Performance and simulation of the surface detector array of the TAx4 experiment
Kozo FujisueRasha AbbasiT. Abu‐ZayyadM. AllenYasuhiko AraiRyuhei ArimuraE. BarcikowskiJohn BelzD. R. BergmanS. A. BlakeIsaac BucklandR. CadyByongGu CheonJ. ChibaM. ChikawaToshihiro FujiiKozo FujisueKaoru FujitaRyota FujiwaraM. FukushimaRyota FukushimaG. FurlichR. GonzàlezW. HanlonMasashi HayashiN. HayashidaKenichi HibinoR. HiguchiK. HondaD. IkedaTaichi InadomiNaoki InoueT. IshiiHaruhiko ItoDmitry Yu. IvanovHirokazu IwakuraAkihito IwasakiHun JeongShinkyu JeongCharlie JuiK. KadotaF. KakimotoO. KalashevK. KasaharaSaori KasamiHiroshi KawaiSatoshi KawakamiS. KawanaK. KawataIvan KharukE. KidoH.B. KimJ. H. KimMichael KimSun-Woo KimYasuhisa KimuraS. KishigamiY. KubotaShinnosuke KurisuVladim KuzminM. KuznetsovY.J. KwonK.H. LeeБ. ЛубсандоржиевJon Paul LundquistKeisuke MachidaHiroyuki MatsumiyaT. MatsuyamaJ. N. MatthewsR. MaytaM. MinaminoK. MukaiI. MyersS. NagatakiK. NakaiRyosuke NakamuraT. NakamuraY. NakamuraArata NakazawaEiji NishioT. NonakaHiroyuki OdaS. OgioM. OhnishiH. OhokaYuya OkuTaichi OkudaY. OmuraM. OnoR. OnogiA OshimaSatoru OzawaI.H. ParkM. PottsМ. С. ПширковJackson RemingtonD. C. RodriguezГ. РубцовDongok RyuH. SagawaRyosuke SaharaYoshinori SaitoН. СакакиT. SakoN. SakuraiK. SanoKotaro SatoTeppei SEKIK. SekinoP. D. ShahYuma ShibasakiF. ShibataN. ShibataToshiharu ShibataHidetoshi ShimodairaB. K. ShinH.S. ShinDaiki ShintoJennifer SmithP. SokolskyNaohiro SoneB. T. StokesT. A. StromanY. TakagiYoshio TakahashiM. TakamuraMasatoshi TakedaRyuji TakeishiA. TaketaM. TakitaY. TamedaHiroki TanakaK. TanakaM. TanakaYuta TanoueS. B. ThomasG. B. ThomsonP. TinyakovИ.В. ТкачевH. TokunoT. TomidaS. TroitskyRyosuke TsudaY. TsunesadaY. UchihoriS. UdoTakafumi UehamaTiffany WongKohei YadaM. YamamotoK. YamazakiJae-Yong YangK. YashiroFugo YoshidaY. YoshiokaY. ZhezherZ. ZundelRasha AbbasiT. Abu‐ZayyadMonica AllenYuto AraiRyuhei ArimuraE. BarcikowskiJohn BelzD. R. BergmanSamuel BlakeR. CadyByongGu CheonJyunsei ChibaMichiyuki ChikawaToshihiro FujiiK. FujitaRyota FujiwaraM. FukushimaRyota FukushimaG. FurlichRicardo GonzálezW. HanlonMotoki HayashiN. HayashidaK. HibinoRyo HiguchiKen HondaD. IkedaTaichi InadomiNaoya InoueTakaaki IshiiHirotaka ItoD. IvanovHirokazu IwakuraAoi IwasakiHyoming JeongSoomin JeongCharlie JuiK. KadotaF. KakimotoO. KalashevK. KasaharaSaori KasamiHideyuki KawaiS. KawakamiS. KawanaKatsumasa KawataIvan KharukE. KidoHangBae KimJi‐Hee KimJihyun KimMin Hyo KimSang‐Woo KimYusuke KimuraShoichi KishigamiYuto KubotaShinnosuke KurisuVladim KuzminM. KuznetsovYoungjoon KwonKwang‐Ho LeeBayarJon Paul LubsandorzhievJon Paul LundquistKazuhiro MachidaHiroyuki MatsumiyaToshio MatsuyamaJ. N. MatthewsR. MaytaM. MinaminoKeijiro MukaiI. MyersShigehiro NagatakiKei NakaiRyo NakamuraToru NakamuraTomoyuki NakamuraYuya NakamuraArata NakazawaEiji NishioT. NonakaHiroyuki OdaS. OgioM. OhnishiH. OhokaYuya OkuTakeshi OkudaYugo OmuraM. OnoR. OnogiA. OshimaS. OzawaIl Hung ParkMatt PottsМ. С. ПширковJackson RemingtonDoug RodriguezГ. РубцовDongsu RyuHiroyuki SagawaRyosuke SaharaYasunori SaitoН. СакакиT. SakoN. SakuraiKengo SanoKoki SatoT. SekiKoichi SekinoPriti ShahYuma ShibasakiF. ShibataNorimichi ShibataT. ShibataHideaki ShimodairaBokkyun ShinHeungsu ShinDaiki ShintoJeremy SmithP. SokolskyNaohiro SoneBen StokesTom StromanYoshinori TakagiYuichi TakahashiMai TakamuraMasahiro TakedaRyuji TakeishiA. TaketaMasato TakitaY. TamedaHideki TanakaKoichi TanakaM. TanakaYuta TanoueStanton ThomasGordon ThomsonPetr TinyakovI. TkachevHisono TokunoTaka TomidaS. TroitskyRyosuke TsudaY. TsunesadaYukio UchihoriShigeharu UdoTakafumi UehamaF. UrbanTiffany WongKohei YadaMashu YamamotoK. YamazakiJongmann YangK. YashiroFugo YoshidaTsubasa YoshiokaYana ZhezherZach Zundel
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Abstract:
The TAx4 experiment is a project to observe highest energy cosmic rays by expanding the detectionarea of the Telescope Array (TA) experiment with newly constructed surface detectors (SDs) andfluorescence detectors (FDs). New SDs are arranged in a square grid with 2.08 km spacing atthe north east and south east of the TA SD array. We use CORSIKA simulations and implementthe calibration data of the new SDs to calculate the performance of the new SDs. We comparethe data with the simulation and validate the performance of the SDs. The comparison and theperformance will be shown in the presentation.The AZT-8 70-cm telescope of the Crimean Astrophysical Observatory was upgraded in the early 2000s. Obsolete pieces of equipment of the telescope were replaced and new ones were developed. The creation of a special control program has enabled the telescope to be pointed at objects automatically. As a result, it has become much easier to control the telescope and the efficiency of using the observing time has increased significantly.
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V-detector algorithm is unable to guarantee a large coverage for generated detector.The shortcoming usually results in a large number of detectors in the detector sets and low detection efficiency.An optimized V-detector algorithm was proposed.In the optimized algorithm,a detector was generated on the basis of a randomly chosen uncovered non-self sample,and the detector generation process ensured the detector covered the non-self sample and extended the detector's coverage by determining the detector's center and detection radius reasonably.Meanwhile,hypothesis testing process was used to estimate the coverage of a detector set,and hypothesis testing process was integrated with detector generation process to ensure the generated detector set fully covered the non-self region,and reduced the number of detectors in the detector set.Experimental results indicate that compared with the V-detector algorithm,the optimized algorithm generates a much smaller detector set and increases the detection efficiency.
Sample (material)
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X-ray telescope
X-Ray Astronomy
Active optics
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We study the change in cosmic-ray pressure, the change in cosmic-ray density, and the level of cosmic-ray induced heating via Alfven-wave damping when cosmic rays move from a hot ionized plasma to a cool cloud embedded in that plasma. The general analysis method outlined here can apply to diffuse clouds in either the ionized interstellar medium or in galactic winds. We introduce a general-purpose model of cosmic-ray diffusion building upon the hydrodynamic approximation for cosmic rays (from McKenzie & Voelk and Breitschwerdt and collaborators). Our improved method self-consistently derives the cosmic-ray flux and diffusivity under the assumption that the streaming instability is the dominant mechanism for setting the cosmic-ray flux and diffusion. We find that, as expected, cosmic rays do not couple to gas within cool clouds (cosmic rays exert no forces inside of cool clouds), that the cosmic-ray density does not increase within clouds (it may slightly decrease in general, and decrease by an order of magnitude in some cases), and that cosmic-ray heating (via Alfven-wave damping and not collisional effects as for ~10 MeV cosmic rays) is only important under the conditions of relatively strong (10 micro-Gauss) magnetic fields or high cosmic-ray pressure (~10^{-11} ergs cm^{-3}).
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Spectrum analyzer is one of the radio frequency measuring instruments in common use.Appropriate detector types should be chosen to analyze and measure a variety of signals to show their characteristics correctly,the results would be inaccurate or absolutely wrong when inappropriate detector types are chosen.Various kinds of detector types of spectrum analyzer are introduced,the features and applications of sample detector,max peak detector,min peak detector,auto peak detector,normal detector,average detector,RMS detector and quasi-peak detector are analyzed in detail,the differences among them are concluded.
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In this paper we summarize our modelling efforts for cosmic rays near the heliopause, and discuss whether galactic cosmic ray modulation beyond the heliopause is possible and present an explanation for the anisotropic nature of the observed cosmic ray intensities in the very local interstellar medium. We show that (i) modulation beyond the heliopause is possible, but highly dependent on the assumed parameters (most notable, the perpendicular diffusion coefficient). Treating the heliopause as a tangential discontinuity, significantly damps this modulation effect and leads to modelled results that are similar to Voyager 1 observations. (ii) By choosing an appropriate functional form of the perpendicular diffusion coefficient on the pitch-angle level, we are able to account for the anisotropic behaviour observed for both galactic and anomalous cosmic rays in the local interstellar medium.
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Chemical composition of ultrahigh-energy cosmic rays is estimated through the reliably determined (both experimentally and theoretically) distribution of the number of showers in the galactic latitude. Experimental data at energies of ∼1019 eV agree with the theoretical calculations, provided that cosmic rays involve predominantly heavy nuclei. An enhanced flux of cosmic rays from the galactic plane is detected at energies of ∼1019 eV.
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Abstract Galactic cosmic rays (GCRs) originate from sources outside the solar system and reach the Earth’s environment from all directions. More than 100 years after the first detection of cosmic rays, the origin of high-energy cosmic rays is still a mystery. Although our knowledge of the origin and propagation of cosmic rays is relatively limited, we can study the radiation conditions in the near-Earth space environment in more detail. The origin, composition, and energy spectra of cosmic rays are briefly discussed in this paper. A brief review of the transport of galactic cosmic rays in the heliosphere is given. The geomagnetic effects on galactic cosmic rays and the atmospheric interactions of primary particles are also discussed in the paper.
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The transport and acceleration of galactic cosmic rays is discussed with emphasis on the highest energies. The mechanism of diffusive shock acceleration is shown to produce a near-universal spectrum which can account for most observed cosmic rays. A quasi-perpendicular shock in general accelerates particles faster and to higher energies than a comparable quasi-parallel shock. Application of these ideas to supernova blast waves suggests that they can produce galactic cosmic rays to the knee in the spectrum, some 3 ×10 15 eV. A similar blast wave, recently identified near the galactic center could accelerate particles to an energy of some 10 18 Z eV or higher (hereinafter Z is the charge in units of the elementary charge). It is possible that the highest-energy cosmic rays could come from the galactic center. If this is the case, there should be an enhancement of the flux of high-energy cosmic rays coming from the galactic center.
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