Abstract
ABSTRACT The detailed knowledge of solar convection now available is used to evaluate the possibility of deriving some of the surface convection parameters of other stars from line-profile measurements. A theory is outlined for computing integrated line profiles with convection, rotation, and limb darkening. This theory is employed to calculate line profiles for rotating convecting stars of the solar class for values of equatorial v sin i ranging from 0 to 10 km/s. Fourier sine transforms for solar-class stars are examined, and applications to stars not of the solar class are discussed. Several possible sources of line asymmetry are identified.
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