The Euroconference “The Evolution of Galaxies on Cosmological Timescales” was held in Puerto de la Cruz, Tenerife, Spain between 1998 November 30 and December 5. It brought together two communities of astronomers who normally do not talk sufficiently together: those studying the detailed evolution of nearby galaxies, and those studying the

The interpretation of detailed spectroscopic observations of late‐type stars reveals inconsistencies that are likely due to inadequacies of the underlying hypothesis. The high accuracy of the parallaxes measured by the Hipparcos satellite established a firm reference frame that is used here to test theoretical classical model atmospheres for these

We start from our six absolutely calibrated continuous stellar spectra from 1.2 to 35 μm for K0, K1.5, K3, K5, and M0 giants. These were constructed as far as possible from actual observed spectral fragments taken from the ground, the Kuiper Airborne Observatory, and the IRAS Low Resolution Spectrometer, and all have a common calibration pedigree

We analyze, for the first time, the scaling behavior of the photospheric vertical velocity field. Our analysis is based on data collected by the Italian Panoramic Monocromator (IPM) mounted at the THEMIS telescope at the Spanish ``Observatorio del Teide'' (Tenerife) of the Instituto de Astrofisica de Canarias. We investigate the occurrence of

Magnitude differences between rotating and non-rotating copartners for a grid of models with solar metallicity are tabulated here. The results are expressed in terms of the dimensionless angular velocity w-bar- defined in Eq.(1) of the paper, the angle of inclination i and the atmospheric parameters Te and ge defined in Eqs.(22) and (21)

Using CGS4 on UKIRT, we have obtained 2.00--2.45 mu m infrared spectra of a number of low-mass X-ray binaries including Sco X-1, Sco X-2, and GX13+1. Sco X-1 shows emission lines only, supporting our previous conclusion that the spectral type of the evolved secondary must be earlier than G5. Emission lines are also seen in the spectrum of Sco X-2