Summary and Future Works

Abstract

Observationally locating the position of the H$_{2}$O snowline in protoplanetary disks is important to understand the processes of planetesimal and planet formation, and the origin of water on terrestrial planets including the Earth. In this thesis, we proposed the method to locate the H$_{2}$O snowline position more directly by analyzing the Keplerian water line profiles which can be obtained by high dispersion spectroscopic observations across a wide range of wavelengths (from mid-infrared to sub-millimeter, e.g., ALMA, SPICA) and selected based on specific criteria. In addition, we also reported the results of water line observations for the protoplanetary disk around the Herbig Ae star HD 163296, and constrained the dust opacity and the line emitting region from the observations. Most contents of this thesis is based on our refereed papers which have been published (Notsu et al. 2016, ApJ, 827, 113; 2017, ApJ, 836, 118; 2018, ApJ, 855, 62; 2019, ApJ, 875, 96).