- Wel Keuzevak
- Wel Contractonderwijs
- Wel Exchange
- Wel Study Abroad
- Geen Avondonderwijs
- Wel A-la-Carte en Aanschuifonderwijs
- Geen Honours Class
None. The course requires basic knowledge of electromagnetism and special relativity, but these concepts will be briefly reviewed.
Our knowledge of the universe is mainly indirect, mediated by the light we receive on earth from the objects in the sky. Therefore, to understand how objects like planets, stars and galaxies work, we need a physical understanding of how their observed light is produced.
We will define a number of fundamental concepts necessary to unambiguously discuss radiation. This is followed by the introduction of the basic equation of radiative transfer, which describes how radiation changes as it traverses a medium. In the remainder of the course we will keep coming back to this equation. This part will be concluded with a discussion of a few methods to solve the equation of radiative transfer.
Then we take a step back and examine the relation between the concepts introduced earlier. We will find that radiation can only be generated and changed by accelerating electrical charges, and we will deduce several fundamental relations.
This is followed by a discussion of three important mechanisms to produce continuous radiation, i.e., radiation that changes only weakly with wavelength.
All these processes involve freely moving electrons: in an ionized plasma (Bremsstrahlung or free-free emission); in the presence of magnetic fields (cyclotron and synchrotron emission, depending on whether the electrons move non-relativistically or relativistically); and the interaction between relativistic electrons and photons (inverse Compton scattering).
We will conclude the lecture series with the production of radiation at discrete wavelengths, i.e., spectral lines. These processes involve electrons bound to atoms or molecules.
The goal of this course is twofold. First, to comprehend how light interacts with matter and how matter can covert different kinds of energy into light. Second, to learn how to extract from observations physical information about the emitter, like its size, temperature and composition.
See BSc schedules.
Mode of instruction
Lectures and seminars.
Written exam. See Exam schedule.
Lecture notes, additional readings and assignments will be provided. To have access to Blackboard, you need an ULCN account. More information:
- “Radiative Processes in High Energy Astrophysics”, available from the following webpage
- Rybicki and Lightman, Radiative Processes in Astrophysics, Wiley Interscience, ISBN 9780471827597
More information about signing up for your classes at the Faculty of Science can be found here
Exchange and Study Abroad students, please see the Prospective students website for information on how to apply.
For Interest only & Contractual enrollment, please see this website.
For more information, see also the Course website: Radiative Processes.
|Maakt deel uit van||Soort opleiding||Semester||Blok|
|Astronomy: Astronomy Research||Master||1|
|Astronomy: Astronomy and Cosmology||Master||1|
|Astronomy: Astronomy and Instrumentation||Master||1|
|Natuurkunde en Sterrenkunde (dubbele bachelor)||Bachelor||1|
|Natuurkunde en Wiskunde (dubbele bachelor)||Bachelor||1|
|Sterrenkunde en Natuurkunde (dubbele bachelor)||Bachelor||1|
|Sterrenkunde en Wiskunde (dubbele bachelor)||Bachelor||1|