High energy astrophysics
Learning objectives
Referring to knowledge
The objective of this course is to acquire research training in high-energy astrophysics, from an observational and theoretical point of view. The subjects provides students with basic and updated knowledge to properly prepare them for the subsequent career in research. For those who do not foresee a career in research, the learning gained on this master’s degree will boost their skills and increase their experience, which could be useful in the job market.
To understand the high-energy universe in which we live, first we explain physical mechanisms that can accelerate particles to high energies and radiation processes that lead to astrophysical sources. Then, we study the phenomenology of various kinds of astrophysical high-energy sources, such as supermassive black holes in galactic nuclei, X-ray binary stars, pulsars or supernova remnants. The most recent observational results are presented and the implication is discussed in the available models.
High-energy astrophysics is currently in a golden age due to the results that are being obtained from existing observatories, which represent a unique opportunity to advance in the field of high energies. The following observatories are notable:
— Soft X-ray satellites, such as XMM-Newton or Chandra.
— Hard X-ray satellites, such as INTEGRAL or Swift.
— High-energy gamma-ray satellites, such as Fermi.
— Cherenkov telescopes, such as MAGIC, HESS or VERITAS.
— Neutrino detectors, such as IceCube.
The enormous amount of information that has been gathered by these instruments over years requires professionals to process the data properly and contribute to advances in the physics field.
Teaching blocks
1. 0. Introduction - Messengers from space
* Cosmic rays
Neutrinos
Gravitational waves
Electromagnetic waves
2. 1. Particle acceleration and radiation mechanisms in high energy astrophysics
* 1.1. Particle acceleration mechanisms
1.2. Diffusion
1.3. Energy losses
1.3. Radiative processes
1.3.1. Thermal emission
1.3.2. Synchrotron radiation
1.3.3. Inverse Compton scattering
1.3.4. Bremsstrahlung
1.3.5. Hadronic processes
1.3.6. Particle annihilation
3. 2. Accretion and ejection in relativistic sources
* 2.1. Accretion onto compact objects
2.2. Outflows: jets and winds (general physical description)
2.3. Flow dynamics (production, propagation, content, termination)
2.4. Emission in relativistic outflows: electron-positron pairs
2.5. Emission in relativistic outflows: protons and nuclei
2.6. Radiation reprocessing
4. 3. Phenomenology of accreting sources with outflows
* 3.1. Observational tools (analysis and fundamental diagrams)
3.2. X-ray binary accretion modes
3.3. Disks and jets
3.4. Black holes at all scales: from X-ray binaries to AGNs
5. 4. High-energy gamma-ray sources in the Universe
* 4.1. High-energy gamma-ray detectors and satellites
4.2. Imaging atmospheric Cherenkov telescopes
4.3. Galactic high-energy gamma-ray sources (pulsars, pulsar wind nebulae, supernova remnants, X-ray and gamma-ray binaries, etc.)
4.4. Extragalactic high-energy gamma-ray sources (AGNs, GRBs, EBL, etc.)
4.5. Fundamental physics at high-energy gamma rays (dark matter, Lorentz invariance, etc.)
Teaching methods and general organization
Lecturers explain the topics in the programme with the support of audiovisual material and the Internet among others.
Students are given the material presented in each class in electronic format.
Students must submit an assignment and give an oral presentation, and a written synthesis test to prove the comprehension of the knowledge acquired.
Official assessment of learning outcomes
Students should work on a topic of high energy astrophysics proposed by teachers. The work, which must be presented orally and submitted in writing, allows part of the assessment to be carried out. The assessment is completed with a written synthesis test and taking into account active participation in class. The percentage of the grade for each part is:
- Participation: 20%
- Written synthesis test: 30%
- Written work: 20%
- Oral presentation of the work: 30%
The same system is used for re-evaluation as for evaluation.
Reading and study resources
Check availability in Cercabib
Book
Aharonian, F. A. Very high energy cosmic gamma radiation : crucial window on the extreme universe. Singapore : World Scientific Publishing, cop. 2004. Enllaç
Charles, Philip A. ; Seward, Frederick D. Exploring the X-ray universe. Cambridge : Cambridge University Press, 1995. Enllaç
Longair, M. S. High energy astrophysics. 3rd ed. Cambridge : Cambridge University Press, 2011 Enllaç
Pacholczyk, A. G. Radioastrofísica : procesos no térmicos en fuentes galácticas y extragalácticas. Barcelona : Reverté, DL 1979 Enllaç
Romero, Gustavo E. ; Paredes i Poy, Josep Maria. Introducción a la astrofísica relativista. Barcelona : Publicacions i Edicions Universitat de Barcelona, cop. 2011 Textos docents ; 365
More information at: http://grad.ub.edu/grad3/plae/AccesInformePDInfes?curs=2023&assig=568433&ens=M0D0B&recurs=pladocent&n2=1&idioma=ENG
Presential
FALSE
High energy astrophysics
Funded by the European Union. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or HaDEA. Neither the European Union nor the granting authority can be held responsible for them. The statements made herein do not necessarily have the consent or agreement of the ASTRAIOS Consortium. These represent the opinion and findings of the author(s).
