演講資訊

摘要：

Planets are thought to be formed from gas and dust in protoplanetary disks. Thanks to recent development of (sub)mm and infrared instruments for astronomical observations, it has become possible to detect transition lines of molecules in the disks, which reveal detailed physical and chemical structure of planet-forming regions. We have constructed models of protoplanetary disks, using a comprehensive astrochemical reaction network together with the detailed calculations of gas density and temperature profiles. The chemical network includes gas-phase reactions as well as grain surface chemistry together with UV- and X-ray-induced reactions. In this talk I will introduce our recent work, especially focusing on how to diagnose formation process of complex organic molecules in the disks and also photoevaporation process which is one of the possible mechanisms for gas dispersal from the disks.