{"id":96681,"date":"2018-03-11T10:16:57","date_gmt":"2018-03-11T10:16:57","guid":{"rendered":"https:\/\/www.deberes.net\/tesis\/sin-categoria\/composition-and-energy-determination-in-cosmic-ray-surface-arrays-an-applicatio-to-the-pierre-auger-observatory\/"},"modified":"2018-03-11T10:16:57","modified_gmt":"2018-03-11T10:16:57","slug":"composition-and-energy-determination-in-cosmic-ray-surface-arrays-an-applicatio-to-the-pierre-auger-observatory","status":"publish","type":"post","link":"https:\/\/www.deberes.net\/tesis\/rayos-cosmicos\/composition-and-energy-determination-in-cosmic-ray-surface-arrays-an-applicatio-to-the-pierre-auger-observatory\/","title":{"rendered":"Composition and energy determination in cosmic ray surface arrays: an applicatio to the pierre auger observatory"},"content":{"rendered":"<h2>Tesis doctoral de <strong> Germ\u00e1n Ros Mag\u00e1n <\/strong><\/h2>\n<p>Esta tesis se enmarca dentro del estudio de los rayos c\u00f3smicos de ultra-alta energ\u00eda, aquellos a los que se dedica el observatorio pierre auger. Tras una breve introducci\u00f3n, en el segundo cap\u00edtulo se resumen los aspectos b\u00e1sicos de la f\u00edsica de rayos c\u00f3smicos, desde su espectro de energ\u00eda, composici\u00f3n y su posible origen, hasta las cuestiones que a\u00fan permanecen desconocidas. En el siguiente cap\u00edtulo se describen las caracter\u00edsticas singulares del observatorio pierre auger y se muestran los resultados publicados m\u00e1s importantes hasta este momento. En los cap\u00edtulos siguientes se abordan los temas centrales de este trabajo: la determinaci\u00f3n de la energ\u00eda y la composici\u00f3n de los rayos c\u00f3smicos de ultra-alta energ\u00eda a partir de su detecci\u00f3n con detectores de superficie. Inicialmente se analiza la determinaci\u00f3n de la energ\u00eda. Se ha propuesto una nueva t\u00e9cnica, y se ha demostrado su aplicabilidad en los detectores de superficie. Adem\u00e1s, se ha mostrado que es significativamente mejor que la que se ha utilizado hasta hoy por parte de todos los experimentos de este tipo. En segundo lugar, se ha propuesto un nuevo par\u00e1metro sensible a la composici\u00f3n del rayo c\u00f3smico primario, el cual se determina a partir de la se\u00f1al y la posici\u00f3n de los detectores de superficie para cada evento. Se han estudiado sus propiedades y se ha demostrado que es capaz de determinar la composici\u00f3n promedio de los rayos c\u00f3smicos de ultra-alta energ\u00eda con mayor precisi\u00f3n que los par\u00e1metros m\u00e1s fiables que se est\u00e1n utilizando hoy en d\u00eda. A continuaci\u00f3n, se han explicado varios trabajos que se est\u00e1n desarrollando y en los que se seguir\u00e1 trabajando en un futuro cercano, relacionados con ambos aspectos, la determinaci\u00f3n de la energ\u00eda y la composici\u00f3n, y se han resumido las conclusiones del trabajo. Para terminar, se han a\u00f1adido varios ap\u00e9ndices y una extensa bibliograf\u00eda.   this thesis studies how to determine the primary energy and the chemical composition of ultra-high energy cosmic rays in pure surface array experiments, and also, how to apply these techniques in the pierre auger observatory. Chapter 1 is a brief introduction. In chapter 2, the main aspects about cosmic ray physics regarding their energy, composition and origin are presented, as well as the questions that still remain open. Next, chapter 3 gives a brief description of the pierre auger observatory, focusing in the detection techniques used and the advantages of auger. The main composition observables are presented and the results published by auger in recent years are summarized and commented. In chapter 4, a new technique to determine the primary energy is shown and applied to pure surface arrays. We demonstrate that the energy determination is more accurate by using this new technique compared to the traditional one that all the previous surface experiments have been used. Chapter 5 is devoted to a new parameter sensitive to the primary composition. We have demonstrated that the average mass inferred by using the new composition estimator is more accurate than that obtained with other parameters traditionally used by cosmic ray experiments. On-going work and perspectives are presented in chapter 6 and the conclusions in chapter 7. Finally several appendixes and an extensive bibliography are included.<\/p>\n<p>&nbsp;<\/p>\n<h3>Datos acad\u00e9micos de la tesis doctoral \u00ab<strong>Composition and energy determination in cosmic ray surface arrays: an applicatio to the pierre auger observatory<\/strong>\u00ab<\/h3>\n<ul>\n<li><strong>T\u00edtulo de la tesis:<\/strong>\u00a0 Composition and energy determination in cosmic ray surface arrays: an applicatio to the pierre auger observatory <\/li>\n<li><strong>Autor:<\/strong>\u00a0 Germ\u00e1n Ros Mag\u00e1n <\/li>\n<li><strong>Universidad:<\/strong>\u00a0 Alcal\u00e1<\/li>\n<li><strong>Fecha de lectura de la tesis:<\/strong>\u00a0 21\/10\/2009<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n<h3>Direcci\u00f3n y tribunal<\/h3>\n<ul>\n<li><strong>Director de la tesis<\/strong>\n<ul>\n<li>Luis Del Peral Gochicoa<\/li>\n<\/ul>\n<\/li>\n<li><strong>Tribunal<\/strong>\n<ul>\n<li>Presidente del tribunal: giorgio Matthiae <\/li>\n<li>Jos\u00e9 Vald\u00e9s galicia (vocal)<\/li>\n<li>Antonio Bueno villar (vocal)<\/li>\n<li>Juan  Antonio Fuster verdu (vocal)<\/li>\n<\/ul>\n<\/li>\n<\/ul>\n<p>&nbsp;<\/p>\n","protected":false},"excerpt":{"rendered":"<p>Tesis doctoral de Germ\u00e1n Ros Mag\u00e1n Esta tesis se enmarca dentro del estudio de los rayos c\u00f3smicos de ultra-alta energ\u00eda, [&hellip;]<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"site-sidebar-layout":"default","site-content-layout":"","ast-site-content-layout":"","site-content-style":"default","site-sidebar-style":"default","ast-global-header-display":"","ast-banner-title-visibility":"","ast-main-header-display":"","ast-hfb-above-header-display":"","ast-hfb-below-header-display":"","ast-hfb-mobile-header-display":"","site-post-title":"","ast-breadcrumbs-content":"","ast-featured-img":"","footer-sml-layout":"","theme-transparent-header-meta":"","adv-header-id-meta":"","stick-header-meta":"","header-above-stick-meta":"","header-main-stick-meta":"","header-below-stick-meta":"","astra-migrate-meta-layouts":"default","ast-page-background-enabled":"default","ast-page-background-meta":{"desktop":{"background-color":"var(--ast-global-color-4)","background-image":"","background-repeat":"repeat","background-position":"center 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