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DEGREE REGULATIONS & PROGRAMMES OF STUDY 2013/2014
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DRPS : Course Catalogue : School of Physics and Astronomy : Undergraduate (School of Physics and Astronomy)

Undergraduate Course: Stellar Evolution (PHYS10045)

Course Outline
SchoolSchool of Physics and Astronomy CollegeCollege of Science and Engineering
Course typeStandard AvailabilityAvailable to all students
Credit level (Normal year taken)SCQF Level 10 (Year 4 Undergraduate) Credits10
Home subject areaUndergraduate (School of Physics and Astronomy) Other subject areaNone
Course website WebCT Taught in Gaelic?No
Course descriptionThis 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.
Entry Requirements (not applicable to Visiting Students)
Pre-requisites Students MUST have passed: Thermodynamics (PHYS09021)
Students MUST have passed: Astrophysics 3 (PHYS10072)
Co-requisites
Prohibited Combinations Other requirements At least 80 credit points accrued in courses of SCQF Level 9 or 10 drawn from Schedule Q.
Additional Costs None
Information for Visiting Students
Pre-requisitesNone
Displayed in Visiting Students Prospectus?Yes
Course Delivery Information
Delivery period: 2013/14 Semester 2, Available to all students (SV1) Learn enabled:  Yes Quota:  None
Web Timetable Web Timetable
Course Start Date 13/01/2014
Breakdown of 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 )
Additional Notes
Breakdown of Assessment Methods (Further Info) Written Exam 100 %, Coursework 0 %, Practical Exam 0 %
Exam Information
Exam Diet Paper Name Hours & Minutes
Main Exam Diet S2 (April/May)Stellar Evolution2:00
Summary of Intended 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
Assessment Information
Degree Examination, 100%
Visiting Student Variant Assessment
Degree Examination, 100%
Special Arrangements
None
Additional Information
Academic description Not entered
Syllabus 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
Transferable skills Not entered
Reading list Not entered
Study Abroad Not entered
Study Pattern Not entered
KeywordsStell
Contacts
Course organiserProf Avery Meiksin
Tel: (0131) 668 8355
Email: A.Meiksin@ed.ac.uk
Course secretaryMiss Paula Wilkie
Tel: (0131) 668 8403
Email: Paula.Wilkie@ed.ac.uk
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