We study X-ray fluorescent emission and monochromatic scattering from the surfaces of asteroids and other atmosphereless solar-system objects using numerical Monte Carlo simulations. X-ray observations allow the assessment of the elemental composition and structure of the surface. We assume that the model regolith consists of close-packed spherical

Velocity oscillations measured simultaneously at the photosphere and the chromosphere of different solar magnetic features (sunspots, pores and facular regions) allow us to study the properties of wave propagation as a function of the magnetic flux of the structure. While photospheric oscillations are similar everywhere, oscillations measured at

New tools have been developed for THEMIS spectropolarimetric data. In this paper we present how these tools work and can be used in order to understand two interesting observed phenomena: a moving magnetic feature and an ephemeral region.

We analyse SAURON kinematic maps of the inner kpc of the early-type (Sa) barred spiral galaxy NGC 5448. The observed morphology and kinematics of the emission-line gas is patchy and perturbed, indicating clear departures from circular motion. The kinematics of the stars is more regular, and displays a small inner disk-like system embedded in a

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Recent XMM-Newton and Chandra observations have revealed that Jupiter's X-ray emission comprises both, thermal and non-thermal spectral components. While the emission from the low-latitude planetary disk has the properties of scattered solar X-rays, with a thermal spectrum and typical coronal emission lines, the auroral soft ( 2 keV) X-rays are