About 150 weakly magnetic neutron stars are known to accrete matter from low-mass stars in neutron star low-mass X-ray binaries (NS-LMXBs). Accretion in these systems is not steady and as a consequence luminosity and spectral shape change on timescales from milliseconds to months. Energy spectrum and rapid variability vary in a correlated way

In this work we present the results of a systematic search for diffuse bands (DBs, hereafter) in the circumstellar envelopes of a carefully selected sample of post-AGB stars. We concentrated on analyzing 9 of the DBs most commonly found in the interstellar medium. The strength of these features is determined using high-resolution optical

We propose a systematic study of all observations of black hole and neutron star low-mass X-ray binaries (LMXBs) in the Spitzer archive. At least 125 unique LMXBs have now been observed with Spitzer, many as part of large Legacy surveys of the Galactic plane and bulge. This LMXB archive has remained largely unexplored. The proposed archival study

Our primary goal is to characterize the surface composition (and other properties such as radius, albedo and thermal inertia) of our sample of Themis-family and Veritas-family asteroids based on their 5 to 14 micron spectra. We chose these two families for several reasons. First, they are compositionally primitive (non-igneous) so they can yield

Aims:I deduced a 3D sunspot model that is in full agreement with spectropolarimetric observations, in order to address the question of a possible penumbral heating process by the repetitive rise of hot flow channels. Methods: I performed inversions of spectropolarimetric data taken simultaneously in infrared (1.5 μm) and visible (630 nm) spectral

We report results from our Spitzer GO-1 program on IRS spectroscopy of a large sample of Luminous Infrared Galaxies and quasars selected from the European Large Area ISO Survey (ELAIS). The selected ELAIS sources have a wide multi-wavelength coverage, including ISOCAM, ISOPHOT, IRAC and MIPS (from SWIRE), and optical photometry. Here we present the