We describe the Long Wavelength Array (LWA), a ground-based radio interferometer capable of serving as a coronal mass ejection (CME) detector. Previous low-frequency (nu 50 MHz) coronal sounding experiments have shown that CMEs exhibit large radar cross sections. The LWA will serve as the imaging receiver for a bi-static radar observatory that

We determine the intrinsic phase lag of the GOLF data for the solar p-mode velocity deduced either from one of the narrow band photometers working alternatively on blue and red wing of the sodium lines. The timing of the ``blue wing'' velocity coming from the current GOLF data is given in respect to the ground-based observations. The phase lag for

An analysis of a new and extensive set of spectroscopic observations of the early-type binary system {AR Cas} , based also on spectral disentangling, has led to the discovery of the spectrum of the secondary star and of line-profile variations of the B4V primary star. A revised spectroscopic orbit based on these and published data is presented. We

We present time-resolved optical spectroscopy of the cataclysmic variable S193. The emission lines are remarkably similar to those of V795 Her and exhibit high-velocity S-waves and complex absorptions that are modulated with the orbital period. Evidence for transient anomalous spectral features is seen during the first two nights of our run. We

Since the 1960s, ground-based radio astronomers have had the capability to image solar radio emissions using aperture synthesis techniques. These images show the two-dimensional time history of CME-driven shock fronts, for example. However, ground-based observations are limited by the terrestrial ionosphere to frequencies above about 15 MHz, which

We have measured the equivalent width WK of the K i resonance line at 7699 Angstroms for a large sample of low activity late-type stars observed with high spectral resolution and we have verified that the relation WK vs. Teff is monotonically decreasing, for both dwarf and giant stars. This behaviour is different from that of the Na I D lines for