Lecture

Passage of Particles Through Matter

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In course

PHYS-400: Selected topics in nuclear and particle physics

This course presents the physical principles and the recent research developments on three topics of particle and nuclear physics: the physics of neutrinos, dark matter, and plasmas of quarks and gluons. An emphasis is given on experimental aspects in thes ...

Description

This lecture covers the passage of particles through matter, focusing on the LPM effect at high energies, muon energy loss, and radiative processes. It discusses the energy loss mechanisms for muons and pions in materials like iron, emphasizing the importance of radiative effects. The lecture also explains the average rate of muon energy loss and the contributions to energy loss by different processes. Additionally, it explores selected topics in nuclear and particle physics, such as solar neutrino mixing parameters and evidence for atmospheric neutrino oscillations.

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Instructor

Frédéric Blanc

Expertise High Energy Physics Teaching & PhD PhD Students Rita De Sousa Ataíde Da Silva, Dimitrios Kaminaris, Maria Carolina Feliciano Faria Past EPFL PhD Students Lino Ferreira Lopes, Vladimir Macko, Guillaume Max Pietrzyk Past EPFL PhD Students as codirector Jessica Prisciandaro, Giovanni Veneziano, Sebastiana Gianì, Lino Ferreira Lopes, Guillaume Max Pietrzyk Courses Selected topics in nuclear and particle physics PHYS-400 This course presents the physical principles and the recent rese

Official source

Ontological neighbourhood

Physics

Particle physics: Standard Model

Related concepts (32)

Solar neutrino problem

The solar neutrino problem concerned a large discrepancy between the flux of solar neutrinos as predicted from the Sun's luminosity and as measured directly. The discrepancy was first observed in the mid-1960s and was resolved around 2002. The flux of neutrinos at Earth is several tens of billions per square centimetre per second, mostly from the Sun's core. They are nevertheless hard to detect, because they interact very weakly with matter, traversing the whole Earth.

Neutrino oscillation

Neutrino oscillation is a quantum mechanical phenomenon in which a neutrino created with a specific lepton family number ("lepton flavor": electron, muon, or tau) can later be measured to have a different lepton family number. The probability of measuring a particular flavor for a neutrino varies between three known states, as it propagates through space. First predicted by Bruno Pontecorvo in 1957, neutrino oscillation has since been observed by a multitude of experiments in several different contexts.

Neutrino

A neutrino (njuːˈtriːnoʊ ; denoted by the Greek letter ν) is a fermion (an elementary particle with spin of 1 /2) that interacts only via the weak interaction and gravity. The neutrino is so named because it is electrically neutral and because its rest mass is so small (-ino) that it was long thought to be zero. The rest mass of the neutrino is much smaller than that of the other known elementary particles excluding massless particles.

Neutrino detector

A neutrino detector is a physics apparatus which is designed to study neutrinos. Because neutrinos only weakly interact with other particles of matter, neutrino detectors must be very large to detect a significant number of neutrinos. Neutrino detectors are often built underground, to isolate the detector from cosmic rays and other background radiation. The field of neutrino astronomy is still very much in its infancy – the only confirmed extraterrestrial sources are the Sun and the supernova 1987A in the nearby Large Magellanic Cloud.

Neutrino astronomy

Neutrino astronomy is the branch of astronomy that observes astronomical objects with neutrino detectors in special observatories. Neutrinos are created as a result of certain types of radioactive decay, nuclear reactions such as those that take place in the Sun or high energy astrophysical phenomena, in nuclear reactors, or when cosmic rays hit atoms in the atmosphere. Neutrinos rarely interact with matter, meaning that it is unlikely for them to scatter along their trajectory, unlike photons.

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