日本地球惑星科学連合2016年大会

講演情報

ポスター発表

セッション記号 P (宇宙惑星科学) » P-PS 惑星科学

[P-PS12] 太陽系における惑星物質の形成と進化

2016年5月24日(火) 17:15 〜 18:30 ポスター会場 (国際展示場 6ホール)

コンビーナ:*宮原 正明(広島大学理学研究科地球惑星システム学専攻)、山口 亮(国立極地研究所)、臼井 寛裕(東京工業大学地球惑星科学科)、癸生川 陽子(横浜国立大学 大学院工学研究院 機能の創生部門)、藤谷 渉(茨城大学 理学部)、瀬戸 雄介(神戸大学大学院理学研究科)、伊藤 正一(京都大学大学院理学研究科)

17:15 〜 18:30

[PPS12-P02] 複合コンドリュールの形成過程:過冷却液滴の衝突による結晶化

*荒川 創太1中本 泰史1 (1.東京工業大学大学院理工学研究科)

キーワード:複合コンドリュール、過冷却、結晶化、衝突

Some chondrules are composed of two (or more) chondrules fused together. They are called compound chondrules. Compound chondrules have several remarkable features. In this study, we focus on three features; (1) textural types, (2) the size ratio between two components, and (3) the fraction of compound chondrules. In previous studies, these three features are remained to explain.
Textural types of chondrules originate from their thermal histories. Non-porphyritic chondrules (e.g., barred olivine, radial pyroxene, and cryptocrystalline) are formed from completely molten precursors, while porphyritic chondrules are formed from partially molten precursors. As for single chondrules, the majority is porphyritic type (84%) and non-porphyritic ones are rare (16%). In contrast, more than 80% of all the compound chondrules have non-porphyritic textures. This significant feature suggests that compound chondrules are crystallized from completely molten precursors.
Experimental studies revealed that floating completely molten precursors turn into supercooled droplets without crystallization, and non-porphyritic chondrules are produced by crystallization of supercooled droplets triggered by contact with something. In addition, theoretical studies suggest that the duration of supercooling can be long.
Here, we propose a new model for the compound chondrule formation: compound chondrules are formed by collision-induced crystallization of supercooled droplets. This model is based on the feature (1) and experimental facts. Additionally, we can obtain the feature (2) that larger ones of compound chondrules keep round shapes while smaller ones are deformed. This feature is explained by the reason that larger ones are likely to be collided more than smaller ones.
We also estimate the product of the number density of precursors n and the duration of supercooling t for reproducing the fraction of compound chondrules. Then the product of the number density and the duration is n t = 0.1 cm-3 s. Thanks to the supercooling, we can explain the fraction of compound chondrules with large t and low n.