Star formation and evolved star research group has focused on observational studies at the mm and sub-mm wavelengths using the domestic facilities such as the TRAO and KVN of KASI and combined VLBI network KVN + VERA (KaVA) and foreign facilities such as the ALMA and JCMT where KASI is participating as a member of East Asian Consortium. Star formation and evolved star research group also leads the KVN Key Science Program (KSP) and KaVA Large Program in the fields of Star formation and evolved stars. The research topics are as follows.

NGC 1333 IRAS 4A: SiO Outflow
VX Sgr : H2O and SiO masers

Star Formation

  • Kinematical and chemical studies on the formation of dense cores and filamentary clouds
  • Magnetic fields in dense cores and filaments
  • Outflows and inward motions in Very Low Luminosity Objects (VeLLOs)
  • Origin of proto-brown dwarfs and their disk formation
  • Study of the structure, physics, and evolution of protostars using radio interferometric imaging
  • Study of the physics and chemistry of infrared dark clouds and massive star-forming regions using radio and infrared observations
  • Study of protostellar collapse and young cluster formation using radio spectroscopy and infrared photometry
  • Statistical study of water and methanol masers in star-forming regions
  • VLBI measurements of the 3D velocity fields of water and methanol masers around high-mass YSOs
  • Studying the physical & chemical properties and magnetic field characteristics of high-mass star-forming regions
  • TRAO Key Science Program: TRAO Observations of Planck cold clumps (TOP) (PI: Tie Liu)
  • TRAO Key Science Program: TRAO multi-beam Survey of Nearby Molecular Clouds (PI: Chang Won Lee)

Evolved Stars

  • Investigating spatial structures and dynamical effects from 43/86/129 GHz SiO maser to 22 GHz H2O maser regions (i.e., atmosphere to circumstellar envelope) according to stellar pulsation through simultaneous time monitoring observations with the KVN single dish, KVN and KaVA VLBI network
  • Studies on correlation and difference of maser properties (spatio-kinematic properties etc) among SiO J=1-0, J=2-1, J=3-2 masers for constraining SiO maser excitation and pumping models
  • Studies on dynamical evolution from AGB to post-AGB stars: Morphology & mechanism, characteristics of SiO and H2O maser properties
  • KVN Key Science Program: Simultaneous Monitoring of KVN 4 Bands toward Evolved Stars (PI: Se-Hyung Cho)
  • KaVA Large Program: Expanded Study on Stellar Masers (ESTEMA) (co-PIs: Se-Hyung Cho, Hiroshi Imai)
Last modified: le 2018/06/08 23:28