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Cosmic Ray Shower Simulation Study at a Global Scale and Associated Applications Georgia State University ScholarWorks @ Georgia State University Physics and Astronomy Dissertations Department of Physics and Astronomy 8-8-2017 COSMIC RAY SHOWER SIMULATION STUDY AT A GLOBAL SCALE AND ASSOCIATED APPLICATIONS Olesya Sarajlic Follow this and additional works at: https://scholarworks.gsu.edu/phy_astr_diss Recommended Citation Sarajlic, Olesya, "COSMIC RAY SHOWER SIMULATION STUDY AT A GLOBAL SCALE AND ASSOCIATED APPLICATIONS." Dissertation, Georgia State University, 2017. https://scholarworks.gsu.edu/phy_astr_diss/98 This Dissertation is brought to you for free and open access by the Department of Physics and Astronomy at ScholarWorks @ Georgia State University. It has been accepted for inclusion in Physics and Astronomy Dissertations by an authorized administrator of ScholarWorks @ Georgia State University. For more information, please contact [email protected]. COSMIC RAY SHOWER SIMULATION STUDY AT A GLOBAL SCALE AND ASSOCIATED APPLICATIONS by OLESYA SARAJLIC Under the Direction of Xiaochun He, PhD ABSTRACT Galactic cosmic rays are the high-energy particles that stream into our solar system from distant corners of our Galaxy. The Earth's atmosphere serves as an ideal detector for the high energy cosmic rays which interact with the air molecule nuclei causing propagation of extensive air showers. The primary cosmic ray particles interact with the molecules in the atmosphere and produce showers of secondary particles (mainly pions) at about 15 km altitude. These pions decay into muons which are the dominant particles of radiation (about 80%) at the surface of the Earth. In recent years, there are growing interests in the applications of the cosmic ray mea- surements such as space/earth weather monitoring, homeland security activities based on the cosmic ray muon tomography, radiation effects on health via air travel, etc. A simulation program (based on the Geant4 software package developed at CERN) has been developed at Georgia State University for studying cosmic ray showers in the at- mosphere. The results of this simulation study will provide unprecedented knowledge of geo-position-dependent cosmic ray shower profiles and will significantly advance cosmic ray applications. Simulation results are critically important for determining the temperature coefficients in every pressure layer in the atmosphere in order to calculate the tempera- ture variations using the cosmic ray data. Using a single particle shower simulation, the weighted particle altitude distributions on a global scale are calculated with geomagnetic field implementation. The results of the simulation can aid the computation of the effective temperature in stratosphere. INDEX WORDS: Cosmic rays, Geant4, geomagnetic field, single particle shower simula- tion, global weather patterns, XSEDE. COSMIC RAY SHOWER SIMULATION STUDY AT A GLOBAL SCALE AND ASSOCIATED APPLICATIONS by OLESYA SARAJLIC A Dissertation Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy in the College of Arts and Sciences Georgia State University 2017 Copyright by Olesya Sarajlic 2017 COSMIC RAY SHOWER SIMULATION STUDY AT A GLOBAL SCALE AND ASSOCIATED APPLICATIONS by OLESYA SARAJLIC Committee Chair: Xiaochun He Committee: Megan Connors Douglas Gies Murad Sarsour Electronic Version Approved: Office of Graduate Studies College of Arts and Sciences Georgia State University August 2017 iv DEDICATION This dissertation is dedicated to Nuclear Particle Group at Georgia State University. v ACKNOWLEDGEMENTS I would like to express my special appreciation to my advisor Dr. Xiaochun He who has been a tremendous mentor for me. I would like to thank Dr. He for encouraging my research and for allowing me to grow as a research scientist. I appreciate all his contributions of time, ideas, and funding to make my Ph.D. experience productive and stimulating. The joy and enthusiasm Dr. He has for his research in Cosmic Rays was extremely motivational for me, even during tough times in the Ph.D. pursuit. The members of Nuclear Physics group have contributed immensely to my personal and professional time at Georgia State. The group has been a source of friendships as well as good advice during group meeting and collaboration during hardware projects. I am especially grateful to the former Nuclear Physics group members during my graduate career for their advice and ideas: Margaret Jezghani and Xiaohang Zhang. I would like to acknowledge a former postdoc, Liang Xue, who inspired me by his hard work. Other past and present group members that I have had the pleasure to work with are the graduate students of Nuclear Physics group: Tristan Haseler, Cheuk-Ping Wong, Montgomery Steele, Anthony Hodges, Cody Hunley, and Beena Meena; electronics developer Sawaiz Syed; specialist in assembly of scintillator detectors Carola Butler; visiting scientist Dr. Raphael Tieulent; and the numerous undergraduate students who have come through the lab. For this dissertation I would like to thank my committee members: Dr. Murad Sarsour, Dr. Megan Connors, and Dr. Douglas Gies for their time, interest, and helpful comments. I gratefully acknowledge the funding sources that made my Ph.D. work possible. My last year I was honored to be a Provost Dissertation Fellow. I would like to thank Semir Sarajlic for his assistance with exploration of XSEDE computing resources, and the use of resources via XSEDE Campus Champion Grant - GEO150002. In addition, I would like to acknowledge the use of XSEDE resources via our Startup grant - PHY160043. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is vi supported by National Science Foundation grant number ACI-1053575. Most importantly, I would like to thank my family for all their love and encouragement. I would like to express my sincere gratitude to my mother and father for their constant support and inspiration throughout this research work toward pursuing my Ph.D. Most of all, I would like to thank my loving, encouraging, and patient husband, Semir, whose faithful support throughout my graduate career is greatly appreciated. I also dedicate this Ph.D. dissertation to my son, Dennis, who is the pride and joy of my life. The support and care of my immediate family helped me to stay focused on my graduate study and pursuit of this Ph.D. vii TABLE OF CONTENTS ACKNOWLEDGEMENTS ::::::::::::::::: v LIST OF TABLES :::::::::::::::::::: x LIST OF FIGURES :::::::::::::::::::: xi LIST OF ABBREVIATIONS :::::::::::::::: xxviii CHAPTER 1 INTRODUCTION ::::::::::::::: 1 CHAPTER 2 COSMIC RAY SHOWERS IN THE ATMOSPHERE : 5 2.1 Discovery of Cosmic Rays ........................ 5 2.1.1 Solar Effects . 8 2.1.2 Geomagnetic Effects . 10 2.1.3 Meteorological Effects . 10 2.2 Applications with Cosmic Ray Measurements . 13 2.2.1 Cosmic Ray Muon Tomography . 13 2.2.2 Atmospheric Ionization . 13 2.2.3 Monitoring the Effective Temperature of the Atmosphere . 17 CHAPTER 3 COSMIC RAY SHOWER SIMULATION :::::: 18 3.1 Geant4 Simulation Software ....................... 18 3.2 ECRS Simulation Setup ......................... 19 3.2.1 Modeling the Atmospheric Layers . 19 3.2.2 Geomagnetic Field Implementation . 21 3.2.3 Physics Processes . 25 3.3 ECRS and CORSIKA Comparison ................... 36 3.3.1 Magnetic Field . 37 viii 3.3.2 Atmosphere . 37 3.3.3 Physics Processes . 38 3.3.4 Comparing Simulation Variables . 39 CHAPTER 4 STUDIES OF SINGLE PARTICLE COSMIC RAY SHOW- ERS IN THE ATMOSPHERE :::::::::: 44 4.1 Computing Resources and Challenges . 44 4.2 Cosmic Ray Shower Characteristics without Geomagnetic Field 47 4.3 Geomagnetic Field Effect on Cosmic Ray Shower Characteristics 56 4.3.1 Cosmic Ray Shower Characteristics on a Global Scale . 56 4.3.2 Production Altitude and Lateral Distribution . 63 4.3.3 Cosmic Ray Showers around Major Cities . 75 4.4 Diurnal Variations ............................. 81 4.5 High Energy Showers with Geomagnetic Field . 83 4.5.1 Production Altitude . 84 4.5.2 Lateral Distribution . 86 4.5.3 Energy Distribution . 92 4.6 Single Particle Weight Function .................... 97 CHAPTER 5 SUMMARY AND OUTLOOK :::::::::: 101 REFERENCES ::::::::::::::::::::: 103 APPENDICES :::::::::::::::::::::: 115 Appendix A ECRS: SELECTED MACROS AND ANALYSIS CODE 115 A.1 Job Submission Macro . 115 A.1.1 Defined Geo-position . 115 A.1.2 Global Showers . 119 A.2 Analysis Code: Selected Cases . 121 ix Appendix B CORSIKA: INSTALLATION, DATA ACQUISITION, AND ANALYSIS :::::::::::::::::: 124 B.1 Installation and Data Acquisition . 124 B.2 Analysis ................................... 127 Appendix C GEANT4: CORE STRUCTURE OF THE ECRS SIMULA- TION :::::::::::::::::::: 130 Appendix D CANDLE PLOT :::::::::::::::: 133 x LIST OF TABLES Table 3.1 Temperature and pressure variables for three different atmospheric re- gions: the troposphere, lower stratosphere, and upper stratosphere. 20 Table 3.2 Physics lists acronyms (hadronic options). 26 Table 3.3 Comparison of ECRS and CORSIKA simulation variables. 36 Table 3.4 Linsley's model coefficients for U. S. Standard Atmosphere for five layers used to parameterize the atmosphere in CORSIKA air shower simulation. 38 Table B.1 Sample of the all − input simulation configuration file for CORSIKA. 126 xi LIST OF FIGURES Figure 1.1 (color online) An illustration of the Pierre Auger Observatory. Left panel shows the schematic representation of the surface array of de- tectors with the particle cascade from the primary cosmic rays. Right panel shows the bird's eye view of the Pierre Auger Observatory. 2 Figure 1.2 (color online) Cosmic ray muon telescopes developed by the Nuclear Physics Group at Georgia State University. 3 Figure 2.1 (color online) Left panel: data from ionization rate measurements by Hess (1912) which shows the increase of ionization with altitude. Right panel: data from coincidence measurements by Regener and Pfotzer. The coincidence rate per 4 minutes at a solid angle of 20 degrees about the zenith is shown as function of decreasing pressure (data points and curve labeled `I'). Data corrected for dead-time losses are shown as the curve labeled `II'. The coincidence rate is at its maximum at about a pressure of 100 mm Hg. 6 Figure 2.2 (color online) Flux distribution of CRs as a function of energy.
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