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Recent studies have revealed that complex organic molecules (COMs) are abundant in not only high-mass star-forming regions but also in a cometary coma and protoplanetary disks. In V883 Ori, known as an outburst object, CH3COCH3, CH3CHO, and CH3OCHO were reported for the first time (Lee et al. 2019). The study of COMs in disk environments is one of the appealing frontlines in protoplanetary disks.
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While the detection of COMs is vigorous, it is not well known if these COMs are newly formed in disks or if they are inherited from the parental clouds. To answer this question, the chemical model is a powerful tool to reveal the origin of COMs. With the rate coefficients of chemical reactions, the chemical model can numerically solve the time evolution of COMs under a given physical condition. While the chemical model study has been mainly applied to high-mass or low-mass star-forming regions, our knowledge of protoplanetary disks is still limited due to the complex nature of the disks. Previous studies assumed the simple statics model where grains stay at the same position of the disk. However, the actual grain motion should be dynamic due to turbulence and dust grains with ice mantles are exposed to the dramatic change in physical condition.
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In this context, we perform chemical model calculations considering turbulence in the disk. First, we reproduce the turbulent motion of grains using the method of Ciesla & Sandford (2012). By tracking the trajectory, we obtain the temporal changes in temperature, UV, etc. for each grain. Then, we performed chemical model calculations with the numerical simulation code, rokko (Furuya et al. 2015). Based on the results of this model, we investigate the evolution of COMs for different grain sizes. We will discuss the origin of COMs and the possibility of future observation.
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