火星水冰分布特征和研究进展

刘正豪; 刘洋; 刘佳; 牛胜利; 邹永廖

doi:10.3799/dqkx.2023.205

火星水冰分布特征和研究进展

doi: 10.3799/dqkx.2023.205

刘正豪^{1, 2, ,},
刘洋^{1, 3, ,},
刘佳¹,
牛胜利¹,
邹永廖¹

1.
中国科学院国家空间科学中心空间天气学国家重点实验室, 北京 100190
2.
中国科学院大学, 北京 100049
3.
中国科学院比较行星学卓越创新中心, 安徽合肥 230026

基金项目:

国家重点研发计划 2019YFE0123300

国家自然科学基金面上项目 42072337

国家自然科学基金青年基金 42202263

中国博士后科学基金 2022M720144

详细信息

作者简介:
刘正豪（1995-），男，博士研究生，主要从事行星地质学与遥感研究. ORCID：0009-0006-3682-7597. E-mail：liuzhenghao17@mails.ucas.ac.cn

通讯作者:
刘洋，研究员，主要从事行星科学，行星宜居性与行星遥感等研究. E-mail：yangliu@nssc.ac.cn

中图分类号: P691
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出版历程
- 收稿日期: 2023-09-25
- 网络出版日期: 2024-07-11
- 刊出日期: 2024-06-25

Distribution Characteristics and Research Progress of Water-Ice on Mars

Liu Zhenghao^{1, 2
,
,},
Liu Yang^{1, 3
, ,},
Liu Jia¹,
Niu Shengli¹,
Zou Yongliao¹

1.
State Key Laboratory of Space Weather, National Space Science Center, Chinese Academy of Sciences, Beijing 100190, China
2.
University of Chinese Academy of Sciences, Beijing 100049, China
3.
Center for Excellence in Comparative Planetology, Chinese Academy of Sciences, Hefei 230026, China

摘要

摘要: 火星作为太阳系中与地球相似的一颗行星，它曾经存在活跃的水活动历史，现今火星稀薄的大气和寒冷干旱的气候使得液态水很难存在于火星表面，火星上水大多以冰的形式在南北两极和中纬度区域分布并形成沉积地貌类型.随着国内外深空探测任务的逐年增多，火星上的水冰环境与宜居性越来越受到关注，以极区冰盖、中纬度冰川作用地貌和浅地表水冰升华地貌为重点，对它们的形貌特征、分布情况、成因机制以及与气候的耦合关系进行介绍和剖析.火星中纬度地区水冰地貌的分布与自转轴倾角有关，当火星处于高倾角时，极区水冰会向中纬度表面转移，此时火星转变为寒冷的冰期，中纬度水冰环境区域增加；反之，则极区冰盖区域增加.因此，火星自转轴倾角的周期性改变引起气候的改变，从而导致形成了水冰在火星表面不断重新分布的过程，主要表现为从极区到中高纬度区域水冰阶段性的富集.通过对火星水冰分布特征的总结，加深了对火星水冰环境的认识，同时结合火星水冰的研究现状提出了展望.火星水冰地貌与火星宜居环境以及生命赋存形式息息相关，对火星水冰的研究可以帮助我们深入了解火星的气候演化历史、宜居环境情况等以及为未来的火星探测任务提供支撑.
- 火星水冰 /
- 冰盖 /
- 冰川 /
- 地貌特征 /
- 气候演化 /
- 行星地质
Abstract: Mars, as a planet in the solar system similar to Earth, once had a history of active water activities. However, its current thin atmosphere and cold, arid climate make it difficult for liquid water to exist on the Martian surface. Water on modern Mars is mostly present in the form of ice at the polar regions and mid-latitude areas, forming various types of depositional landforms. With the growing number of deep space exploration missions, the water-ice environment and habitability of Mars have attracted more attention. In this article it focuses on polar ice caps, glacial landforms in mid-latitudes and sublimation landforms of shallow subsurface water-ice in mid-latitudes. It introduces and analyzes their morphological characteristics, distribution, formation mechanisms, and their coupling with the climate. The formation of mid-latitude water-ice landforms on Mars is, due to the migration of polar water-ice to the mid-latitude surface when Mars is at a high obliquity, transitioning to a cold glacial period in those regions. Conversely, this leads to an expansion of polar ice cap regions. Thus, the periodic changes in Martian obliquity have driven climate variations and the subsequent redistribution of water-ice on the Martian surface, characterized by a cyclic enrichment from polar to mid-high latitude regions. By summarizing the distribution characteristics of water-ice on Mars, our understanding of the Martian water-ice environment is improved. Also, several prospects on the future research directions are provided based on the current research status of Martian water-ice. The Martian water-ice landforms are closely linked to the habitable environment and potential forms of life on Mars. Studying water-ice on Mars can help us gain insights into Martian climate evolution history, habitability conditions, and provide support for future Mars exploration missions.
- Martian water-ice /
- ice sheets /
- glaciers /
- geomorphology characteristic /
- climate evolution /
- planetary geology

HTML全文

图 1 随季节改变的火星极地冰盖.由E.S.Holden在Lick天文台拍摄的火星图像，并由Ted Stryk修复和增强(修改自Smith, 2022)

Fig. 1. Seasonally changing polar ice caps on Mars.Image of Mars taken by E.S.Holden at Lick Observatory, restored and enhanced by Ted Stryk (modified from Smith, 2022)

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图 2 早期发现的类水冰地貌

a.中纬度区域Fretted terrain，中央经纬度：61.5°W，44.0°N（修改自Sharp，1973）；b.中纬度沉积覆盖层，中央经纬度：30.0°E，64.0°S（修改自Soderblom et al.，1973）；c.中纬度区域热岩溶地貌，中央经纬度：153.3°W，69.4°N；修改自Gatto and Anderson（1975）

Fig. 2. Earlier water-ice like landforms

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图 3 火星60°纬度以下SWIM水冰综合分布结果，Ci值为水冰综合出现可能性，其大于0.2时置信度较高，Ci值为1时水冰最可能出现(修改自Butcher, 2022)

Fig. 3. The comprehensive distribution results(SWIM) of water-ice below 60° latitude on Mars, Ci value is the possibility of comprehensive occurrence of water-ice.The confidence is high when Ci value is greater than 0.2, and water-ice is most likely to occur when Ci value is 1 (modified from Butcher, 2022)

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图 4 火星南北极冰盖区域地形地貌特征与剖面图，经度间隔30°，纬度间隔5°

a图中Planum Boreum为NPLD分布范围；b图中Planum Australe为SPLD分布范围，图区左上角为DAF沉积；修改自Byrne（2009）

Fig. 4. Topography and profile of the North and South Polar ice cap regions of Mars, 30° longitude interval, 5° latitude interval

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图 5 中纬度典型LVF、LDA、CCF类型的冰缘沉积地貌分布，底图为MOLA高程图(引自Levy et al., 2014)

Fig. 5. Typical distribution of periglacial sedimentary landforms of LVF, LDA and CCF types in mid-latitude, the basemap is MOLA elevation (cited from Levy et al., 2014)

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图 6 中纬度典型LVF地貌分布，中央经纬度：23.2°E, 38.1°N(a)；山谷中的LVF平行纹理(b，c)

Fig. 6. Typical LVF landform distribution in mid-latitude, central coordinates: 23.2°E, 38.1°N (a); LVF parallel texture in the valley (b, c)

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图 7 中纬度典型LDA地貌分布，中央经纬度：26.3°E, 45.5°N

Fig. 7. Typical LDA landform distribution in mid-latitude, central coordinates: 26.3°E, 45.5°N

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图 8 中纬度典型CCF地貌，中央经纬度：87.9°E, 36.1°N

Fig. 8. Typical CCF landform in mid-latitude, central coordinates: 87.9°E, 36.1°N

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图 9 中纬度LDM沉积，中央经纬度：173.9°W, 35.1°S

Fig. 9. Mid-latitude LDM deposit, central coordinates: 173.9°W, 35.1°S

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图 10 Utopia平原扇形凹陷，中央经纬度：90.7°E, 45.9°N

a.独立和合并分布的扇形凹陷；b.扇形凹陷内部结构

Fig. 10. Utopia planitia scallop depression, central coordinates: 90.7°E, 45.9°N

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图 11 扇形凹陷外的多边形地貌，中央经纬度：93.7°E, 45.6°N

Fig. 11. Polygon outside scallop depression, central coordinates: 93.7°E, 45.6°N

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图 12 火星小尺度多边形地貌类型(修改自Levy et al., 2009a)

Fig. 12. Small-scale polygons on Mars (modified from Levy et al., 2009a)

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图 13 火星典型冲沟地貌，中央经纬度：1.5°E, 68.4°S

Fig. 13. Typical gullies on Mars, central coordinates: 1.5°E, 68.4°S

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图 14 火星典型暴露水冰区域

a.凤凰号着陆点挖掘冰，中央经纬度：125.8°W，68.2°S（修改自Mellon et al.，2009）；b.撞击坑暴露冰，中央经纬度：94.8°W，50.5°N；c.陡坎暴露冰，中央经纬度：96.3°E，56.8°S

Fig. 14. Typical exposed water-ice areas on Mars

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图 15 20~10 Ma自转轴倾角变化(a); 20~10 Ma轨道偏心率变化(b); 20~10 Ma北极夏至太阳辐照度变化(c)

a图单位为度; c图单位为W/m²; 修改自Laskar et al.(2004)

Fig. 15. 20-10 Ma Martian obliquity change (a); 20-10 Ma eccentricity change (b); 20-10 Ma insolation change of north pole surface at summer solstice (c)

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表 1 火星水冰地貌分类

Table 1. Classification of Martian water-ice landforms

地貌类型	分布区域	形成机制
极地冰盖	极区-高纬度	冰层沉积覆盖
冰川沉积地貌	中纬度-高纬度	冰川流动沉积
浅地表水冰地貌	中纬度-高纬度	浅地表水冰升华
冰下湖泊	南极区域	冰盖基底融化

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