11:15 〜 11:30
[SIT21-03] 原始太陽系円盤の化学進化－地球外物質からの制約
★招待講演
キーワード：原始惑星系円盤、太陽系、化学進化
Solar System bodies exhibit physical and chemical diversity, at least partially reflecting the chemical evolution of the Sun's protoplanetary disk during the first few to several million years after its formation. Astronomical observations indicate that protoplanetary disks vary in physical and chemical properties, including mass, size, molecular composition, and lifetime. The Sun's protoplanetary disk was one of these diverse disks, of which properties cannot be fully constrained by astronomical observations alone (e.g., Pascucci and Tachibana 2010). Instead, they should be inferred through the study of primordial extraterrestrial materials that preserve records of the early evolution of the Solar System.
The chemical evolution of the Sun's protoplanetary disk is likely to be recorded in the elemental and isotopic compositions of meteorites and spacecraft returned samples, the mineralogy and petrology of a variety of primordial components, the formation timing of various chondritic components, and the evolutionary processes of planetesimals.
Primordial extraterrestrial materials preserve records of physicochemical environments, but they are not reliable indicators of specific locations within the protoplanetary disk. We should thus be cautious when using them to reconstruct the evolution of the Sun's protoplanetary disk. To address this issue, my research group has been integrating knowledge from extraterrestrial materials, including returned asteroid samples (e.g., Tachibana et al. 2022), with laboratory experiments (e.g., Tachibana et al. 2011; Takigawa et al. 2015; Tachibana et al. 2017; Piani et al. 2017; Yamamoto and Tachibana 2018; Yamamoto et al. 2018, 2020, 2024; Isono et al. 2019; Mendynaev et al. 2020; Kamibayashi et al. 2021), disk modeling (e.g., Ishizaki et al. 2023), and astronomical observation (e.g., Tachibana et al. 2019; Tachibana and Sakai 2024). In the session, I will discuss the advantage and limitations of extraterrestrial materials in revealing the Sun's protoplanetary disk, review our currect understanding, and share my (probably biased) view on its evolution.
The chemical evolution of the Sun's protoplanetary disk is likely to be recorded in the elemental and isotopic compositions of meteorites and spacecraft returned samples, the mineralogy and petrology of a variety of primordial components, the formation timing of various chondritic components, and the evolutionary processes of planetesimals.
Primordial extraterrestrial materials preserve records of physicochemical environments, but they are not reliable indicators of specific locations within the protoplanetary disk. We should thus be cautious when using them to reconstruct the evolution of the Sun's protoplanetary disk. To address this issue, my research group has been integrating knowledge from extraterrestrial materials, including returned asteroid samples (e.g., Tachibana et al. 2022), with laboratory experiments (e.g., Tachibana et al. 2011; Takigawa et al. 2015; Tachibana et al. 2017; Piani et al. 2017; Yamamoto and Tachibana 2018; Yamamoto et al. 2018, 2020, 2024; Isono et al. 2019; Mendynaev et al. 2020; Kamibayashi et al. 2021), disk modeling (e.g., Ishizaki et al. 2023), and astronomical observation (e.g., Tachibana et al. 2019; Tachibana and Sakai 2024). In the session, I will discuss the advantage and limitations of extraterrestrial materials in revealing the Sun's protoplanetary disk, review our currect understanding, and share my (probably biased) view on its evolution.