DOI: 10.1016/j.epsl.2020.116406
论文题名: Mud flow levitation on Mars: Insights from laboratory simulations
作者: Brož P. ; Krýza O. ; Conway S.J. ; Mueller N.T. ; Hauber E. ; Mazzini A. ; Raack J. ; Balme M.R. ; Sylvest M.E. ; Patel M.R.
刊名: Earth and Planetary Science Letters
ISSN: 0012821X
出版年: 2020
卷: 545 语种: 英语
中文关键词: analogue experiments
; levitation
; low pressure chamber
; Mars
; mud flow
; sedimentary volcanism
英文关键词: Atmospheric pressure
; Celestial bodies
; Flow features
; Laboratory simulation
; Martian surface
; Sand particles
; Surface of Mars
; Surface temperatures
; Unconsolidated sands
; Morphology
; atmospheric pressure
; computer simulation
; laboratory method
; Mars
; mudflow
; surface temperature
英文摘要: Sediment mobilisation occurring at depth and ultimately manifesting at the surface, is a process which may have operated on Mars. However, the propagation behaviour of this mixture of water and sediments (hereafter simply referred to as mud) over the martian surface, remains uncertain. Although most of the martian surface is below freezing today, locally warmer surface temperatures do occur, and our current knowledge suggests that similar conditions prevailed in the recent past. Here, we present the results of experiments performed inside a low pressure chamber to investigate mud propagation over a warm (∼295 K) unconsolidated sand surface under martian atmospheric pressure conditions (∼7 mbar). Results show that the mud boils while flowing over the warm surface. The gas released during this process can displace the underlying sand particles and hence erode part of the substrate. This “entrenched” flow can act as a platform for further mud propagation over the surface. The escaping gas causes intermittent levitation of the mud resulting in enhanced flow rates. The mud flow morphologies produced by these phenomena differ from those produced when mud flows over a frozen martian surface as well as from their terrestrial counterparts. The intense boiling removes the latent heat both from the mud and the subsurface, meaning that the mud flow would eventually start to freeze and hence changing again the way it propagates. The diverse morphology expressed by our experimental mudflows implies that caution should be exercised when interpreting flow features on the surface of Mars and other celestial bodies. © 2020 Elsevier B.V. Citation statistics:
资源类型: 期刊论文
标识符: http://119.78.100.158/handle/2HF3EXSE/164892
Appears in Collections: 气候变化与战略
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作者单位: Institute of Geophysics of the Czech Academy of Sciences, Boční II/1401, Prague, 14131, Czech Republic; CNRS UMR-6112 Laboratoire de Planétologie et Géodynamique, Université de Nantes, France; Institute of Planetary Research, DLR, Rutherfordstr. 2, Berlin, 12489, Germany; Centre for Earth Evolution and Dynamics (CEED), University of Oslo, Norway; Institut für Planetologie, Westfälische Wilhelms-Universität, Münster, Germany; School of Physical Science, STEM, The Open University, Milton Keynes, United Kingdom; Space Science and Technology Department, STFC Rutherford Apple-ton Laboratory, Oxford, United Kingdom
Recommended Citation:
Brož P.,Krýza O.,Conway S.J.,et al. Mud flow levitation on Mars: Insights from laboratory simulations[J]. Earth and Planetary Science Letters,2020-01-01,545