Course syllabus adopted 2019-02-14 by Head of Programme (or corresponding).
Overview
- Swedish nameDet interstellära mediet och stjärnbildning
- CodeRRY041
- Credits7.5 Credits
- OwnerMPPHS
- Education cycleSecond-cycle
- Main field of studyElectrical Engineering, Engineering Physics
- DepartmentSPACE, EARTH AND ENVIRONMENT
- GradingTH - Pass with distinction (5), Pass with credit (4), Pass (3), Fail
Course round 1
- Teaching language English
- Application code 85129
- Block schedule
- Open for exchange studentsYes
Credit distribution
Module | Sp1 | Sp2 | Sp3 | Sp4 | Summer | Not Sp | Examination dates |
|---|---|---|---|---|---|---|---|
| 0115 Written and oral assignments 1.5 c Grading: UG | 1.5 c | ||||||
| 0215 Examination 6 c Grading: TH | 6 c |
|
In programmes
Examiner
Jonathan Tan- Full Professor, Space, Earth and Environment
Eligibility
General entry requirements for Master's level (second cycle)Applicants enrolled in a programme at Chalmers where the course is included in the study programme are exempted from fulfilling the requirements above.
Specific entry requirements
English 6 (or by other approved means with the equivalent proficiency level)Applicants enrolled in a programme at Chalmers where the course is included in the study programme are exempted from fulfilling the requirements above.
Course specific prerequisites
It is desired that the students will have done a basic introduction to astronomy. Students also need basic knowledge about electromagnetic waves and spectroscopy/quantum physics.Aim
The aim of the course is to provide the students with a description of our current knowledge about the physics of the interstellar medium and the processes by which stars form.Learning outcomes (after completion of the course the student should be able to)
- Describe observations of the interstellar medium in different parts of the electromagnetic spectrum- Explain how physical concepts are used to understand the various forms of interstellar matter
- Describe the current theory for the formation of stars and some of its observational tests
- List the ISM recycling, depletion and destruction time scales.
- Calculate the ionization structure of and emission from an HII region.
- Calculate the idealized interaction between SN and ISM.
- Determine the average electron density and magnetic field in the Galaxy from pulsar observations.
- Describe the role of dust in the interstellar medium and calculate its effect on observations.
- Discuss the most important heating and cooling mechanisms of the different ISM phases.
- Use the virial theorem
- Discuss the effect of radiation pressure during star formation
Content
The course covers the following items:Overview of interstellar matter across the electromagnetic spectrum
Photoionized nebulae
Nebular modelling, including computer models
Multi-phase interstellar medium. Gas and dust content of the Galaxy
Molecular clouds: physics of H2 and CO molecules, interstellar chemistry
Initial conditions for the formation of stars
Formation of stars: Protostellar collapse, formation of disks, outflows of protostars and young stellar objects
Shocks