PoS - Proceedings of Science
Volume 342 - Accretion Processes in Cosmic Sources – II (APCS2018) - Accretion Onto Young Stellar Objects and Evolution
High Resolution Observations of Young Stellar Objects with Extreme-AO Systems: Jets, Disks, and Accreting Companions
S. Antoniucci
Full text: pdf
Pre-published on: February 07, 2019
Published on: February 14, 2020
State-of-the-art high-contrast optical and near infrared instruments equipped with Extreme Adaptive Optics (ExAO) systems have recently started to provide high-resolution images of Young Stellar Objects (YSOs) of unprecedented quality, which are revolutionising our view and understanding of the structures around young sources.

Narrow-band ExAO observations of jets from YSOs (the first ones of which were carried out with VLT/SPHERE) are able to resolve for the first time the base of the jets and provide crucial clues to discriminate the jet launching region and mechanism, which is key to evaluate the jet feedback on the disk and eventually on the structure of planetary systems.
High-contrast observations of protoplanetary disks have been hugely successful in providing fundamental insights on the disk structures (spiral arms, gaps, rings). These results, in conjunction with ALMA data, have fostered a great advancement in the development of disk evolution models, which take into account gas and dust interaction with forming planets within the disk.

Most observations with ExAO instruments have focused in particular on the detection of these young planets. A very promising technique to detect actively accreting giant planets still in formation is based on narrow-band imaging in accretion tracers such as \ha. Upcoming ExAO instruments like SHARK-VIS at LBT will be specifically optimised to perform these kind of observations in \ha\ on large samples of YSOs. The final aim is to provide constraints on giant planet formation models and to asses the effects of planetary formation on the evolution of the observed disk structures.
DOI: https://doi.org/10.22323/1.342.0014
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