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We present the results of the analysis of a Large Program of deep XMM-Newton observations of SN1006. We focus on the rim of the supernova remnant to derive important constraints for the shock acceleration process and for the back-reaction of the accelerated particles on the evolution of the remnant. The physical properties of the shocked ambient medium are expected to

Hinode and SDO high spatial/temporal/spectral resolution solar observations provide us with accurate diagnostics of solar coronal plasmas (density, temperature, abundances,…). I will discuss some of the limitations of these diagnostics due e.g. to completeness and accuracy of the atomic data (in particular in the narrow passbands of the Atmospheric Imaging Assembly onboard SDO), or to superposition of different structures in

To study the accretion shocks of classical T Tauri stars (CTTS) we obtained high-resolution X-ray spectra of two CTTS, V2129 Oph and V4046 Sgr, to look for phase-resolved X-ray signatures of shock-heated plasma. The 200 ks Chandra/HETGS observation of V2129 Oph (a 1.35 M_sun star, rotating in 6.5 d) covered ~0.5 stellar rotation. The 360 ks XMM/RGS observation of V4046