發(fā)布時(shí)間：2018-04-05 08:05

  本文選題：γ射線(xiàn)　切入點(diǎn)：100TeV　出處：《河北師范大學(xué)》2014年碩士論文

【摘要】：自1912年Victor Hess發(fā)現(xiàn)宇宙線(xiàn)至今，一百多年來(lái)，人們通過(guò)對(duì)宇宙線(xiàn)的研究，推動(dòng)了粒子物理和天體物理的發(fā)展。但是，宇宙線(xiàn)的起源和加速問(wèn)題仍是沒(méi)有得到解決的世紀(jì)難題。人們普遍認(rèn)為對(duì)100TeV能區(qū)γ射線(xiàn)的觀(guān)測(cè)是尋找宇宙線(xiàn)源的最有效手段。 中日合作ASγ實(shí)驗(yàn)位于西藏當(dāng)雄縣羊八井鎮(zhèn)，海拔4300m，擁有789個(gè)閃爍體探測(cè)器（Tibet-III）和已建成的5組水契倫科夫地下繆子單元探測(cè)器（MD-I）。為了進(jìn)一步提高實(shí)驗(yàn)的靈敏度，我們計(jì)劃在現(xiàn)有表面陣列的外圍增設(shè)160個(gè)閃爍體探測(cè)器，，這樣不僅可以花費(fèi)少，而且把100TeV能區(qū)的有效探測(cè)面積增大2倍。實(shí)驗(yàn)靈敏度將在TibetIII+MD-I的基礎(chǔ)上提高2倍，我們稱(chēng)升級(jí)陣列為“擴(kuò)展陣列”。 本論文重點(diǎn)介紹本人在碩士研究生期間參與的ASγ實(shí)驗(yàn)擴(kuò)展陣列探測(cè)器研制、測(cè)試和優(yōu)化工作。首先第一章和第二章分別簡(jiǎn)要介紹了宇宙射線(xiàn)的背景知識(shí)和西藏羊八井ASγ實(shí)驗(yàn)。在第三章介紹了對(duì)四種2英寸候選光電倍增管的主要性能（絕對(duì)增益、高壓響應(yīng)、暗計(jì)數(shù)率、讀出信號(hào)線(xiàn)性范圍、地磁效應(yīng)、光陰極的均勻性以及時(shí)間特性）的測(cè)試方法和測(cè)試結(jié)果。第四章介紹了通過(guò)改進(jìn)光電倍增管R7725CA0130的分壓器（優(yōu)化分壓配比，使用“錐形分壓”），采用陽(yáng)極和第9打拿極共同讀出來(lái)實(shí)現(xiàn)探測(cè)器對(duì)大動(dòng)態(tài)范圍的要求。第五章是對(duì)研制的擴(kuò)展陣列原型探測(cè)器的電荷和時(shí)間一致性的性能測(cè)試。第六章是總結(jié)和展望。
[Abstract]:Since the discovery of cosmic rays by Victor Hess in 1912, the research on cosmic rays has promoted the development of particle physics and astrophysics.However, the origin and acceleration of cosmic rays are still unsolved century problems.It is generally believed that the observation of 緯-ray in the 100TeV energy region is the most effective way to find the cosmic ray source.The Sino-Japanese cooperative as 緯 experiment is located in Yangbajing Town, Dangxiong County, Tibet, at an altitude of 4300m. It has 789 scintillator detectors Tibet-III) and five groups of underground Miao subunit detectors of Shuichilenkov, Tibet.In order to further improve the experimental sensitivity, we plan to add 160 scintillator detectors to the periphery of the existing surface array, which can not only cost less, but also increase the effective detection area of the 100TeV energy region by 2 times.The experimental sensitivity will double that of TibetIII MD-I. We call the upgraded array "extended array."This thesis focuses on the development, test and optimization of as 緯-experiment expanded array detector.In the first and second chapters, the background of cosmic ray and the as 緯 experiment of Yangbajing in Tibet are briefly introduced.In chapter 3, the main performances of four 2-inch candidate photomultiplier tubes (absolute gain, high voltage response, dark counting rate, linear range of readout signal, geomagnetic effect) are introduced.Methods and results of measurement of photocathode uniformity and time characteristics.In the fourth chapter, by improving the voltage divider of the photomultiplier tube (R7725CA0130), the requirements of the detector for a large dynamic range are realized by using the anode and the 9th pole to read out the detector by optimizing the proportion of the voltage divider, using the "conical voltage divider" and using the anode and the 9th pole.The fifth chapter is the performance test of charge and time consistency of the prototype detector with extended array.The sixth chapter is the summary and prospect.
【學(xué)位授予單位】：河北師范大學(xué)
【學(xué)位級(jí)別】：碩士
【學(xué)位授予年份】：2014
【分類(lèi)號(hào)】：P171

【參考文獻(xiàn)】

相關(guān)期刊論文 前1條

1 馮朝陽(yáng);張毅;劉成;樊超;李紅超;王博;吳含榮;胡紅波;盧紅;譚有恒;;Study on the separation of 100 TeV γ-rays from cosmic rays for the Tibet ASγ experiment[J];中國(guó)物理C;2011年02期

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