systematic noise and is limited by photon statistics. The measured relative scatter of the CXB intensity between different sky directions is compatible with cosmic variance, which opens new possibilities for studying CXB anisotropy over the whole sky with NuSTAR.

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Biteau, J., T. Bister, L. Caccianiga, O. Deligny, A. di Matteo, T. Fujii, D. Harari, et al. "Covering the celestial sphere at ultra-high energies: Full-sky cosmic-ray maps beyond the ankle and the flux suppression." EPJ Web of Conferences 210 (2019): 01005. http://dx.doi.org/10.1051/epjconf/201921001005.

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Despite deflections by Galactic and extragalactic magnetic fields, the distribution of ultra-high energy cosmic rays (UHECRs) over the celestial sphere remains a most promising observable for the identification of their sources. Thanks to a large number of detected events over the past years, a large-scale anisotropy at energies above 8 EeV has been identified, and there are also indications from the Telescope Array and Pierre Auger Collaborations of deviations from isotropy at intermediate angular scales (about 20 degrees) at the highest energies. In this contribution, we map the flux of UHECRs over the full sky at energies beyond each of two major features in the UHECR spectrum – the ankle and the flux suppression -, and we derive limits for anisotropy on different angular scales in the two energy regimes. In particular, full-sky coverage enables constraints on low-order multipole moments without assumptions about the strength of higher-order multipoles. Following previous efforts from the two Collaborations, we build full-sky maps accounting for the relative exposure of the arrays and differences in the energy normalizations. The procedure relies on cross-calibrating the UHECR fluxes reconstructed in the declination band around the celestial equator covered by both observatories. We present full-sky maps at energies above ~ 10 EeV and ~ 50 EeV, using the largest datasets shared across UHECR collaborations to date. We report on anisotropy searches exploiting full-sky coverage and discuss possible constraints on the distribution of UHECR sources.

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van Vliet, Arjen, Andrea Palladino, Andrew Taylor, and Walter Winter. "Extragalactic magnetic field constraints from ultrahigh-energy cosmic rays from local galaxies." Monthly Notices of the Royal Astronomical Society 510, no. 1 (December 3, 2021): 1289–97. http://dx.doi.org/10.1093/mnras/stab3495.

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ABSTRACT We interpret the correlation between local star-forming galaxy positions and ultrahigh-energy cosmic-ray (UHECR) directions, recently detected by the Pierre Auger Observatory (PAO), in terms of physical parameters: the local density of sources and the magnetic fields governing the UHECR propagation. We include a Galactic magnetic field model on top of a random extragalactic magnetic field description to determine the level of UHECR deflections expected from an ensemble of source positions. Besides deflections in magnetic fields, we also take into account energy losses with background photon fields as well as spectrum and composition measurements by the PAO. We find consistency between the PAO anisotropy measurement and the local star-forming galaxy density for large extragalactic magnetic field strengths with $B \gt 0.2 \ \rm nG$ (for a coherence length of $1 \ \rm Mpc$) at the 5σ confidence level. Larger source densities lead to more isotropic background and consequently allow for weaker extragalactic magnetic fields. However, the acceleration of UHECR by such abundant sources is more challenging to motivate. Too large source densities and extragalactic magnetic field strengths, on the other hand, are also disfavoured as that decreases the expected level of anisotropy. This leads to upper limits of $B \lt 22 \ \rm nG$ and $\rho _0 \lt 8.4 \times 10^{-2} \ \rm Mpc^{-3}$ at the 90 per cent confidence level.

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Migkas, K., G. Schellenberger, T. H. Reiprich, F. Pacaud, M. E. Ramos-Ceja, and L. Lovisari. "Probing cosmic isotropy with a new X-ray galaxy cluster sample through the LX–T scaling relation." Astronomy & Astrophysics 636 (April 2020): A15. http://dx.doi.org/10.1051/0004-6361/201936602.

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The isotropy of the late Universe and consequently of the X-ray galaxy cluster scaling relations is an assumption greatly used in astronomy. However, within the last decade, many studies have reported deviations from isotropy when using various cosmological probes; a definitive conclusion has yet to be made. New, effective and independent methods to robustly test the cosmic isotropy are of crucial importance. In this work, we use such a method. Specifically, we investigate the directional behavior of the X-ray luminosity-temperature (LX–T) relation of galaxy clusters. A tight correlation is known to exist between the luminosity and temperature of the X-ray-emitting intracluster medium of galaxy clusters. While the measured luminosity depends on the underlying cosmology through the luminosity distance DL, the temperature can be determined without any cosmological assumptions. By exploiting this property and the homogeneous sky coverage of X-ray galaxy cluster samples, one can effectively test the isotropy of cosmological parameters over the full extragalactic sky, which is perfectly mirrored in the behavior of the normalization A of the LX–T relation. To do so, we used 313 homogeneously selected X-ray galaxy clusters from the Meta-Catalogue of X-ray detected Clusters of galaxies. We thoroughly performed additional cleaning in the measured parameters and obtain core-excised temperature measurements for all of the 313 clusters. The behavior of the LX–T relation heavily depends on the direction of the sky, which is consistent with previous studies. Strong anisotropies are detected at a ≳4σ confidence level toward the Galactic coordinates (l, b) ∼ (280°, − 20°), which is roughly consistent with the results of other probes, such as Supernovae Ia. Several effects that could potentially explain these strong anisotropies were examined. Such effects are, for example, the X-ray absorption treatment, the effect of galaxy groups and low redshift clusters, core metallicities, and apparent correlations with other cluster properties, but none is able to explain the obtained results. Analyzing 105 bootstrap realizations confirms the large statistical significance of the anisotropic behavior of this sky region. Interestingly, the two cluster samples previously used in the literature for this test appear to have a similar behavior throughout the sky, while being fully independent of each other and of our sample. Combining all three samples results in 842 different galaxy clusters with luminosity and temperature measurements. Performing a joint analysis, the final anisotropy is further intensified (∼5σ), toward (l, b) ∼ (303°, − 27°), which is in very good agreement with other cosmological probes. The maximum variation of DL seems to be ∼16 ± 3% for different regions in the sky. This result demonstrates that X-ray studies that assume perfect isotropy in the properties of galaxy clusters and their scaling relations can produce strongly biased results whether the underlying reason is cosmological or related to X-rays. The identification of the exact nature of these anisotropies is therefore crucial for any statistical cluster physics or cosmology study.

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Popa, Lucia Aurelia. "Dark Matter Sterile Neutrino from Scalar Decays." Universe 7, no. 8 (August 21, 2021): 309. http://dx.doi.org/10.3390/universe7080309.

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We place constraints on DM sterile neutrino scalar decay production (SDP) assuming that sterile neutrinos representa fraction from the total Cold Dark Matter energy density. For the cosmological analysis we complement the CMB anisotropy measurements with CMB lensing gravitational potential measurements, that are sensitive to the DM distribution to high redshifts and with the cosmic shear data that constrain the gravitational potential at lower redshifts than CMB. We also use the most recent low-redshift BAO measurements that are insensitive to the non-linear effects, providing robust geometrical tests. We show that our datasets have enough sensitivity to constrain the sterile neutrino mass mνs and the mass fraction fS inside the co-moving free-streaming horizon. We find that the best fit value mνs=7.88±0.73 keV (68% CL) is in the parameter space of interest for DM sterile neutrino decay interpretation of the 3.5 keV X-ray line and that fS=0.86±0.07 (68% CL) is in agreement with the upper limit constraint on fS from the X-ray non-detection and Ly-α forest measurements that rejects fS=1 at 3σ. However, we expect that the future BAO and weak lensing surveys, such as EUCLID, will provide much more robust constraints.

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ZIRAKASHVILI, VLADIMIR N. "COSMIC RAY ANISOTROPY PROBLEM." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6858–60. http://dx.doi.org/10.1142/s0217751x05030314.

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The anisotropy of cosmic rays, produced by Galactic supernovae is calculated. It is a factor 100 ÷ 1000 larger than the observed value at 1 PeV. It is shown that this contradiction can be explained if a cosmic ray diffusion coefficient is small in the local vicinity of the Sun.

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Zhang, Yiran, Siming Liu, and Dejin Wu. "Cosmic-Ray Convection–Diffusion Anisotropy." Astrophysical Journal 938, no. 2 (October 1, 2022): 106. http://dx.doi.org/10.3847/1538-4357/ac8f28.

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Abstract Under nonuniform convection, the distribution of diffusive particles can exhibit dipole and quadrupole anisotropy induced by the fluid inertial and shear force, respectively. These convection-related anisotropies, unlike the Compton–Getting effect, typically increase with the cosmic-ray (CR) energy, and are thus candidate contributors for the CR anisotropy. In consideration of the inertial effect, CR observational data can be used to set an upper limit on the average acceleration of the local interstellar medium in the equatorial plane to be on the order of 100 μm s−2. Using Oort constants, the quadrupole anisotropy above 200 TeV may be modeled with the shear effect arising from the Galactic differential rotation.

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37

Erlykin, A. D., S. K. Machavariani, and A. U. Wolfendale. "Enigmas of Cosmic Ray Anisotropy." Bulletin of the Russian Academy of Sciences: Physics 83, no. 8 (August 2019): 1035–37. http://dx.doi.org/10.3103/s1062873819080148.

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Peregudov, Dmitriy, Anatoly Soloviev, Igor Yashin, and Victor Shutenko. "GALACTIC COSMIC RAY ANISOTROPY MODELLING." Solar-Terrestrial Physics 6, no. 1 (April 1, 2020): 29–34. http://dx.doi.org/10.12737/stp-61202003.

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We calculate the angular distribution of cosmic rays at a given point of the heliosphere under the assumption that the incoming flux from outer space is isotropic. The static magnetic field is shown to cause no anisotropy provided that the observation point is situated out of the trapped particle area. We consider a coronal ejection model in the form of a static cylinder with an axial homogeneous magnetic field inside. We calculate angular distribution samples in the trapped particle area (inside the cylinder) and show that there is a certain cone of directions with a reduced flux. For the same model with the moving cylinder, the angular distribution samples are calculated for different positions of the observation point outside the cylinder. Anisotropy of order of the ejection to light velocity ratio is shown to arise. The calculated samples are in qualitative agreement with URAGAN muon hodoscope data.

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39

Peregudov, Dmitriy, Anatoly Soloviev, Igor Yashin, and Victor Shutenko. "GALACTIC COSMIC RAY ANISOTROPY MODELLING." Solnechno-Zemnaya Fizika 6, no. 1 (March 30, 2020): 36–42. http://dx.doi.org/10.12737/szf-61202003.

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We calculate the angular distribution of cosmic rays at a given point of the heliosphere under the assumption that the incoming flux from outer space is isotropic. The static magnetic field is shown to cause no anisotropy provided that the observation point is situated out of the trapped particle area. We consider a coronal ejection model in the form of a static cylinder with an axial homogeneous magnetic field inside. We calculate angular distribution samples in the trapped particle area (inside the cylinder) and show that there is a certain cone of directions with a reduced flux. For the same model with the moving cylinder, the angular distribution samples are calculated for different positions of the observation point outside the cylinder. Anisotropy of order of the ejection to light velocity ratio is shown to arise. The calculated samples are in qualitative agreement with URAGAN muon hodoscope data.

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40

Feder, Toni. "LANL Rescues Cosmic-Ray Detector." Physics Today 55, no. 7 (July 2002): 26–27. http://dx.doi.org/10.1063/1.1506745.

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Konobeevski, E. S., M. V. Mordovskoy, and V. M. Skorkin. "The cosmic gamma-ray detector." Astronomical & Astrophysical Transactions 22, no. 6 (December 2003): 875–78. http://dx.doi.org/10.1080/1055679031000153888.

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42

Tapadar, Ananya, Sougata Ganguly, and Sourov Roy. "Non-adiabatic evolution of dark sector in the presence of U(1)_{L_μ} – _{L_τ} gauge symmetry." Journal of Cosmology and Astroparticle Physics 2022, no. 05 (May 1, 2022): 019. http://dx.doi.org/10.1088/1475-7516/2022/05/019.

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Abstract In secluded dark sector scenario, the connection between the visible and the dark sector can be established through a portal coupling and its presence opens up the possibility of non-adiabatic evolution of the dark sector. To study the non-adiabatic evolution of the dark sector, we have considered a U(1) Lμ – Lτ ⊗ U(1) X extension of the standard model (SM). Here the dark sector is charged only under U(1) X gauge symmetry whereas the SM fields are singlet under this symmetry. Due to the presence of tree-level kinetic mixing between U(1) X and U(1) Lμ – Lτ gauge bosons, the dark sector evolves non-adiabatically and thermal equilibrium between the visible and dark sector is governed by the portal coupling. Depending on the values of the portal coupling (ϵ), dark sector gauge coupling (gX ), mass of the dark matter (m χ) and mass of the dark vector boson (m Z'), we study the temperature evolution of the dark sector as well as the various non-equilibrium stages of the dark sector in detail. Furthermore we have also investigated the constraints on the model parameters from various laboratory and astrophysical searches. We have found that the parameter space for the non-adiabatic evolution of dark sector is significantly constrained for m Z' ≲ 100 MeV from the observations of beam dump experiments, stellar cooling etc. The relic density satisfied region of our parameter space is consistent with the bounds from direct detection, and self interaction of dark matter (SIDM) for the mass ratio r ≡ m Z'/m χ = 10-3 and these bounds will be more relaxed for larger values of r. However the constraints from measurement of diffuse γ-ray background flux and cosmic microwave background (CMB) anisotropy are strongest for r = 10-1 and for smaller values of r, they are not significant.

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Mishra, Rajesh K., and Rekha Agarwal Mishra. "Cosmic ray anisotropy and solar activity." Brazilian Journal of Physics 37, no. 4 (December 2007): 1227–31. http://dx.doi.org/10.1590/s0103-97332007000800006.

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Krymsky, G. F., P. A. Krivoshapkin, S. K. Gerasimova, V. G. Grigoryev, and V. P. Mamrukova. "Heliolatitudinal dependence of cosmic-ray anisotropy." Astronomy Letters 32, no. 8 (August 2006): 574–76. http://dx.doi.org/10.1134/s1063773706080093.

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Pohl, Martin, and David Eichler. "UNDERSTANDING TeV-BAND COSMIC-RAY ANISOTROPY." Astrophysical Journal 766, no. 1 (February 28, 2013): 4. http://dx.doi.org/10.1088/0004-637x/766/1/4.

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Erlykin, A. D., S. K. Machavarian, and A. W. Wolfendale. "Puzzles of the Cosmic Ray Anisotropy." Journal of Physics: Conference Series 1181 (February 2019): 012037. http://dx.doi.org/10.1088/1742-6596/1181/1/012037.

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Mishra, Rajesh K., and Rekha Agarwal Mishra. "Interplanetary Transients and Cosmic-Ray Anisotropy." Solar Physics 240, no. 2 (February 2007): 359–72. http://dx.doi.org/10.1007/s11207-006-0242-y.

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Clay, RW. "Cosmic Ray Anisotropy above 1015 eV." Australian Journal of Physics 40, no. 3 (1987): 423. http://dx.doi.org/10.1071/ph870423.

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An examination is made of published data on cosmic ray anisotropy at energies above about 1015 eV. Both amplitude and phase results are examined in an attempt to assess the confidence which can be placed in the observations as a whole. It is found that whilst many published results individually may suggest quite high confidence levels of real measured anisotropy, the data taken as a whole are less convincing. Some internal consistency in the phase results suggests that a real effect may have been measured but, again, this is not at a high confidence level.

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Bird, DJ, RW Clay, and PG Edwards. "Cosmic Ray Anisotropy below 1015 eV." Australian Journal of Physics 42, no. 4 (1989): 465. http://dx.doi.org/10.1071/ph890465.

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Measurements have been made of the cosmic ray anisotropy at 35�S with a sea-level unshielded air shower array sensitive primarily to the proton component of the cosmic ray beam with energies between 1014 and 3x101S eV. The first harmonic of the anisotropy was found to have an amplitude of O� 34(�0 �09)% at a phase of 318(�18)o.

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Erlykin, A. D., S. K. Machavariani, and A. W. Wolfendale. "Puzzles of the cosmic ray anisotropy." Advances in Space Research 63, no. 1 (January 2019): 794–99. http://dx.doi.org/10.1016/j.asr.2018.09.042.

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Journal articles on the topic 'Cosmic ray; detector; anisotropy'

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