演講資訊

摘要：

Unlike the formation of Solar-type stars, the formation of massive stars (M>8 Msun) is not yet well understood. For Solar-type protostars, the presence of circumstellar or protoplanetary disks which provide a path for mass accretion onto protostars is well established. However, to date only few cases of young massive stars show the evidence of circumstellar disks which might support the idea that a scaled-up version of low-mass star formation could be applied to young massive stars. To what extend this hypothesis can be applied is still unclear and more observational evidences are required to characterize the physical properties of the disk-like structures around massive stars in order to understand how exactly massive stars gain their masses in the equatorial regions. In this talk, I will present high resolution (sub)millimeter interferometric observations of two massive star-forming regions: AFGL 2591 and S255IR. The data imply that massive stars may form via disk accretion in some relatively isolated star-forming cores. Our studies serve as the basis for the coming Atacama Large Millimeter/submillimeter Array (ALMA) studies of massive star formation at very high angular resolution, which is the only instrument that can resolve the sources with great details and provide hints on how exactly massive stars can be formed.