Context. Planetary studies demand precise and accurate stellar parameters as input for inferring the planetary properties. Different methods often provide different results that could lead to biases in the planetary parameters. Aims: In this work, we present a refinement of the spectral synthesis technique designed to treat fast rotating stars

The data used in the publication consist of a set of CaII H spectra taken near and beyond the solar limb on 25/08/2009 at UT 08:43-09:15. The data were obtained with the POLIS instrument at the German VTT. The wavelength range covers the core and the blue wing of the CaII H line from 396.332nm to 396.969nm in 326 steps of 1.96pm. The observations

Spicules of the so-called type II were suggested to be relevant for coronal heating because of their ubiquity on the solar surface and their eventual extension into the corona. We investigate whether solar spicules are heated to transition-region or coronal temperatures and reach coronal heights ({≫} 6 Mm) using multiwavelength observations of limb

We present optical and near-infrared spectroscopy (600-1000 nm) of eight faint (I > 18) very red (R - I > 2.2) objects discovered in a recent deep CCD survey of the Pleiades cluster by ZapateroOsorio, Rebolo, & Martin. We compare them with reliable cluster members like PP1 15 and Teide 1, and with several field very late type dwarfs (M4-M9.5)

We have started a near-infrared spectroscopic study of the Veritas asteroid family. This family is of particular interest for several reasons: 1) This 8.2 million-year-old family contains fresh fragments of a primitive parent body (Nesvorney et al., 2005). 2) Interplanetary dust from the Veritas collision makes up over 25% of interplanetary dust

The measurements reported were made during a flight to an altitude of 40 km, on Mar. 13, 1974. A polarizing Michelson interferometer cooled, by a liquid helium bath, to a temperature of 1.4 K was used in the measurements. One hour of useful time was achieved at float altitude. The fitted spectrum obtained is shown in a graph. The measured spectrum