(Proposal ID) S14A-125 (PI) Ootsubo Takafumi (Proposal Title) Grain properties of crystalline silicate in Oort cloud comets II (Abstract) Crystalline silicate is sometimes observed in comets as an 11.3-micron resonant emission feature, and may be used for probing the early solar nebula. Because the formation of the crystalline silicate grains requires high temperature, they are thought to be born from amorphous silicates at the inner region, and then transported toward the outer region where comets were born. This transportation can produce the difference in the fraction of crystalline silicate in the cometary dust between two dynamical types of comets, Oort- cloud comets (OCs) and Ecliptic comets (ECs), due to the different heliocentric distances of their birth places. Recently, it is suggested that infrared spectra and peak wavelengths of silicate (forsterite) features depend on particle shapes. From this point of view, peak wavelengths of crystalline silicate features in comet spectra are important to investigate the conditions of the crystalline silicate formation in the early solar nebula. Fortunately, we can observe the comet C/2012 K1 (PanSTARRS) along with C/2012 X1 (LINEAR) in this semester. In particular, the comet C/2012 K1 is a bright and good target for this silicate peak feature study.