S21A0039
S21A0039
Understanding the mechanisms for mass accretion and jet ejection is one of the key issues for star formation theories. However, observational studies are hampered by the limited angular resolutions of current telescopes, which are not sufficient to resolve the structure and kinematics in the jet launching region. We are therefore pursuing an alternative approach to tackle this important issue: long-term monitoring of mass accretion and jet ejection for active young stars. Our observations since 2010 include IFU imaging spectroscopy of extended jets in [Fe II] 1.64-micron emission (Gemini-NIFS etc.); optical high-resolution spectroscopy to observe gas kinematics very close to the star (CFHT-ESPaDOnS etc.); and optical photometry to monitor changes in mass accretion rates with high time resolution. The results so far suggest that the jet-launching region is very close to the star, and associated with the stellar magnetic field. We need to observe the jets for another few years to confirm or reject this scenario. To continue and complete our study, we request use of Keck-OSIRIS, which will offer a unique opportunity for our observations during the forthcoming autumn-winter period.
This document was translated from LATEX by HEVEA.