Physics of Stars and Nebulae (U01367)

? Credit Points : 10 ? SCQF Level : 9 ? Acronym : PHY-3-StarNeb

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

? Pre-requisites : Physics 2B: Waves, Quantum Physics and Materials (PHY-2-B); Foundations of Mathematical Physics (PHY-2-FoMP) or Principles of Mathematical Physics (PHY-2-PoMP).

Variants

? This course has variants for part year visiting students, as follows

Physics of Stars and Nebulae (VS1) (Semester 1 (Blocks 1-2))

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

First Class Information

Date	Start	End	Room	Area	Additional Information
20/09/2005	12:00	13:00			ROE LECTURE THEATRE

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 a student will be able to:
1)describe the physics which determines the interior structure of stars, apply hydrostatic equilibrium and radiative diffusion equations to estimate various physical conditions and time scales in stellar interiors
2)state the energy production source of stars and describe the overall physical process
3)describe how the energy produced at the centre of stars is transported, and how this is related to the convective instability in stellar interiors
4)describe color-magnitude diagram of Main-sequence stars, based on the physics governing the stellar structure
5)derive the equation of state in degenerate gas, describe the degeneracy pressure in white dwarfs and neutron stars and how these stars are supported, and explain Chandrasekhar limit for the mass of these stars
6)explain the photoionization equilibrium in interstellar media around hot stars, apply it to estimate the Stromgren radius, and describe how temperature and density are measured in these regions
7)describe the fluid dynamics equations for interstellar medium, derive the sound speed and jump conditions for shock waves
8)state the definition of the equatorial coordinate system and local siderial time, and explain where and when to undertake observations of a star or any given astronomical objects
9)calculate and correct for the damage on light from both interstellar dust and the earth's atmosphere
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