Numerical simulations of protostellar jets: on the origin of the high-energy emission

The exploration of the physics of accretion and outflows in young stars is one of the main objectives of theWorld Space Observatory – Ultraviolet (WSO-UV) project. Jets are a fundamental part of the formation and evolution processes of young stars, participating in the loss of mass and angular momentum from the whole system. They are detected in diferent wavelength bands and are ubiquitous at the earliest stages of star formation. However, many questions about the origin and feedback of protostellar jets remain unanswered. In this context, the study of high-energetic phenomena emitting in the extreme ultraviolet (EUV) and X-rays is fundamental as they could have a relevant role in ionizing large parts of the circumstellar environment. In particular, X-ray observations showed evidence of X-ray emitting sources characterized by diferent luminosities and locations within jets. In some cases, the X-ray emitting region is located at the base of the jet close to the star from which the jet originates (e.g. HH 154 and DG Tau jets), while, in other cases, the X-ray source is located further away from the star (e.g. HH 248 jet)..