Astrophysics 3 (VS1) (U03504)

? Credit Points : 10 ? SCQF Level : 10 ? Acronym : PHY-3-VS1Ap3

Students are introduced to the physics of stars and their influence on their galactic environment. The basic observational properties of stars are reviewed including the HR diagram, followed by a discussion of the physical structure of stars on the Main Sequence to their final states as exotic objects: white dwarfs, neutron stars, and black holes. The interactions of stars with their surroundings are described. Topics covered are HII regions around young stars, stellar winds, and supernova remnants.

Entry Requirements

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

? This course is a variant of the following course : U03212

? Pre-requisites : Year 2 Physics and Mathematics

Subject Areas

Home subject area

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

Delivery Information

? Normal year taken : 3rd year

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

? Contact Teaching Time : 3 hour(s) per week for 11 weeks

All of the following classes

Type	Day	Start	End	Area
Lecture	Tuesday	12:10	13:00	Other
Lecture	Friday	12:10	13:00	Other

? Additional Class Information : Workshop/tutorial sessions, as arranged.

Summary of Intended Learning Outcomes

Upon successful completion of this course, it is intended that the student will be able to :

1) Understand the physics behind the colour-magnitude diagram of stars.
2) Describe the physics of stellar structure, and apply hydrostatic equilibrium and radiative diffusion equations to get physical conditions and timescales.
3) Explain a star's energy production source and process, and describe how energy is transported out of a star.
4) Derive the equation of state of degenerate gas and describe the degeneracy pressure and support of white dwarfs and neutron stars.
5) Explain photoionization equilibrium, estimate the Stromgren radius and describe how the temperature and density of the intergalactic medium are measured.
6) Describe fluid dynamics equations, derive the sound speed and shock jump conditions, and explain the impact of stellar winds and supernovae on the intergalactic medium.
7) Correct for the effect on light of interstellar dust and the earth's atmosphere.