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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.
Radiant light is what we see from stars.Radiant light carries the energy outward through the star's photosphere.This chapter gives us the terms and vocabulary to describe radiation processes.
If we want the information contained in spectral lines, we have to measure them.How we do this, the equipment and techniques, the role of the instrumental profile and scattered light in degrading the information, and types of information we can extract fill this chapter.
Thechemical composition of stars is a central issue in the study of stellar photospheres.What observations are needed, how are they to be processed, and what is the nature of the results?Other topics include variations in metallicity with location in the galaxy and with time.Thebehavior of lithium with temperature and time is particularly intriguing.