(Quantum) Field Theory and the Electroweak Standard Model
What is the Standard Model?
Introducing Quantum Fields
Renormalizable or Non-Renormalizable?
Constructing the EW SM
Experimental tests of the EW SM
Issues and Prospects of the EW SM
Lecture I: theory and phenomenology of neutrino oscillations
Lecture II: Neutrino masses and mixing, the phenomenology view
Lecture III: Neutrino masses and mixing: theory Neutrinos in cosmology
Eduardo S. Fraga
QCD under Extreme Conditions
★ First question you should ask: WHY??
‣ Motivation and some disturbing facts
Collective effects x “fundamental” physics
★ Second question you should ask: WHERE??
‣ Accelerator experiments, astro, early universe
My focus: the EoS
★ Third question you should ask: HOW??
‣ Theory, models, etc
★ Effective model building
★ Z(N), the Polyakov loop, and confinement
★ Chiral symmetry breaking
★ Two examples on relevance and difficulties in exploring
the phase diagram
‣ Chiral magnetic effect and the strong CP problem
‣ Drawing the phase diagram
★ Final comments
Motivations for QCD
QCD Lagrangian and Feynman rules
QCD and phenomenology ( e+e- )
‣Renormalization and running coupling
‣Infrared and collinear safety|
Hadrons in the initial state
Naive parton model and Deep Inelastic Scattering
parton evolution and the proton structure functions
colliders are discovery machines
QCD is ubiquitous in hadronic collisions (many tests) and
essential to establish signal and background rates
Higher order corrections for LHC processes
Resummation for specific distributions
Merging, Matching, and both
Flavor physics and cp violation
flavor structure of the standard model
testing the Kobayashi-Maskawa mechanism
test Kobayashi Maskawa mechanism
constraints on new physics
the BSM probes using the mixing
BSM probes using decays
Higgs and flavor
Harrison B. Prosper
Practical Statistics for Particle Physicists
The Frequentist Principle
The Profile Likelihood
Introduction to Bayesian Inference
Introduction to Machine Learning
Beyond the Standard Model
Pastrone LHC Run-2 and Future Prospects
The need of the Large Hadron Collider
The experiments and the enabling technologies
The physics: before LHC and Run1 – a short recap
The ongoing Run2 – what’s new – Standard Model
(SM) – BSM – Flavour physics – Heavy ions
Prospects for near and far future
Jo van den Brand
Andrea De Simone Cosmology and Dark Matter
The Universe around us. Dynamics. Energy Budget.
The Standard Model of Cosmology: the 3
pillars (Expansion, Nucleosynthesis, CMB).
Dark Energy. Dark Matter as a thermal relic.
Searches for WIMPs.
Shortcomings of Big Bang cosmology. Inflation.