Stellar Evolution (VS1) (U02591)

? Credit Points : 10 ? SCQF Level : 10 ? Acronym : PHY-4-VStellEv

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.

Entry Requirements

? This course is only available to part year visiting students.

? This course is a variant of the following course : U01424

? Pre-requisites : Year 3 Astrophysics, including Thermodynamics and Physics of Stars & Nebulae, or equivalent.

Subject Areas

Home subject area

Undergraduate (School of Physics), (School of Physics, Schedule Q)

Delivery Information

? Normal year taken : 4th year

? Delivery Period : Semester 1 (Blocks 1-2)

? Contact Teaching Time : 2 hour(s) per week for 11 weeks

All of the following classes

Type	Day	Start	End	Area
Lecture	Monday	12:10	13:00	Other
Lecture	Thursday	12:10	13:00	Other

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