Please use this identifier to cite or link to this item: https://ah.nccu.edu.tw/handle/140.119/60831


Title: Late Noachian to Hesperian Climate Change on Mars: Evidence of Episodic Warming from Transient Crater Lakes near Ares Vallis
Authors: Warner,Nick;Gupta,Sanjeev;Lin,Shih-Yuan;Kim,Jung-Rack;Muller,Jan-Peter;Morley,Jeremy
林士淵
Contributors: 政大地政系
Keywords: Iani Chaos;chaos;catastrophic floods;Mars;Ares Vallis;interior layered deposits
Date: 2011-03
Issue Date: 2013-09-13 14:10:17 (UTC+8)
Abstract: The origin mechanisms and geologic evolution of chaotic terrain on Mars are poorly constrained. Iani Chaos, located at the head Ares Vallis, is among the most geomorphologically complex of the chaotic terrains. Its morphology is defined by (1) multiple, 1 to 2 km deep basins, (2) flat-topped, fractured plateaus that are remnants of highland terrain, (3) knobby, fractured remnants of highland terrain, (4) plateaus with a knobby surface morphology, (5) interchaos grooved terrain, (6) interior layered deposits (ILDs), and (7) mantling material. Topography, the observed geomorphology, and measured fracture patterns suggest that the interchaos basins formed as a result of subsurface volume loss and collapse of the crust, likely owing to effusion of groundwater to the surface. Regional patterns in fracture orientation indicate that the basins developed along linear zones of preexisting weakness in the highland crust. Multiple overlapping basins and fracture systems point to multiple stages of collapse at Iani Chaos. Furthermore, the total estimated volume loss from the basins (104 km3) is insufficient to explain erosion of 104–105 km3 of material from Ares Vallis by a single flood. Comparisons with the chronology of Ares Vallis indicate multiple water effusion events from Iani Chaos that span the Hesperian, with termination of activity in the early Amazonian. Recharge of groundwater through preexisting fracture systems may explain this long-lived, but likely episodic, fluvial activity. Late-stage, early to middle Amazonian aqueous processes may have deposited the ILDs. However, the topography data indicate that the ILDs did not form within lacustrine environments.
Relation: Journal of Geophysical Research: Planets, 116
Data Type: article
Appears in Collections:[地政學系] 期刊論文

Files in This Item:

File Description SizeFormat
2761.pdf1930KbAdobe PDF1062View/Open


All items in 學術集成 are protected by copyright, with all rights reserved.


社群 sharing