Geologic Constraints on Early Mars Climate
Geologic Constraints on Early Mars Climate
复制标题
早期火星气候的地质限制
DOI：
10.1007/s11214-018-0575-5
复制
发表时间：
2018
影响因子：
10.3
通讯作者：
E. Kite
中科院分区：
文献类型：
--
作者：
E. Kite
Early Mars climate research has well-defined goals (MEPAG 2018). Achieving these goals requires geologists and climate modelers to coordinate. Coordination is easier if results are expressed in terms of well-defined parameters. Key parameters include the following quantitative geologic constraints. (1) Cumulative post-3.4 Ga precipitation-sourced water runoff in some places exceeded 1km$1~\mbox{km}$ column. (2) There is no single Early Mars climate problem: the traces of ≥2 river-forming periods are seen. Relative to rivers that formed earlier in Mars history, rivers that formed later in Mars history are found preferentially at lower elevations, and show a stronger dependence on latitude. (3) The duration of the longest individual river-forming climate was >(102–103)yr${>}(10^{2}\mbox{--}10^{3})~\mbox{yr}$, based on paleolake hydrology. (4) Peak runoff production was >0.1mm/hr${>}0.1~\mbox{mm}/\mbox{hr}$. However, (5) peak runoff production was intermittent, sustained (in a given catchment) for only <10% of the duration of river-forming climates. (6) The cumulative number of wet years during the valley-network-forming period was >105yr${>}10^{5}~\mbox{yr}$. (7) Post-Noachian light-toned, layered sedimentary rocks took >107yr${>}10^{7}~\mbox{yr}$ to accumulate. However, (8) an “average” place on Mars saw water for <107yr${<}10^{7}~\mbox{yr}$ after the Noachian, suggesting that the river-forming climates were interspersed with long globally-dry intervals. (9) Geologic proxies for Early Mars atmospheric pressure indicate pressure was not less than 0.012 bar but not much more than 1 bar. A truth table of these geologic constraints versus currently published climate models shows that the late persistence of river-forming climates, combined with the long duration of individual lake-forming climates, is a challenge for most models.
Early Mars climate research has well-defined goals (MEPAG 2018). Achieving these goals requires geologists and climate modelers to coordinate. Coordination is easier if results are expressed in terms of well-defined parameters. Key parameters include the following quantitative geologic constraints. (1) Cumulative post-3.4 Ga precipitation-sourced water runoff in some places exceeded 1km$1~\mbox{km}$ column. (2) There is no single Early Mars climate problem: the traces of ≥2 river-forming periods are seen. Relative to rivers that formed earlier in Mars history, rivers that formed later in Mars history are found preferentially at lower elevations, and show a stronger dependence on latitude. (3) The duration of the longest individual river-forming climate was >(102–103)yr${>}(10^{2}\mbox{--}10^{3})~\mbox{yr}$, based on paleolake hydrology. (4) Peak runoff production was >0.1mm/hr${>}0.1~\mbox{mm}/\mbox{hr}$. However, (5) peak runoff production was intermittent, sustained (in a given catchment) for only <10% of the duration of river-forming climates. (6) The cumulative number of wet years during the valley-network-forming period was >105yr${>}10^{5}~\mbox{yr}$. (7) Post-Noachian light-toned, layered sedimentary rocks took >107yr${>}10^{7}~\mbox{yr}$ to accumulate. However, (8) an “average” place on Mars saw water for <107yr${<}10^{7}~\mbox{yr}$ after the Noachian, suggesting that the river-forming climates were interspersed with long globally-dry intervals. (9) Geologic proxies for Early Mars atmospheric pressure indicate pressure was not less than 0.012 bar but not much more than 1 bar. A truth table of these geologic constraints versus currently published climate models shows that the late persistence of river-forming climates, combined with the long duration of individual lake-forming climates, is a challenge for most models.
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影响因子：
3.5
作者：
F. Rivera‐Hernández;D. Sumner;T. Mackey;I. Hawes;D. Andersen
通讯作者：
F. Rivera‐Hernández;D. Sumner;T. Mackey;I. Hawes;D. Andersen
影响因子：
56.9
作者：
Rebecca M. E. Williams;J. Grotzinger;W. Dietrich;Sanjeev Gupta;D. Sumner;R. Wiens;N. Mangold;M. Malin;K. Edgett;S. Maurice;O. Forni;O. Gasnault;A. Ollila;H. Newsom;G. Dromart;M. Palucis;R. Yingst;R. Anderson;K. Herkenhoff;S. Mouélic;W. Goetz;M. Madsen;A. Koefoed;J. Jensen;J. Bridges;S. Schwenzer;K. Lewis;K. Stack;D. Rubin;Linda C. Kah;J. Bell;J. Farmer;R. Sullivan;T. V. Beek;D. Blaney;O. Pariser;R. Deen
通讯作者：
Rebecca M. E. Williams;J. Grotzinger;W. Dietrich;Sanjeev Gupta;D. Sumner;R. Wiens;N. Mangold;M. Malin;K. Edgett;S. Maurice;O. Forni;O. Gasnault;A. Ollila;H. Newsom;G. Dromart;M. Palucis;R. Yingst;R. Anderson;K. Herkenhoff;S. Mouélic;W. Goetz;M. Madsen;A. Koefoed;J. Jensen;J. Bridges;S. Schwenzer;K. Lewis;K. Stack;D. Rubin;Linda C. Kah;J. Bell;J. Farmer;R. Sullivan;T. V. Beek;D. Blaney;O. Pariser;R. Deen
影响因子：
5
作者：
Bedford, C. C.;Bridges, J. C.;Gasda, P. J.
通讯作者：
Gasda, P. J.
唐璜池的地球化学：南极洲莱特谷深层地下水流动系统的证据
影响因子：
5.3
作者：
Toner, J.D.;Catling, D.C.;Sletten, R.S.
通讯作者：
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影响因子：
5.8
作者：
Davis, J. M.;Balme, M.;Gupta, S.
通讯作者：
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