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To use spectral lines for stellar analysis, we need to have some basic understanding of how and why they respond to variations in chemical abundances, temperature, and pressure.Here in Chapter 13 these issues are explored and we learn how to select spectral lines suitable for specific tasks.
In this chapter we bring together some of the techniques of observing and calculating stellar spectra with the aim of measuring the sizes and temperatures of stars.Results are summarized.
Surface gravity is one of the basic parameters of a star.The tools we have to measure a star's gravity are reviewed and examples of their application aregiven.A summary of gravity values is given.
Rotation of stars affects stellar spectra and stellar physics.Spectral lines are broadened and imprinted with the characteristic shape of the rotational velocity distribution, and there may be modulation from spots being carried across the visible hemisphere.Methods for extracting rotation rates from line profiles are discussed in detail.Results are summarized.Rotation circulates material inside stars, mixing chemicals and transporting angular momentum.And rotation couples with convection to generate magnetic fields.The magnetic fields produce many types of activity, including spots and flares and energy for coronae, and they hold on to escaping mass, acting as a magnetic brake on the rotation.We look into how rotation changes with time, with evolutionary stage, and for binaries with tidal interaction.
The black body plays a central role in stellar atmospheres in describing the radiation field within the photosphere.The equation describing the photon distribution is Planck's law.Because the characteristics of black-body radiation are completely determined by the temperature of the black body, it forms a fundamental radiation standard, used to calibrate absolute radiant energy received from stars.