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Astronomy 383C  Spring 2009
STELLAR ATMOSPHERES
MWF 11:0012:00 · RLM 15.216B · Unique No. 48580
Professor
RLM 16.236 · (512) 4713404 · email

LEVEL:
BöhmVitense, Introduction to Stellar Astrophysics: Volume 2, Stellar Atmospheres
Mihalas, Stellar Atmospheres
Gray, Observations and Analysis of Stellar Photospheres
Rybicki and Lightman, Radiative Processes in Astrophysics
SYLLABUS
Summary of Observational Data: Motivations for studying stars. Spectral and luminosity classification. Relation of theory and observation.
Elements of Radiative Transfer Theory: Definitions. Emission, absorption, and scattering. Equation of transfer, radiative equilibrium.
Gray Atmospheres: Milne's equation. Twostream and Eddington approximations. Emergent flux and limb darkening.
Local Thermodynamic equilibrium (LTE): Elements of statistical mechanics. Perfect gases and the Saha equation. Conditions for LTE. Depression of the adiabatic gradient in a partial ionization zone.
NonLTE: Rate: Rate equations. Radiative and collisional rates; departure coefficients. Calculation of Einstein coefficients and collision crosssections.
Continuum Opacity: Opacity sources in high, intermediate, and lowtemperature stellar atmospheres.
LTE Continuum model Atmospheres: Basic equations. Numerical solution of transfer equation: (iteration; Kurucz's and Feautrier's methods. Temperaturecorrection procedures.
Results and Comparison With Observations: Absolute energy distributions. The Balmer jump. Sample model atmosphere calculation. Flux distributions for sample model stars. Effect of absorption edges on atmospheric structure, lineblanketing, molecule formation.
Mixing Length Theory: Convection and partial ionization zones. Simple phenomenological models.
Line Spectra: Line absorption profiles. Natural broadening and the Lorentz profile. Doppler broadening and the Voigt profile. Collisional broadening. Stark broadening, Inglis Teller formula.
Line Transfer Problem.: Line transfer equation: pure scattering lines and pure absorption lines. Centertolimb variations. Schuster mechanisms. Curve of growth and abundance determinations. Model atmosphere line calculations. Line blanketing theory, LTE line formation.
Moving Atmospheres: Modeling stellar atmospheres with winds require hydrodynamic NLTE treatment. Development of a firstprinciples approach to the problem. Applications to Hot stars.