5 Apr 2017

Announcement
Date: February 6-9, 2018
Place: National Tsing Hua University, Hsinchu, Taiwan

Whether magnetic fields or turbulence play a critical role in the star formation processes has been one of the most important unresolved questions in star formation. Classical low mass star formation theory claims that ambipolar diffusion is essential to remove magnetic flux for gravitational collapse; however, many MHD simulations shows that molecular clouds can fragment and form stars under the influence of turbulence without much assistance from the magnetic fields. Since ALMA has started to offer us unprecedented sensitive polarization measurements, we may finally have data good enough to answer this question. On the other hand, more and more dust polarization observations at disk scales reveal that scattering cannot be ignored which would challenge the reliability of the magnetic field measurement but also could provide critical information on dust growths for the formation of planetesimals.

We hope that this conference offers an opportunity to facilitate the discussions on all aspects of star and planetary disk formation, such as
1. Magnetic field and turbulence measurements
2. Molecular cloud structure and dynamics
3. Formation of protoplanetary disks
4. Chemical contents of molecular cores and disks
5. Star formation efficiency