Undergraduate Course: Stellar Evolution (PHYS10045)
Course Outline
| School | School of Physics and Astronomy |
College | College of Science and Engineering |
| Credit level (Normal year taken) | SCQF Level 10 (Year 4 Undergraduate) |
Availability | Available to all students |
| SCQF Credits | 10 |
ECTS Credits | 5 |
| Summary | This course investigates particularly the post main sequence stages of stellar evolution. The physical processes involved are applied to the evolution of core and envelope through the red giant phase to the final fate as a Supernova explosion. |
| Course description |
- state the definition of a polytrope and relate it to the structure of stars
- define `homology' and use it to derive the properties of stars on the Main Sequence and during stages of their subsequent evolution
- state the time-dependent virial theorem and apply it to physical situations
- describe the nature of quantum degeneracy pressure and its relevance to stellar evolution
- describe the evolution of stars on the Main Sequence and explain what drives the evolution
- explain the meaning of the Schonberg-Chandrasehkar mass limit and discuss its relevance to stellar evolution
- explain the `mirror principle' and apply it to the relevant stages of stellar evolution
- explain the origin of convective instability and describe its relevance to stellar evolution
- sketch the HR diagram of star clusters of various ages and account for the locus of stars in terms of the evolutionary stages of stars
- describe the role of mass law in stellar evolution, including stars in mass-transfer binaries
- discuss the origin of the Chandrasekhar mass limit and its consequences for stellar evolution
- describe the final stages of stellar evolution
|
Entry Requirements (not applicable to Visiting Students)
| Pre-requisites |
Students MUST have passed:
Thermodynamics (PHYS09021)
Students MUST have passed:
Astrophysics (PHYS10102)
|
Co-requisites | |
| Prohibited Combinations | |
Other requirements | At least 80 credit points accrued in courses of SCQF Level 9 or 10 drawn from Schedule Q. |
Information for Visiting Students
| Pre-requisites | None |
Course Delivery Information
|
| Academic year 2014/15, Available to all students (SV1)
|
Quota: None |
| Course Start |
Semester 2 |
Timetable |
Timetable |
| Learning and Teaching activities (Further Info) |
Total Hours:
100
(
Lecture Hours 22,
Summative Assessment Hours 2,
Revision Session Hours 2,
Programme Level Learning and Teaching Hours 2,
Directed Learning and Independent Learning Hours
72 )
|
| Assessment (Further Info) |
Written Exam
100 %,
Coursework
0 %,
Practical Exam
0 %
|
| Additional Information (Assessment) |
Degree Examination, 100%
Visiting Student Variant Assessment
Degree Examination, 100% |
| Feedback |
Not entered |
| Exam Information |
| Exam Diet |
Paper Name |
Hours & Minutes |
|
| Main Exam Diet S2 (April/May) | Stellar Evolution | 2:00 | |
Learning Outcomes
Upon completion of this course it is intended that a student will be able to:
1) state the definition of a polytrope and relate it to the structure of stars
2) define `homology' and use it to derive the properties of stars on the Main Sequence and during stages of their subsequent evolution
3) state the time-dependent virial theorem and apply it to physical situations
4) describe the nature of quantum degeneracy pressure and its relevance to stellar evolution
5) describe the evolution of stars on the Main Sequence and explain what drives the evolution
6) explain the meaning of the Schonberg-Chandrasehkar mass limit and discuss its relevance to stellar evolution
7) explain the `mirror principle' and apply it to the relevant stages of stellar evolution
8) explain the origin of convective instability and describe its relevance to stellar evolution
9) sketch the HR diagram of star clusters of various ages and account for the locus of stars in terms of the evolutionary stages of stars
10) describe the role of mass law in stellar evolution, including stars in mass-transfer binaries
11) discuss the origin of the Chandrasekhar mass limit and its consequences for stellar evolution
12) describe the final stages of stellar evolution
|
Contacts
| Course organiser | Prof Avery Meiksin
Tel: (0131) 668 8355
Email: A.Meiksin@ed.ac.uk |
Course secretary | Miss Paula Wilkie
Tel: (0131) 668 8403
Email: Paula.Wilkie@ed.ac.uk |
|
© Copyright 2014 The University of Edinburgh - 12 January 2015 4:39 am
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