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姓名	周欣毅(Hsin-Yi Chou)  查詢紙本館藏	畢業系所	物理學系
論文名稱	利用國際太空站上的反物質磁譜儀精確測量宇宙射線中的反質子與質子通量比的時間變化 (Measurement Time Variation of the Antiproton-to-Proton Flux Ratio with the Alpha Magnetic Spectrometer on the International Space Station)
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摘要(中)	我們提出一種針對高能物理實驗的軌跡演算法處理非高斯探測器效應,它使用完整的傳播模型預測粒子軌跡以及靈活參數化模型(FPM算法),以描述非高斯探測器效應的表現。FPM軌跡演算法顯著提升測量的分辨解析度速度、剛度(每單位電荷的動量)以及質量。 利用國際太空站(ISS)上的反物質磁譜儀(AMS)精確測量宇宙射線中的反質子與質子通量比在絕對剛度區間1GV至525GV,並從2011年5月19日至2019年10月29日期間收集6.92億質子跟81萬的反質子。反質子與質子通量比在~30GV達到最大值,其譜指數在高剛度時為零。 利用國際太空站上的反物質磁譜儀精確測量宇宙射線中的反質子與質子通量比的時間變化在絕對剛度區間1GV至45.1GV,並從2011年5月至2019年10月期間(由於AMS的TTCS關閉,故BR2427至BR2474除外。)收集6.78億質子跟78萬的反質子。這些數據允許研究在太陽磁極性反轉期間的剛度和電荷符號依賴性。反質子與質子通量比以及電子與正電子的通量比的時間變化顯示出相同的振幅剛性依賴性在絕對剛度高於2GV時,以及兩者在過渡期的週期(持續時間)剛度獨立性。兩者之間的時間延遲在過渡期間顯示出剛性依賴性。其值約1年在絕對剛度低於3GV,並在~7GV處為零。
摘要(英)	We present a new tracking algorithm for high energy physics experiments dedicated to handling the non-Gaussian detector effects. It uses a comprehensive propagation model to predict the particle trajectory, as well as flexible and parameterized models (FPM method), to describe non-Gaussian detector effects. The performance of the FPM tracking algorithm shows significant improvements in the measurement resolution of velocity, rigidity (momentum per unit charge), and mass. A precision measurement of the antiproton-to-proton flux ratio in primary cosmic rays in absolute rigidity range from 1 to 525 GV is presented based on ∼6.92 billion proton events and ∼0.81 million antiproton events, collected by the Alpha Magnetic Spectrometer (AMS), on the International Space Station (ISS) from May 19. 2011, to October 29, 2019. The antiproton-to-proton flux ratio reaches a maximum at ∼ 30 GV, and its spectral index crosses zero at high rigidity. A precision time variation measurement of the antiproton-to-proton flux ratio in the absolute rigidity range from 1.0 GV to 45.1 GV as a function of Bartels rotation (BR; 27 days), from May 2011 to October 2019, excluded period BR2472-BR2474 which is TTCS-OFF in the AMS, is presented based on ∼6.78 billion proton events and ∼0.78 million antiproton events collected by the AMS on the ISS. These data allow studies of the rigidity and charge-sign dependence during the polarity reversal of the solar magnetic field. The time variation of the antiproton-to-proton flux ratio and the electron-to-positron flux ratio show the same rigidity dependence on the amplitude of the transition when absolute rigidity above 2 GV, and the rigidity independence on the period (duration) of the transition. The time delay of the transition between two flux ratios shows the rigidity dependence. Its value reaches ∼1 year when absolute rigidity below 3GV, and crosses zero at ∼7 GV.
關鍵字(中)	★ 反物質磁譜儀 ★ 宇宙射線 ★ 磁極性反轉 ★ 太陽磁場 ★ 反質子 ★ 軌跡演算法	關鍵字(英)	★ AMS ★ cosmic rays ★ polarity reversal ★ solar magnetic field ★ antiproton ★ tracking algorithm
論文目次	1 Introduction 29 2 Cosmic Rays in the Galaxy 31 2.1 Experimental Observations ............................ 31 2.1.1 Energy Spectra............................... 31 2.1.2 Chemical Composition........................... 33 2.2 Galactic CosmicRay................................ 38 2.2.1 The Galaxy................................. 38 2.2.2 Cosmic Ray Propagation.......................... 39 2.2.3 Measurements................................ 42 2.3 Solar Modulation.................................. 44 2.3.1 Solar Wind ................................. 44 2.3.2 GCR Transport Equation.......................... 44 2.3.3 Force-Field Approximation ........................ 45 2.3.4 Charge-Sign Dependent Effect....................... 46 2.4 Earth’s Magnetic Field............................... 49 2.5 Dark Matter Search ................................ 52 2.5.1 Dark Matter Search Using Antiparticles ................. 52 3 The Alpha Magnetic Spectrometer 57 3.1 The AMS Detector................................. 57 3.1.1 The Coordinate System .......................... 57 3.1.2 Permanent Magnetic and Silicon Tracker................. 58 3.1.3 Time-of-Flight Counters (TOF)...................... 60 3.1.4 Anti-Coincidence Counters (ACC) .................... 60 3.1.5 Transition Radiation Detector (TRD) .................. 60 3.1.6 Ring Imaging Cherenkov Detector(RICH)................ 61 3.1.7 Electromagnetic Calorimeter(ECAL) .................. 62 3.1.8 Particle Identification ........................... 62 3.2 Trigger and Data Acquisition (DAQ)....................... 63 3.3 Calibration and Test Beam ............................ 66 3.4 Data Correction and Monte Carlo Simulation .................. 66 4 The Tracking Algorithm using Flexible and Parameterized Models 69 4.1 Introduction..................................... 69 4.2 Propagation Model................................. 72 4.2.1 Lorentz Force................................ 72 4.2.2 Multiple Scattering............................. 73 4.2.3 Ionization Energy Loss........................... 74 4.2.4 Bremsstrahlung Energy Loss ....................... 76 4.2.5 Numerical Integration Method ...................... 76 4.3 Measurement Models................................ 78 4.3.1 The Symmetrical Multi-Gaussian Model ................. 78 4.3.2 The Approximate Landau-Gaussian Model............... 80 4.3.3 Robust Statistical Method......................... 83 4.4 Minimization Method ............................... 86 4.5 Track Reconstruction................................ 88 4.6 Performances .................................... 92 4.6.1 MC Simulations .............................. 92 4.6.2 Flight Data................................. 94 4.7 Summary ......................................101 5 Antiproton-to-Proton Flux Ratio 103 5.1 Event Selection and Data Samples ........................104 5.1.1 Real Time Information (RTI) .......................105 5.1.2 Geomagnetic Rigidity Cutoff .......................105 5.1.3 General Selection of Events ........................106 5.2 Measurement Strategy ...............................108 5.2.1 The Low Rigidity Region(1.00-13.0GV) ......... .......109 5.2.2 The Intermediate Rigidity Region(13.0-60.3GV) ...........113 5.2.3 The High Rigidity Region(60.3-525.0GV)...............114 5.3 Flux and Flux Ratio ................................118 5.3.1 Exposure Time ...............................118 5.3.2 5.3.2 Trigger Efficiency..............................119 5.3.3 Effective Acceptance ............................119 5.3.4 Antiproton-to-Proton Flux Ratio .....................120 5.4 Systematic Errors..................................123 5.4.1 Event Selection Uncertainties .......................123 5.4.2 Effective Acceptance Uncertainties ....................123 5.4.3 Rigidity Measurement Uncertainties ...................125 5.4.4 Summary of Errors.............................126 5.5 The Antiproton-to-Proton Flux Ratio ......................132 5.5.1 Fine Structure of the FluxRatio .....................132 5.6 The Time Variation of the Antiproton-to-Proton Flux Ratio .......... 135 5.6.1 Measurement Strategy and Result ....................135 5.6.2 Charge-Sign Dependent Effect.......................139 5.7 Summary ......................................146 6 Conclusion and Outlook 147 6.1 Charge Reconstruction...............................148 6.2 Continued Observations to 2024 and Beyond........ ........... 150 A Supplemental Materials of the Tracking Algorithm 151 A.1 Units, Constants, and Definitions .........................151 A.2 Density Effect Correction .............................153 A.3 Runge-Kutta-Nystrom Method .......................... 153 B Tables 155 B.1 The Antiproton-to-Proton Flux Ratio ...................... 155 Bibliography 159
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指導教授	張元翰(Yuan-Hann Chang)	審核日期	2020-7-23
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