Central line wavelengths in the spectrum of the Sun observed at the centre of the disc, and in the flux spectrum, line identification and solar log(gf). (1 data file).

In non-equilibrium plasma spectroscopy it may happen to have to deal with ensembles of particles, whose velocity distribution is not the equilibrium (i.e. Maxwell) one. Consequently, the shape-profile-of the relevant emission or absorption coefficient is different from the profile (Gauss or Voigt) that corresponds to the equilibrium velocity

During magnetopause crossings, the AMPTE CCE satellite frequently observed flux transfer events (FTEs) characterized by fluctuations in the magnetic field strength (B) and bipolar signatures in the field component (BN) normal to the nominal magnetopause. In this study, we survey 110 events observed from October to December 1984 and during January

The complete set of data from the Tenerife 10-GHz (8-deg FWHM) twin-horn, drift scan experiment is described. These data are affected by both long-term atmospheric baseline drifts and short-term noise. A new maximum entropy procedure, utilizing the time invariance and spatial continuity of the astronomical signal, is used to achieve a clean

It is well-established that velocities in the immediate surroundings of solar magnetic elements produce an asymmetry in the Stokes V profiles emerging from the magnetic feature. Conversely, the observed Stokes V asymmetry can be used to infer the velocity field. Taking as constraints the area asymmetries of the Stokes V profiles of two lines of

We checked the change of the effective temperature with the atmospherical pulsation of rho Cas from combined analyses of optical spectra of 1993-95 and IUE spectra of 1979-81. We find an upper range for bigtriangleup T_eff =~ 750 K over a period of 16-17 months. We present a thorough study of the related absorption line profile changes from which a