Wavelength flux Spectral energy distributions of bright stars can be used to derive effective temperatures Ay 123 Lecture I - Physical Properties.

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Presentation transcript:

wavelength flux Spectral energy distributions of bright stars can be used to derive effective temperatures Ay 123 Lecture I - Physical Properties

Wavelength(  m) flux T eff Model atmospheres of varying [T eff, g] used to fit data

Stellar Spectral Energy Distributions Wavelength(Å) flux

Spectral Classification Diagnostic spectral lines act as independent measures of temperature in stellar atmosphere provided surface gravity is known

Stellar Spectra: Giants vs Dwarfs G K Stars are a 2-D sequence! Giants are slightly cooler than dwarfs of a similar spectral class with redder continua. This is because line strengths depend on T eff and g

Luminosity Classes

Overview of Stellar Evolution on H-R Diagram

Evolution During the Main Sequence Zero Age MS

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