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Anisotropic emission of gravitational waves during the coalescence of supermassive black hole binaries can deliver a large “kick” velocity to the new BH (v~103 km/s). N-body simulations predict that, for kick velocities larger than 40% of the galactic escape velocity, the BH may experience long lived (few Gyr) oscillations with amplitudes comparable with the size of the galactic core (~10^2

Nearby star-forming regions are ideal laboratories to study high-energy emission of different stellar populations, from very massive stars to brown dwarfs. NGC 2023 is a reflection nebula situated to the south of the Orion B. In this work, we present a comprehensive study of X-ray emitters in the region of NGC 2023 and its surroundings. We combine optical and infrared

Activity cycles are of major interest to understand the solar physics and the influence of the Sun in the Earth’s climate. The effects of solar activity in the Earth are mainly produced by the high energy photons and particles. The solar coronal cycle varies as much as a factor of 50, as measured in terms of Lx. But there is

La corona solare visibile nelle bande X ed Estremo UltraVioletto (EUV) \`e costituita per lo pi\`u da plasma confinato dal campo magnetico in tubi di flusso curvi e ancorati sulla superficie, gli archi coronali. Sebbene ultimamente i telescopi spaziali solari abbiano portato a notevoli progressi nella conoscenza dei meccanismi che strutturano e riscaldano la corona, il dibattito \`e ancora aperto

Since the past decade, the knowledge of high-energy processes in stars has experienced large advance. However, there are still some issues about physical processes taking place in stars that remain uncertain and need a more accurate study. In particular, to deep into some aspects of X-ray coronal emission, we need new observational methods and/or new instrumentation. An example of it

Accretion processes onto classical T Tauri stars (CTTSs) are believed to generate shocks at the stellar surface due to the impact of supersonic downflowing plasma. Although current models of accretion streams provide a plausible global picture of this process, several aspects are still unclear. For example, the observed X-ray luminosity in accretion shocks is, in general, well below the predicted