To provide students with an understanding of the properties of the light  emitted by stars, of the effect of expanding atmospheres and of the  relevance for Supernovae. To enable students to determine the basic phy sical properties of stars  from observational data (e.g. Temp, Radius, Mass, composition) and the  properties of expanding media (stellar winds: velocity, mass-loss rate;  Supernovae: velocity, mass, kinetic energy, nucleosynthesis)

(LO1) The knowledge of how the physical properties of stars and supernovae can be determined from spectroscopic observations.

(LO1) Knowledge of how the physical properties of stars and supernovae can be determined from spectroscopic observations.

(LO2) An understanding of how the interaction between radiation and matter determines the observable properties of stars.

(LO2) An understanding of how the interaction between radiation and matter determines the observable properties of stars.

(LO3) An understanding of how radiation propagates through a medium (a gas) affecting its properties.

(LO3) An understanding of how radiation propagates through a medium (a gas), affecting its properties

(S1) Problem solving skills.

(S1) Problem solving skills

(S2) Analytic skills applied to stellar atmospheres.

(S2) Analytic skills applied to stellar atmospheres

Introduction, clarification of what students are expected to know at the start of the course; Introduction & Observables Herzsprung-Russell diagram. Observables: Luminosity, colour,  temperature. Measurement of stellar parameters (mass, radius,  luminosity) and interrelations.  Transport of energy: Radiation Definition of Radiation quantitites. Optical depth, absorption and  emission. Equation of Transfer. Formal solution. Limb darkening.  Temperature distribution. Grey atmosphere. Main sources of opacity. Atomic Processes Atomic processes relevant for stellar spectra. Interaction of radiation  and matter. Continuum and line processes. Einstein coefficients for  absorption. Oscillator strength. Line profile, broadening. Continuum  absorption. Scattering. Stellar Spectra Excitation, Ionization. Saha-Boltzmann equation. Stellar spectra,  classification. Line Transfer 2-level atom. Milne relations. Curve of Growth. Stellar Winds Radiation Pressure. Mass-loss in hot stars. Diagnostics of winds. Line  formation in expanding atmospheres. Sobolev Approximation. Radiation  transport in moving media. Supernovae Observational classification. Underlying physical mechanisms  (thermonucler explosion, core collapse). Montecarlo radiation transport.  Derivation of SN properties. Application to Cosmology.

Teaching Method 1 - Lecture
Description: Lecture to class on all topics covered in course
Attendance Recorded: Yes

Teaching Method 2 - Tutorial
Description: Weekly tutorials to discuss lecture topics, go over examples, any other questions students might have
Attendance Recorded: Yes
Notes: This activity provides students a chance to test their knowledge and prepare for the final exam

All lecture notes made available from beginning of module via VLE.

All lectures are recorded, and can be streamed by the students via the VLE within 1 day of the lecture.