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A parametric model of granulation employing a small number of parameters wasdeveloped. Synthetic spectra calculated using this model closely match observedspectra and, in particular, reproduce the asymmetries observed in spectrallines. Both the microturbulent motions and the large-scale flow velocitydecrease exponentially with a scale height of 368 km as the height within thephotosphere increases. The model agrees with observations of the solargranulation (from which it was derived).  The horizontal motions associated with granulation were found and used tocalculate spectra emergent away from disk centre. These calculated spectra werecompared to observed spectra, with the agreement supporting the accuracy of thegranular model.  Also in the course of this work, the Brueckner-O'Mara damping theory wasfound to predict damping constants accurately. The photospheric abundances of anumber of elements were determined. The abundance obtained for iron agrees withthe meteoric iron abundance. Astrophysical f-values for some lines were alsodetermined.

Solar Line Asymmetries: Modelling the Effect of Granulation on the Solar Spectrum