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Título : On the formation of globular clusters from tidal streams
Autor : Noreña Blandón, David Andrés
Asesor : Muñoz Cuartas, Juan Carlos
Palabras clave : Theoretical Framework
Globular Clusters
The Satellite Galaxy
Gravitational Potential Evaluation
Turbulent Molecular Clouds
Density
Fecha de publicación : 2018
Editorial : Universidad de Antioquia
Citación : Noreña, D. On the formation of globular clusters from tidal streams (Tesis de Maestría). Universidad de Antioquia, Medellín, Colombia. 2018
Abstract : INTRODUCTION: Globular Clusters are old acquaintances for Astrophysics, but the interest in them remains unchanged. It has been established that a globular cluster is a stellar system consisting of between 104 to 106 gravitationally bound stars, spherically distributed around the center of mass of the cluster (see Figure1.1). The number of belonging stars and spatial distribution are precisely two of the parameters that di erentiate globular from open clusters, which are less numerous and their stars are distributed in less-de ned shapes in space [Binney 2008]. In addition, for the Milky Way (MW), open clusters are found only in the galactic disk, unlike the vast distribution of globular clusters present both in the vicinity of the disc and all over the galactic halo [Carroll 2007]. With regard to this spatial distribution, globular clusters are divided in two distinct populations, being the metallicity and the ages of the clusters the main two features that di erentiate them. Usually expressed in terms of the [Fe/H] abundance, the metallicity of a globular cluster around -0.5 places that cluster within the metal-rich clusters (MRGC) and clusters with values below -1 are the metal-poor ones (MPGC) [Harris 1999].
Programa Académico : Maestría en Física
Grupo de INV. : Grupo de Fisica y Astrofisica Computacional (FACOM)
URI : http://hdl.handle.net/10495/11256
Aparece en las colecciones: Maestrías en Ciencias Exactas y Naturales

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