Spectroscopic analysis of the light coming from an atmosphere is a powerful tool for revealing its properties. The problem when using conventional spectroscopy for solar fluxtubes is their unresolved character: magnetic and non-magnetic regions of a plage have to be observed as a whole. With the aim of obtaining the true intensity spectrum of an

A method is presented for reconstructing the intensity profile, I, formed in the magnetic elements which have diameters smaller than the best presently achievable spatial resolution. It follows the same line as in Solanki and Stenflo (1984). As a starting point I and V of the facula and the I observed in the quiet sun are used. The filling factor

Binary models of symbiotic stars are discussed, analyzing the results of recent IR observations. It is indicated that a binary must have component masses of about 1 solar mass and a period greater than 100 days to exhibit a symbiotic spectrum, and a number of combinations of hot and cool components which would satisfy these criteria are considered

The authors present accurate positions and near infrared photometry of 11 point-like objects in the neighbourhood of GGD objects.

High resolution high signal-to-noise spectral profiles of the 8498 and 8542 Å lines of the Ca II infrared triplet (IRT) have been obtained for a sample of quiescent and active dwarfs from spectral types F8 to K5. Line core intensity indices are related to the stellar spectral type, effective temperature, gravity and rotation. The Ca II IRT spectra

The following are the main findings: (1) Fragments with typically 1021Mx preserve their identity and even survive to the decay of the sunspots. (2) Each fragment has a very precise location in the whole ensemble. (3) The incomplete coalescense of the fragments leaves interstices which are penetrated by hot gas. This gives a natural explanation of