Two-dimensional simulation of solar granulation: description of technique and comparison with observations

The physical properties of the solar granulation are analyzed on the basis of 2-D fully compressible, radiation-hydrodynamic simulations and the synth etic spectra they produce. The basic physical and numerical treatment of th e problem as well as tests of this treatment are described. The simulations are compared with spatially averaged spectral observations made near disk centre and high resolution spectra recorded near the solar limb. The presen t simulations reproduce a significant number of observed features, both at the centre of the solar disc and near the solar limb. Reproduced observable s include the magnitude of continuum and line-core intensity fluctuations, line bisectors and correlations between different line parameters. Spatiall y averaged line shifts near disc centre, however, are not so well reproduce d, as are individual correlations between line parameters near the solar li mb. Possible causes of these discrepancies are discussed. The present models predict the existence of two photospheric layers at whic h the temperature fluctuations change sign. We point out a diagnostic of th e hitherto undetected upper sign reversal based on high spatial resolution spectral observations of a sample of lines formed over a wide range of heig hts in the photosphere.