The energy distribution, or how the starlight is distributed in wavelength across wide wavelength spans, depends strongly on the temperature of the star.In the visible spectral region, we see the Paschen continuum and a short portion of the Balmer continuum.How the flux in these regions is measured and calibrated is a central theme of this chapter.We look at both observed and calculated energy distributions with the aim of deriving stellar temperatures and surface gravities, and eventually radii.
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