Jets

Details. Jets and outflows are ubiquitously observed in Young Stellar Objects. The ejection of matter is indeed tightly connected with the accretion process (from the circumstellar disk onto the central star) that characterizes the early phases of a star's life.  Jets are believed to be launched from the innermost regions of the circumstellar disk, through the action of a large-scale magnetic field that is anchored in the rotating star-disk system.  As such, jets can have a major role in extracting the angular momentum from the system and heavily affect the properties of the inner disk region in which planets are going to form. Observing the jet as close as possible to the star is therefore fundamental to directly probe and measure the jet formation region and assess the jet launching mechanism, which will allow us to eventually determine the jet feedback on the disk. However, the regions where the jets are believed to originate have spatial scales spanning from fractions to a few astronomical units. This means that angular resolutions at least better than 70 mas (corresponding to about 10 au at a distance of 150 pc) are required for studying the base of the jets in the closest jet-driving sources of the Taurus-Auriga star-forming region. SHARK-VIS has the potential to achieve these angular resolutions and deliver unprecedented images of the jet formation region in the Hα and [OI] 6300Å lines, which are typical jet tracers. Finally, the analysis of the jet morphology can reveal a wiggling close to the source, which in some cases can be interpreted as an indirect indication of the presence of unseen close-in companions.