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Deuteron and Antideuteron Production in Galactic Cosmic-Rays

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Deuteron and Antideuteron Production in Galactic Cosmic-Rays UNIVERSIDAD NACIONAL AUTONOMA´ DE MEXICO´ POSGRADO EN CIENCIAS F´ISICAS INSTITUTO DE F´ISICA Deuteron and antideuteron production in galactic cosmic-rays Tesis QUE PARA OPTAR POR EL GRADO DE: DOCTOR EN CIENCIAS (F´ISICA) PRESENTA: Diego Mauricio G´omezCoral TUTOR PRINCIPAL: Dr. Arturo Alejandro Menchaca Rocha Instituto de F´ısica CERN-THESIS-2019-034 26/04/2019 MIEMBROS DEL COMITE´ TUTOR: Dr. Varlen Grabski Instituto de F´ısica Dr. Andr´esSandoval Espinosa Instituto de F´ısica CIUDAD DE MEXICO´ 29 de abril de 2019 Producci´onde deuterio y antideuterio en rayos c´osmicosgal´acticos Diego Mauricio G´omezCoral 29 de abril de 2019 To my beloved family: Glorita, Hernando, Carito, and Mart´ın. Abstract The increasing role of antideuterons in the indirect search for dark matter and new cosmic-ray propagation features from deuterons have generated that the study of the cosmic-ray deuteron and antideuteron receives an increasing interest in current astrophysics investigations. To de- termine such fluxes precisely, it is necessary to consider the contribution from the nuclear in- teractions of primary cosmic rays with the interstellar matter. For that purpose, in this thesis, the production of cosmic-ray deuterons and antideuterons in the Galaxy is calculated using advanced Monte Carlo (MC) generators and an updated database of collider measurements. Deuteron and antideuteron production in hadron interactions is modeled through the coa- lescence model, which has demonstrated to reproduce data successfully. The coalescence mech- anism is simulated with an event-by-event afterburner in tandem with MC generators such as EPOS-LHC, QGSJET-II-04, and FTFP-GEANT4. These estimates depend on a single parame- ter (p0) obtained from a fit to the latest collider data, including ALICE-LHC current results. It was found that p0 for antideuterons is not a constant at all energies as previous works suggested, and as a result, the antideuteron production cross section can be at least 20 times smaller in the low collision energy region than earlier estimations. CR deuterons and antideuterons propagation in the Galaxy is calculated using GALPROP, along with a set of parameters that fit AMS-02 latest observations in proton, Helium and Boron- to-Carbon ratio. The resulting antideuteron flux, employing EPOS-LHC, shows a larger mag- nitude compared to previous studies and a slightly different shape in the energy distribution as a consequence of the coalescence parameter (p0) energy dependence. Deuteron flux evaluation with QGSJET-II-04 shows an improved description of measurements at high energy compared to the result without considering coalescence. A simulation of the antideuteron production in AMS-02 as a consequence of CR collisions with the detector materials was conducted. It was concluded, that it is unlikely an antideuteron generated in the detector can be misidentified as an antideuteron from an external source in the lifetime of AMS-02 operations. iii iv Resumen El creciente inter´esen la b´usquedaindirecta de materia oscura a trav´esde la detecci´onde antideuterones, as´ıcomo la posibilidad de encontrar nuevas caracter´ısticasen la propagaci´onde rayos c´osmicosen la galaxia usando la raz´onentre deuterones y helio, motivan la realizaci´on de este trabajo. En este contexto, se vuelve fundamental entender y calcular con las her- ramientas m´asmodernas y con los conocimientos m´asrecientes la producci´onde deuterones y antideuterones a trav´esde colisiones nucleares entre los rayos c´osmicosprimarios y el medio inter- estelar. Por estos motivos en este trabajo se estima la producci´onde deuterones y antideuterones en la galaxia usando generadores Monte Carlo (MC) y una base de datos actualizada de medidas realizadas en experimentos sobre colisiones de part´ıculas. La producci´onde deuterones y antideuterones en la galaxia se describe con el modelo de coalescencia, el cual a demostrado ser acertado en la predicci´onde los datos experimentales. La implementaci´onde la simulaci´ondel modelo de coalescencia se realiza usando un gratinador o \afterburner", en conjunto con los generadores Monte Carlo (EPOS-LHC, QGSJET-II-04 y FTFP-GEANT4). Las predicciones de la simulaci´ondependen de un solo par´ametro,el momento de coalescencia (p0), el cual se obtiene de los datos sobre colisiones incluyendo los resultados actuales de ALICE-LHC. En este trabajo se encontr´oque para antideuterones p0 no es constante a todas las energ´ıascomo se afirmaba en trabajos previos. Como consecuencia, la secci´oneficaz de producci´onde antideuterones puede llegar a ser 20 veces menor a lo encontrado anteriormente en la regi´onde baja energ´ıa. La propagaci´onde deuterones y antideuterones en la galaxia fue calculada con GALPROP, usando par´ametrosque fueron ajustados a datos recientes del experimento AMS-02. El flujo de antideuterones estimado con EPOS-LHC, muestra una magnitud mayor comparada con c´alculos anteriores, as´ı como tambi´enuna forma ligeramente diferente en la distribuci´onde energ´ıa. Dicha diferencia es consecuencia de p0 y su dependencia con la energ´ıa.Por otro lado, el flujo de deuterones en rayos c´osmicoscalculado con QGSJET-II-04 y el modelo de coalescencia describe apropiadamente los datos a altas energ´ıas. Por ´ultimo,se realiz´ouna simulaci´onde la producci´onde antideuterones en AMS-02 como consecuencia de las colisiones de rayos c´osmicoscon los materiales del detector. Se concluy´o que es muy poco probable que un antideuteron producido en el detector se confunda con un antideuteron proveniente de la Galaxia durante el tiempo de operaci´onde AMS-02. v vi Acknowledgments I want to express my sincere gratitude to my advisor Prof. Arturo Menchaca for his continuous support developing ideas for the construction of this work, as well as his comments, critics and corrections to this manuscript. Furthermore, I thank him for encouraging me to recognize my abilities and to pursue a research career. My sincere thanks also goes to the rest of my advisor committee: Prof. Andr´esSandoval and especially Prof. Varlen Grabski, who helped me many times to solve arising questions during the elaboration of this work. Besides, I want also to thank the thesis evaluation committee: Dra. Irais Bautista, Dra. Catalina Espinoza, Dr. Gustavo Medina Tanco, and Dr. Jos´eVald´es. I am also grateful to the cosmic-ray group at the University of Hawaii at Manoa led by Prof. Philip von Doetinchem, and its members Dr. Amaresh Datta, and Anirvan Shukla. A special mention to the computation department of the Institute of Physics, UNAM in particular to Carlos Ernesto L´opez Natar´en.I also thank T. Pierog, C. Baus, and R. Ulrich for providing the Cosmic Ray Monte Carlo package and for answering my questions about the program. The GALPROP team for allowing me to use and to edit the propagation code. Vladimir Uzhinskii and Dennis Wright who observed and commented on some of the results from this work and made suggestions about the afterburner implementation in GEANT4. I gratefully acknowledge the financial support by CONACyT through a Ph.D. fellowship and PNPC project, and by UNAM projects: PAPIIT-DGAPA IN109617 and PAEP. A special men- tion to the institutions involved and their people: Instituto de F´ısica(IFUNAM) and Posgrado en Ciencias F´ısicasUNAM (PCF). My gratitude goes to the ALICE and AMS-02 collabora- tions for allowing me to participate in such amazing experiments and to show me a universe of knowledge and exciting open questions in particle physics and astrophysics from which I am still learning. Last but by no means the least, I would like to thank my family: Glorita, Hernando, Carito y Mart´ınfor their unconditional love and support during my studies and in my life. Special gratitude to my Colombian friends: Tatiana, Juano and Myriam. To all my friends and col- leagues who made my stay in Mexico a wonderful experience. Among them, los lovers: Guerito, Gusi, Cesar, Vladis, R2, Yorch, Peter, Jefe, Miguelover, Javier, Richi y Sult´an.Los del ciruelo: Francisco, Richard, Rafa, and Chava. My friends from the institute: Karina, David, Mario, Mariana, To~no,Javi, Zu~niga,Bora, and Sa´ul. Diego G´omez Mexico City, April 2019 vii viii Agradecimientos Agradezco profundamente a mi asesor el Dr. Arturo Menchaca por su constante apoyo en el desarrollo de ideas para la construcci´onde este trabajo, as´ıcomo su ayuda en la revisi´ony correcci´ondel mismo en varias etapas de su elaboraci´on.Tambi´enagradezco la motivaci´onque me ha transmitido para continuar un proceso acad´emico y de investigaci´on.Adem´as,agradezco a los dem´asmiembros del comit´etutor Dr. Andr´esSandoval Espinoza y especialmente al Dr. Varlen Grabski con quien acud´ınumerosas veces para consultarle inquietudes que surg´ıandurante el desarrollo del trabajo. Adem´as,quiero agradecer a los miembros del jurado evaluador: Dra. Irais Bautista, Dra. Catalina Espinoza, Dr. Gustavo Medina Tanco, y Dr. Jos´eVald´es. Tambi´enquiero expresar mi gratitud al grupo de rayos c´osmicos de la universidad de Hawaii encabezado por el Dr. Philip von Doetinchem, y sus miembros Dr. Amaresh Datta y Anirvan Shukla. Al grupo de computaci´oncient´ıfica del Instituto de F´ısica, especialmente a Carlos Ernesto L´opez Natar´en. Igualmente agradezco a T. Pierog, C. Baus, and R. Ulrich por facil- itarme el programa CRMC y resolver algunas dudas acerca de su funcionamiento, tambi´enal equipo de GALPROP por suministrar el c´odigoque se utiliz´oen este estudio. A Vladimir Uzhin- skii y Dennis Wright quienes tuvieron la amabilidad de observar y criticar algunos resultados de este trabajo as´ıcomo hacer sugerencias sobre la implementaci´ondel afterburner en GEANT4. Agradezco igualmente el apoyo financiero brindado por CONACyT a trav´esde la beca para doctorado nacional, a la UNAM con el proyecto PAPIIT-DGAPA: IN109617 y los apoyos PAEP y PNPC.
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