日本地球惑星科学連合2019年大会

講演情報

[E] ポスター発表

セッション記号 A (大気水圏科学) » A-OS 海洋科学・海洋環境

[A-OS11] 陸域海洋相互作用-惑星スケール物質循環

2019年5月29日(水) 17:15 〜 18:30 ポスター会場 (幕張メッセ国際展示場 8ホール)

コンビーナ:山敷 庸亮(京都大学大学院総合生存学館)、升本 順夫(東京大学大学院理学系研究科)、Behera Swadhin(Climate Variation Predictability and Applicability Research Group, Application Laboratory, JAMSTEC, 3173-25 Showa-machi, Yokohama 236-0001)、佐々木 貴教(京都大学 大学院理学研究科 宇宙物理学教室)

[AOS11-P02] Hydrological and Debris-flow simulation of Martian Surface in Hesperian & early Amazonian epoch

*佐藤 啓明2山敷 庸亮1黒木 龍介1宮本 英昭3逸見 良道3 (1.京都大学大学院総合生存学館、2.京都大学工学部、3.東京大学工学系研究科)

キーワード:へスペリア紀、土石流

It is considered that the Mars in Noachian ecoch to early Amazonian was much warmer temperature than current condition, with atmosphere and ocean supported by its magnetic activity. Several valley which seems to be developed by ancient hydrological processes are obsered in Martian surface, is being considered to be built long time before. Some fluvial fun was formed during the following Hesperian to early Amazonian epoch, which is considered as much cooler and drier than Noachian epoch. In this study, we applied Hydro-debris 2D model into Martian surface in Hesperian epoch in order to try develping surface vallay formation throughout hydrological processes.

Sediment transport and associated small-scale debris-flow occurrence may be the key for valley formation, where might be the micro-habitable zone in ancient period. At the same time it is still uncertain how much precipitation and erosion should have been required to formulate such topography. Following the last year’s calculation we attempted to compare several cases of debris flow experiments by changing hypothetical precipitation rate and erosive coefficients in the initially distributed regolith.