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Il futuro degli studi exoplanetari e’ chiaramente focalizzato attorno ad osservazioni nell’ottico e nel vicino Infrarosso. Tuttavia l’eventuale realizzazione di una grande missione per astronomia X con un telescopio focalizzante con area efficace di almeno 2 sq. m. pone la questione se nel campo degli studi esoplanetari ci sia una qualche interessante spazio per le osservazioni in raggi X. Sulla

High-energy observations of gamma-ray bursts (GRBs) with the Fermi satellite have enabled detailed studies of the temporal and spectral behaviour over seven decades in energy (from 8 keV to ~100 GeV) and provided new insight into the emission mechanisms of these powerful outbursts. I will briefly outline some highlights from Fermi GRBs observations, along with their possible implications. Key observational

Impacts of falling fragments observed after the eruption of a filament in a solar flare on June 7, 2011 are similar to those inferred for accretion flows on young stellar objects. As imaged in the UV/EUV by the Atmospheric Imaging Assembly on-board the Solar Dynamics Observatory, many impacts of dark, dense matter display uncommonly intense, compact brightenings. High-resolution hydrodynamic simulations

I present broad-band (350-2500nm) mid-resolution X-Shooter/VLT spectra of three accreting young stellar objects with spectral types between M5 and M8, i.e. near or within the brown dwarf regime. These observations provide a rich database of accretion diagnostics from the Br$\gamma$ and Pa$\beta$ lines in the near-IR to the Balmer jump in the UV including the full optical band with the

The Hi-C (High resolution Coronal imager) sounding rocket has provided the highest resolution EUV solar coronal images ever obtained, resolving structures down to ~0.3 arcsec. The unprecedented spatial and temporal resolution of Hi-C data has revealed several new features, including highly braided coronal loops undergoing reconnection, and very rapid variability (down to ~15s) in the moss of bright hot loops.

X-ray sources with very few counts can be identified with low-noise in X-ray detectors, especially for the Advanced CCD Imaging Spectrometer (ACIS-I) camera on board the Chandra X-ray Observatory. Most of these studies concerns to the large populations of faint X-ray sources associated with pre- main sequence stars (PMS). Several of these sources seems to be faint enough for parametric