teaching
 
High School level lectures
¿Qué es una estrella? (I) PDF (1.7 MBytes): estrella_I.pdf ¿Qué es una estrella? (II) PDF (1.8 MBytes): estrella_II.pdf Teaching_files/estrella_I-1.pdfTeaching_files/estrella_II-1.pdfshapeimage_3_link_0shapeimage_3_link_1
Lectures in international schools
I have given these lectures in an event called “Taller de Ciencia para Jóvenes” (in spanish)../MiSitio/Taller_de_Ciencias.htmlshapeimage_5_link_0
These are the lectures I gave in the Guillermo Haro International School: “A Panchromatic View of Clusters of Galaxies and the LSS”, organized by Manolis Plionis, Omar López Cruz & David Hughes, in Tonantzintla, Puebla, on June, 2005.http://www.inaoep.mx/gh2005/shapeimage_6_link_0
Dynamics of Galaxies and Clusters of Galaxies (I) Basic Galactic Dynamics PDF (6.5 MBytes): GHaro05_L1.pdf Dynamics of Galaxies and Clusters of Galaxies (II) The Orbital Structure of Spherical Potentials PDF (6.5 MBytes): GHaro05_L2.pdf Dynamics of Galaxies and Clusters of Galaxies (III) When the Sky Falls: Dynamical Friction and Tidal Force PDF (6.5 MBytes): GHaro05_L3.pdf Dynamics of Galaxies and Clusters of Galaxies (IV) When the Sky Falls: Tidal Heating and Tidal Stripping PDF (6.5 MBytes): GHaro05_L4.pdf Lecture notes To be published in 2007 in Lecture Notes in Physics, Springer. GH05_Aguilar.pdf (1.9 MB) Mathematica Notebook for the 1st lecture GH05_NFW.nb Teaching_files/GHaro05_L1.pdfTeaching_files/GHaro05_L2.pdfTeaching_files/GHaro05_L3.pdfTeaching_files/GHaro05_L4.pdfTeaching_files/GH05_Aguilar.pdfTeaching_files/GH05_NFW.nbshapeimage_7_link_0shapeimage_7_link_1shapeimage_7_link_2shapeimage_7_link_3shapeimage_7_link_4shapeimage_7_link_5
These are the lectures I gave in the Guillermo Haro International School: “International School on Galactic & Cosmological N-Body Simulations”, taught by Luis Aguilar, Lia Athanassoula, Walter Dehnen, Jean Charles Lambert & Peter Teuben, in Tonantzintla, Puebla on July, 2006.http://www.inaoep.mx/~gh2006/shapeimage_8_link_0
The Art of N-Body Simulations Luis Aguilar PDF (1.3 MBytes): GH06_Intro_NBody.pdf Initial Conditions (I) Luis Aguilar PDF (1.2 MBytes): GH06_InitCond1.pdf Initial Conditions (II) Luis Aguilar PDF (1.8 MBytes): GH06_InitCond2.pdfTeaching_files/GH06_Intro_NBody.pdfTeaching_files/GH06_InitCond1.pdfTeaching_files/GH06_InitCond2.pdfshapeimage_9_link_0shapeimage_9_link_1shapeimage_9_link_2
Notes for courses Classical Mechanics (Undergraduate)
Dynamics of Rockets (in spanish) PDF (1.5 MBytes): cohetes_SinSols.pdf Lagrangian Points (in spanish) PDF (0.8 MBytes): Puntos_de_Lagrange.pdf Numerical modeling of the Solar System (in spanish) PDF (0.2 MBytes): BasicEqns.pdfTeaching_files/cohetes_SinSols.pdfTeaching_files/Puntos_de_Lagrange.pdfTeaching_files/BasicEqns-1.pdfshapeimage_12_link_0shapeimage_12_link_1shapeimage_12_link_2
Galactic Dynamics (Graduate)
Oort substitution In 1907, K. Schwarzschild proposed a gaussian distribution to describe the velocities of stars in the Solar neighborhood. In 1913, Charlier generalized it to a triaxial ellipsoid of arbitrary orientation. In a classic study, J. Oort substituted this form for the velocity distribution in the Boltzmann equation in cylindrical coordinates and obtained several results, including an expected rotation curve. Although we now know this is not a good assumption, this is still a very pedagogical exercise about handling the Boltzmann equation. PDF (152 KBytes): sustoort.pdf The Oort formulae for galactic rotation In 1927 J. Oort developed a descriptive model for the differential rotation of the Galaxy. The customary derivation of the Oort formulae for galactic rotation is based in Trigonometry. In these notes we present the usual derivation, but we also present a more modern derivation based in the deformation tensor of a fluid. We show that Oort’s constants are related to the shear and vorticity of the stellar fluid in the Solar neighborhhod. PDF (188 KBytes): notas10.pdf Rotating logarithmic bars Brief note about the dynamics supported by a rotating logarithmic potential. We show orbits in the corotating and inertial frames. PDF (336 KBytes): rotlogbar.pdf The radius of influence of black holes at the center of galaxies In these notes we described the “Lindblad diagram”, which constitutes a complete and unambiguous catalogue of all bound orbits in a non-rotating, arbitrary spherical potential. As an example of its use, we calculate the size of the region in phase space for stars whose orbits take them within the Schwarzschild radius of a massive black hole at the center of a galaxy. PDF (400 KBytes): bholes.pdf Integrals of motion A brief note that shows how the integrals of motion provide a geometric description of regular orbits in phase space. The Kepler potential is used as an example. PDF (260 KBytes): ints_of_motion_notes.pdf Sérsic profiles Recently, the profiles first proposed by José Luis Sérsic to describe the surface brightness profiles of elliptical galaxies, and which are a generalization of deVaucouleurs profiles, have been proposed to describe the mass density profiles of dark halos. In these notes we explore this profile and derive some analytical expressions for some of its most important properties. PDF (340 KBytes): SersicProfiles.pdf Teaching_files/sustoort.pdfTeaching_files/sustoort_1.pdfTeaching_files/notas10.pdfTeaching_files/rotlogbar.pdfTeaching_files/bholes.pdfTeaching_files/ints_of_motion_notes.pdfTeaching_files/SersicProfiles.pdfshapeimage_14_link_0shapeimage_14_link_1shapeimage_14_link_2shapeimage_14_link_3shapeimage_14_link_4shapeimage_14_link_5shapeimage_14_link_6