Wavelength flux Spectral energy distributions of bright stars can be used to derive effective...
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wavelengthflux
Spectral energy distributions of bright stars can be used to derive effective temperatures
Ay 123 Lecture I - Physical Properties
Wavelength(m)
fluxTeff
Model atmospheres of varying [Teff, 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 Teff and g
Luminosity Classes
Overview of Stellar Evolution on H-R Diagram
Evolution During the Main Sequence
Zero Age MS