Abstract
A high resolution spectrogram of the Mg b2 line from the quiet Sun disc centre is subjected to a coherence analysis. We find that the coherence between intensity fluctuations in the continuum and the wings of the line breaks down at a distance Δλ = 0.35 A from line centre. From this and the r.m.s. intensity contrast as a function of Δλ we are led to the following simple model of temperature fluctuation δT in the solar photosphere: A lower part (below 50 km, or τ5000 > 0.25) with strongly inward increasing δT and an upper part (above 50 km) with constant δT = 75 K. The two parts are supposed to fluctuate incoherently.
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