We are happy to announce the third annual session of the 3rd Summer School and Internship Programme at CTP organized by the Centre for Theoretical Physics (CTP) at The British University in Egypt (BUE). This is a pedagogical scheme aimed at advanced undergraduate and beginning postgraduate students in physics, mathematics, or engineering. It allows highly motivated potential researchers to attend short courses on scientific topics not widely taught or researched in Egypt; such as general relativity and cosmology, quantum field theory and black hole physics. Among our motivations is to provide a taste of active research areas in fundamental physics and astrophysics; to familiarize students with topical problems and proposed solutions. This year's programme will include a more thorough discussion of currently topical issues in galaxy formation, as well as an introduction to machine learning, with applications to high energy physics, and to the fundamentals of quantum computing. As was the case last year, we expect to have lectures on the standard model of particle physics and the search for physics beyond it. In addition, as in past two years, there will be student projects, which will include training with numerical computation and symbolic manipulation packages (such as GRTensor). The courses are listed as follows:
Self-gravitating N-body systems are ubiquitous in astrophysics, as a first approximation to everything from small star clusters to superclusters of galaxies. Except for the most compact objects, and the largest scales approaching the cosmological horizon, the Newtonian approximation is adequate. Nevertheless, Newton himself famously noted that, beyond N= 2 bodies, the N-body problem gave him a headache. From a modern point of view the pain partly comes from the fact that systems are not ‘integrable’, in the sense o being solvable in terms of symmetry principles (leading to enough conserved quantities as degrees of freedom). The ‘chaotic’ nature of the problem makes it difficult to tackle, and tricky to understand the meaning of it numerical simulation, due to the associated information loss. In this project (s) we investigate the divergence of various dynamical quantities (in 6-N phase space and in energy and angular momentum space) of neighbouring N-body trajectories when significant softening is present. Goals are to study effects of variation of: [1] Particle numbers and find optimal softening that minimizes divergence, [2] Numerical (ir)reversibility of (exactly reversible) trajectories, [3] In-out of (dynamical) equilibrium initial conditions (optional).
In this project we are going to test different alternative models to the standard model of cosmology – ΛCDM - as possible solutions to problems that it faces, e.g., 𝐻0 and 𝜎8 tensions. We will use Bayesian inference (or likelihood analysis) to test these models against different cosmological datasets (Supernovae, cosmic microwave background etc...). Required skills: Basic Knowledge of cosmology (at the level of the book Introduction to Cosmology by Andrew Liddle or Amr El-Zant’s lectures). Intermediate knowledge of Python; Basic knowledge of Linux.
General Relativity is the most successful theory describing gravity so far. The theory encodes the gravitational field as a curvature of spacetime. It has many applications in astrophysics and cosmology. Indeed, these applications intersect with general area of differential geometry, which needs some basic knowledge of tensor calculus. Fortunately, the GRTensor II package provides an easy tool to calculate tensor components on curved spacetimes, specified in terms of a given metric. The package contains a library of standard definitions designed for use in the field of general relativity. GRTensor II is not a standalone package, but requires an algebraic engine (originally developed to run with different versions of Maple). A limited version has been designed to run with Mathematica. GRTensor II and related software and documentation are distributed free of charge, please visit the URL http://grtensor.phy.queensu.ca/ and download the Maple version of GRTensor II. For more details about the package installation see the documentation link in the aforementioned URL. Three group projects will be offered during the programme, each consisting of two to three members: Project I: Schwarzschild metric, which describes the geometry of a spherically symmetric spacetime configuration. The general relativistic solution of an empty space is suitable for solar system applications. Project II: Kerr metric, which describes the geometry of an axially symmetric spacetime configuration. The general relativistic solution of an empty space is suitable for rotating black hole applications. Project III: Friedmann–Lemaître–Robertson–Walker (FLRW) metric, which describes the geometry of a homogeneous and isotropic spacetime configuration. The general relativistic solution is suitable for cosmological applications.
The resistive plate chamber (RPC) is a fast gaseous detector, which consists of two parallel plates; a positively charged anode and a negatively charged cathode, both made of a very high resistivity plastic material and separated by a gas volume. It is used in many high-energy physics experiments due to its simple design, construction, good time resolution, high efficiency, and low-cost production. This project aims to find the ideal operating conditions of the CMS RPCs using Garfield++ as simulation software. It represents the effect of temperature on various RPC parameters. The electron transport parameters like drift velocity, Townsend coefficient and Diffusion coefficient have been computed under different temperatures and gas mixtures using MAGBOLTZ. While the primary ionization number and energy loss have been studied using HEED. We used the nearly exact Boundary Element Method (neBEM) solver in the calculation of the weighting field and electric field. Finally, we applied Ramo’s theorem to calculate the induced signal.
Garfield is a computer program for the detailed simulation of two and three- dimensional drift chambers. It has an interface to the Magboltz program for the computation of electron transport properties in arbitrary gas mixtures. Garfield also has an interface with the Heed program to simulate the ionization of gas molecules by particles traversing the chamber. Transport of particles, including diffusion, avalanches, and current induction is treated in three dimensions irrespective of the technique used to compute the fields. In this work, we use Garfield to calculate the transport parameters like drift velocity, longitudinal diffusion, transverse diffusion Townsend coefficient attachment coefficient, and Lorentz angle.
The standard model (SM) of particle physics is a very successful model for describing the interactions between the elementary particles (leptons and quarks) and between the elementary particles and the gauge bosons (W+, W- and Z) in the 80's at LEP experiment at CERN, which appears as a consequence of the unification between the electromagnetic force and the nuclear weak force. In 2012, both CMS and ATLAS experiments at CERN discovered the SM Higgs boson, which was the last block in the SM. Higgs boson plays important role in our understanding of mass determination of the elementary particles (from Yukawa interaction), and how the gauge bosons acquire masses via Higgs mechanizem. These processes have been produced at the LHC via quark - antiquark Annihilation process in proton-proton collision at 13 TeV. Work plan: performing MC simulation for the production of the SM gauge bosons (W+, W- and Z) via their leptonic decays using Madgraph package. Pre-requested: knowledge of C++, Madgraph and ROOT analysis framework. Needed packages: [1] Madgraph version MG5_aMC_v3_5_0 from https://launchpad.net/mg5amcnlo , [2] Delphes version Delphes-3.5.0 from wget http://cp3.irmp.ucl.ac.be/downloads/Delphes-3.5.0.tar.gz. Please noticed that Madgraph+Pythia8+Delphes can be downloaded together if you follow the instructions given in https://twiki.cern.ch/twiki/bin/view/CMSPublic/MadgraphTutorial.
Ahmed Hammad [PPTX I , II , III , IV , V , VI], [Tutorials] | Amr El-Zant [PPTX I], [PPTX II] | Sayed Lashin [PDF I , II , III] | Ahmed Moursy [PDF I & II] | Waleed Abdallah [PDF] |