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宇宙射线对地表矿物晶格的损伤及其地质作用的研究 总被引:2,自引:2,他引:0
文章从理论与实验两个方面论证了宇宙射线对地表矿物晶格造成损伤的可能性。并初步计算了宇宙射线对地表矿物晶格造成损伤的大小及其对土壤形成影响的程度。把宇宙射线发挥地质作用的方式与太阳能和地球外天体的万有引力能的地质作用方式作了比较,得出宇宙射线对地表矿物晶格的损伤是地质作用研究中不可忽视的因素的结论 相似文献
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MA Ling-Ling BAI Yun-Xiang CAO Zhen CHEN Ming-Jun CHEN Li-Hong CHEN Song-Zhan CHEN Yao DING Kai-Qi HE nui-Hai LIU Jia LIU Jia-Li LI Xiao-Xiao MA Xin-Hua SHENG Xiang-Dong XIAO Gang ZHA Min ZHANG Shou-Shan ZHANG Yong ZHAO Jing ZHOU Sin 《中国物理C(英文版)》2011,35(5)
The Large High Altitude Air Shower Observatory (LHAASO) project is proposed to study high energy gamma ray astronomy (40 GeV-1 PeV) and cosmic ray physics (20 TeV-1 EeV). The wide field of view Cherenkov telescope array, as a component of the LHAASO project, will be used to study the energy spectrum and composition of cosmic rays by measuring the total Cherenkov light generated by air showers and the shower maximum depth. Two prototype telescopes have been in operation since 2008. The pointing accuracy of each telescope is crucial for the direction reconstruction of the primary particles. On the other hand, the primary energy reconstruction relies on the shape of the Cherenkov image on the camera and the unrecorded photons due to the imperfect connections between the photomultiplier tubes. UV bright stars are used as point-like objects to calibrate the pointing and to study the optical properties of the camera, the spot size and the fractions of unrecorded photons in the insensitive areas of the camera. 相似文献
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宇宙线对地球气候的影响 总被引:4,自引:2,他引:2
对宇宙线影响地球气候的一些观测结果和物理机制的研究进行了总结和概述,主要讨论了宇宙线对大气中化学反应、云形成过程等的影响,并给出了羊八井宇宙线观测站对宇宙线流强和大气参量日变化的初步观测结果. 相似文献
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小型宇宙射线探测仪的模拟和测量 总被引:1,自引:0,他引:1
介绍了一款小型宇宙射线探测仪。该仪器具有宇宙射线科普演示功能,主要用于实时测量μ子射线并显示计数,以及长时间尺度下(年)稳定地对不同角度的次级宇宙线通量进行监控记录。简要地展示了探测器的硬件构造和探测效率的模拟计算。探测仪单个探测器的探测效率为93.1%,两个探测器符合测量的探测效率为86.6%。根据探测器的计数率以及模拟计算的探测效率,估计了次级宇宙射线垂直地面方向的通量,为J=29±3 m-2 sr-1 s-1。另外,利用该宇宙射线探测仪,测量了兰州市区的次级宇宙射线的天顶角分布。其结果很好地满足I(θ)=IH+I0 cosα θ经验公式,其中的角度依赖参数α=2.42±0.52。A small cosmic ray device is introduced in this paper.It has the demonstration function for popularization of science,and can be used mainly to display the μ counts in a real-time measurement,and to monitor the secondary cosmic ray flux at different angles in a very long time scale (years).We briefly show the hardware of the device and the detecting efficiency calculation by simulation.The detecting efficiency for one detector of the device is 93.1%,and the detecting efficiency is 86.6% for the coincidence measurement of two detectors.Based on the count rate by the detector and the simulated efficiency,the secondary cosmic ray flux perpendicular to the ground surface is measured,which is J=29±3 m-2sr-1 s-1.Moreover,with an application of the device,we measured the angular distribution of the secondary cosmic ray rate in Lanzhou City.The resulting angular distribution agrees well with the empirical formula as I(θ)=IH+I0 cosα θ,in which the parameter for the angle-dependence is α=2.42±0.53. 相似文献
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CAO Zhen 《中国物理C(英文版)》2010,34(2):249-252
Gamma ray source detection above 30 TeV is an encouraging approach for finding galactic cosmic ray sources. All sky survey for gamma ray sources using wide field of view detector is essential for population accumulation for various types of sources above 100 GeV. In order to target those goals, a large air shower particle detector array of 1 km~2 (the LHAASO project) at 4300 m a.s.l, is proposed. By adding two MagicII-type telescopes in the array as proposed, LHAASO will be enhanced in source morphologic investigation power. The proposed array will be utilized also for energy spectrum measurement for individual cosmic ray species above 30 TeV. By re-configuring the wide field of view telescopes into fluorescence light detector array, the aperture of the detector array can be enlarged to cover an energy region above 100 PeV where the second knee is located. Cosmic ray spectrum and composition will be measured in order to transfer an energy scale to ultra high energy cosmic ray experiments. 相似文献
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Analysis of Forbush decreases observed using a muon telescope in Antarctica starting on 21 June 2015
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De-Hong Huang Hong-Qiao Hu Ji-Long Zhang Hong Lu Da-Li Zhang Bin-Shen Xue Jing-Tian Lu 《中国物理C(英文版)》2018,42(12):125001-125001
A cosmic-ray muon telescope has been collecting data since the end of 2014, which was shortly after the telescope was built in the Zhongshan Station of Antarctica. The telescope is the first observation device to be built by Chinese scientists in Antarctica. The pressure change is very strong in Zhongshan station. The count rate of the pressure correction results shows that the large variations in the count rate are likely caused by pressure fluctuations. During the period from 18 June to 22 June 2015, four halo coronal mass ejections(CMEs) were ejected from the Sun. These CMEs initiated a series of Forbush decreases(FD) when they reached the Earth. We conducted a comprehensive study of the intensity fluctuations of galactic cosmic rays recorded during FDs. The intensity fluctuations used in this study were collected by cosmic ray detectors of multiple stations(Zhongshan, McMurdo,South Polar, and Nagoya), and the solar wind measurements were collected by ACE and WIND. The profile of the FD of 22 June demonstrated a four-step decrease. The traditional one-or two-step FD classification method does not adequately explain the FD profile results. The interaction between the faster CME that occurred on 21 June 2015 and the two slow CMEs of the earlier few days should be considered. The cosmic ray intensities of the South Pole,McMurdo, and Zhongshan stations have similar hourly variations, whereas the galactic cosmic rays recorded between polar and non-polar locations are distinct. The FD pre-increase of 22 June 2015 for the Nagoya muon telescope(non-polar location) lags those of the McMurdo and Zhongshan stations(polar locations) by 1 h. The FD onset of22 June 2015 for the Nagoya muon telescope lags those of the polar locations by 1 h. 相似文献
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基于小波变换的1—10TeV宇宙线周期变化研究 总被引:3,自引:2,他引:1
利用小波变换, 结合折叠周期分析方法, 对羊八井宇宙线观测站Tibet AS γ阵列1998年4—6月的实验记录数据进行了周期分析, 发现 TeV和10 TeV宇宙线流强观测数据中包含0.5 和1 d周期变化, 其信噪比分别达到10和6. TeV宇宙线0.5 和1 d周期变化的最大变化幅度分别约为0.3%和0.5%, 10 TeV宇宙线约为0.4%和0.7%. We use the technique of wavelet analysis and epoch folding methods to search for the superimposed periodic signals of 1—10 TeV cosmic ray in the data obtained with Tibet Ⅱ/HD AS Array for April to June of 1998. Solar time semi diurnal and diurnal variations have been detected with about signal noise ratio 10 and 6 for the 1 TeV and 10 TeV cosmic ray flux respectively. The semi diurnal variations are of an amplitude 0.3%, a phase 0.9 for 1 TeV cosmic ray and 0.4%, 0.9 for 10 TeV. The diurnal variations are of amplitude 0.5%, 0.7%, and phase 0.8 for 1 TeV and 10 TeV cosmic ray respectively. 相似文献
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宇宙线是来自宇宙空间的高能粒子流,研究宇宙线的起源、加速、传播机制及其所涉及的天体物理和宇宙学过程是宇宙线天体物理研究的重要内容。本文介绍并讨论其中几个涉及物理学一些基本问题的重要课题的研究现状及前景,其中包括极高能宇宙线的观测研究,太阳中微子能谱的实时测量,宇宙线中新粒子的搜寻等。 相似文献
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The observed hardening of the spectra of cosmic ray protons and helium nuclei is studied within the model of nonlinear diffusive shock acceleration of supernova remnants(SNRs). In this model, the injected particles with energies below the spectral "knee" are assumed to be described by two populations with different spectral indexes around 200 GeV. The high-energy population is dominated by the particles with energies above 200 GeV released upstream of the shock of SNR, and the low-energy population is attributed to the particles with energies below 200 GeV released downstream of the shock of SNR. In this scenario, the spectral hardening of cosmic ray protons and helium nuclei observed by PAMELA, AMS-02, and CREAM experiments can be reproduced. 相似文献
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XU Mei-Hang LIU Rong-Guang ZHU Qi-Ming ZHANG Jian HUANG Jie CHEN Chang CHEN Yuan-Bo WU Zhi QIN Zhong-Hua WU Ling-Hui LIU Jian-Bei WANG Lan JIN Yan 《中国物理C(英文版)》2008,32(12)
After examination of the designed high voltage power supply system of the BESⅢ drift chamber in the beam test of the full length prototype of drift chamber,a full system covering all the channels of high voltage was installed.The system's training and the high voltage value adjustment were carried out in the cosmic ray test of the BESⅢ drift chamber.The cosmic ray test for the full system and its final installation on the BESⅢ drift chamber were reported.The full system of high voltage power supply works stably and reliably. 相似文献
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总结了1990年6月到1993年10月期间西藏空气簇射阵列的观测结果。寻找了来自于蟹状星云、X射线双星、脉冲星、活动星系核和其它活动天体的能量为10TeVγ射线连续发射,没有发现连续稳定发射的迹象,但给出了每个源的流强上限。在阵列所观测的天区寻找了10TeV的γ暴,结果没有发现能量10TeV的γ暴,最后也给出了发现此种γ暴的上限。应用该阵列,明显地观测到了能量为10TeV的宇宙线流强的太阳和月亮阴影。观测了朝向和远离太阳的行星际空间磁场对宇宙线阴影的影响,这是行星际磁场对阴影位移影响的第一次直接观测。研究并发现在实验期间,太阳阴影的位置每年都在变化。同时观测在此期间,朝向和远离方向的宇宙线阴影的不同变化。另外,应用该实验的数据,给出了所谓的“膝”区的原初宇宙线能谱。 相似文献
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S Biswas R Chakraborti R Cowsik N Durgaprasad P J Kajarekar R K Singh M N Vahia J S Yadav N Dutt J N Goswami D Lal H S Mazumdar D V Subhedar M K Padmanabhan 《Pramana》1986,27(1-2):89-104
The measurements of the ionization states, composition, energy spectra and spatial distribution of heavy ions of helium to
iron of energies 10–100 MeV/amu in the anomalous cosmic rays are of major importance in understanding their origin which is
unknown at present.Anuradha (IONS) cosmic ray experiment in Spacelab-3 was designed to determine the above properties in near earth space and this had
a highly successful flight and operations aboard the shuttle Challenger at an orbital altitude of 352 km during 29 April to
6 May 1985. The instrument employs solid state nuclear track detectors (CR-39) of high sensitivity and large collecting area
of about 800 cm2 and determines the arrival time information of particles with active elements. Experimental methods, flight operations and
preliminary results are briefly described. Initial results indicate that relatively high fluxes of low energy cosmic ray α-particles,
oxygen group and heavier ions were obtained. The flight period corresponded to that of quiet Sun and the level of solar activity
was close to solar minimum. It is estimated that about 10,000 events of low energy cosmic ray alpha particles with time annotation
are recorded in the detector together with similar number of events of oxygen and heavier ions of low energy cosmic rays.
The authors felicitate Prof. D S Kothari on his eightieth birthday and dedicate this paper to him on this occasion. 相似文献
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M. A. Kondratyeva Ch. A. Tretyakova S. P. Tretyakova D. A. Zhuravlev 《Radiation measurements》2001,34(1-6):293-295
For observation of low energy cosmic ray particles we used CN-Kodak nuclear track detectors on Cosmos satellites. In solar quiet periods during solar minima conditions the detectors registered anomalous cosmic rays (ACRs). The ACRs are characterized by flux enhancements of several elements and it is known that the carbon enhancement is small compared with that of oxygen. In all of our quiet-time exposures the relation between carbon and oxygen was extremely small (C/O 0.03). But in two quiet-time periods of 14.03.96–11.06.96 and of 15.12.97–14.04.98 we have identified many tracks as carbon in a L–R diagram. As a result the observed C/O ratio appears to be more than 0.5, whereas other experiments show no evidence of enhanced flux of carbon during these periods. The reason for the unexpected response of CN-Kodak is discussed. 相似文献
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W. Weber 《Annalen der Physik》2010,522(6):372-381
Terrestrial solar irradiance data of the Smithsonian Astrophysical Observatory from 1905 to 1954 and of Mauna Loa Observatory from 1958 to 2008 are analyzed. The analysis shows that, with changing solar activity, the atmosphere modifies the solar irradiance on the percentage level, in all likelihood via cosmic ray intensity variations produced by the active sun. The analysis strongly suggests that cosmic rays cause a large part of the atmospheric aerosols. These aerosols show specific absorption and scattering properties due to an inner structure of hydrated ionic centers, most probably of O2‐ and O2+ produced by the cosmic rays. 相似文献