Stellar Astrophysics
Duration
- One Semester or equivalent
Contact hours
- 150 contact hours - Online
On-campus unit delivery combines face-to-face and digital learning. For Online unit delivery, learning is conducted exclusively online.
2022 teaching periods
Hawthorn HOL Study Period 3 |
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Dates: Results: Last self enrolment: Census: Last withdraw without fail: |
Prerequisites
AST80004 Exploring Stars and the Milky WayAims and objectives
This unit aims to cover the physical processes underlying stellar properties and the principles behind models of stellar evolution.
Unit Learning Outcomes
Students who successfully complete this unit will be able to:
1. Explain the classification schemes of stars, their physical parameters and the importance of the HR diagram
2. Explain and summarise the mechanism of star formation and the evolution of stars from the main sequence through to the RGB and AGB phase
3. Appraise and state the processes and properties of high mass stellar remnants, including supernovae, planetary nebulae, white dwarfs, neutron stars and black holes;
4. Solve mathematical problems related to the physical processes that underlie stellar properties and evolution;
5. Explain and summarise stellar astrophysical concepts in a non-technical manner understandable to the general public
6. Design and create a research project on an astronomy topic, assessing and critiquing current knowledge, using credible sources of astronomical information, data and research articles
Unit information in detail
- Teaching methods, assessment and content.
Teaching methods
Type | Hours per week | Number of Weeks | Total |
Online Contact Directed Online Learning and Independent Learning | 12.5 | 12 | 150 |
TOTAL | 150 hours |
Assessment
Types | Individual or Group task | Weighting | Assesses attainment of these ULOs |
Computer Managed Tests | Individual | 20% | 1,2,3,5 |
Newsgroups | Individual | 30% | 1,2,3,4 |
Project | Individual | 50% | 6 |
Content
• Stellar energy: gravitational contraction versus fusion, stellar nucleosynthesis
• Hydrostatic equilibrium and radiation pressure; equations of stellar structure; stellar atmospheres
• Protostars: cloud collapse, initial mass function, evolutionary tracks and ZAMS
• Main sequence stars: lifetime on the MS
• Evolution off the main sequence: low mass versus high mass stars
• Supernovae: explosive nucleosynthesis, supernovae remnants
• Neutron stars
• Stellar mass black holes
• Pulsating stars: the instability strip, helioseismology
• Binary stars
• Stellar clusters: types of clusters, open clusters and stellar evolution models, globular clusters; colour-magnitude diagrams
Study resources
- References.
References
http://astronomy.swin.edu.au/sao/students/textbooks.xml