Zoom info: https://stanford.zoom.us/j/98604058568

Shinnaga: While significant progress has been made in theoretical studies of star formation, the mass that stars acquire from their precursor cores remains a key unsolved problem. The initial stellar mass function (IMF) determines the evolution of the universe.  Since stars form from the core, the core mass function (CMF) is expected to be the origin of the stellar IMF. For this to be true, there must be a correlation between the mass of the core and the mass of the star to be born, i.e., the star formation efficiency must be nearly constant within a specific range, which is not obvious. In order to investigate this, it is necessary to answer the questions, "How much mass does a star acquire from the core?" and "Can the history of the antagonism between the gravitational and magnetic forces (mass-to-flux ratio) of the core explain the acquired mass of the star?"  In this study, we aim to reveal the three-dimensional spatial distribution of magnetic field lines by directly detecting and measuring the Zeeman effect of atomic and molecular lines, tracing multiple different density regions using state-of-the-art radio observation techniques. Combined with the latest 3D theoretical simulations, this novel approach will potentially revolutionize our understanding of star formation and the universe.

Glombitza: TBD