Im Rahmen der relativistischen Kosmologie wird für den Fall des verschwindenden kosmologischen Gliedes Λ ein strenger Zusammenhang zwischen der bolometrischen Helligkeit und der Rotverschiebung angegeben. Die sich ergebenden Differenzen gegenüber der bisher benutzten Näherung werden berechnet. Es zeigt sich, daß diese Differenzen bei größeren Beträgen der Rotverschiebung nicht mehr zu vernachlässigen sind.

Spectrograms of high spatial resolution taken every 15s reveal rapid variations of the continuum intensity and line width. Variations of the latter seem to be related to Doppler velocity gradients.

Spectral observations of solar velocity fields made during a partial solar eclipse are described. Continuum intensity measurements at the lunar limb allow the modulation transfer function to be derived and the true spatial power spectrum of the velocity field to be reconstructed. The oscillatory and granular components are separated by applying spatial filters cutting off at 3'.'7. The oscillatory component values are in good agreement with those of Canfield (1976) but the granular component has substantially more power and a smaller height gradient. The discrepancy can be resolved by noting the uncertainties of the seeing corrections and of the separation into components in the work of Canfield.However on the basis of this limited material, we would go no further than to claim that the height dependence of the granular velocities remains an open question. C. J. DURRANT ET AL.

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Observations with the French (L.P.S.P.) experiment on board OSO-8 of a sunspot and nearby plage region are described. The behaviour of the emission cores of the Ca II H and K and Mg II h and k resonance lines is very similar and the correspondence in intensity between the four lines persists in all observed features. In contrast, the Lyman lines show little correlation with the other lines. Their emission regions appear broader in the spectroheliograms than the underlying sunspot structure and must not necessarily possess a counterpart in lower layers. From the central intensity of La above the umbra an