月球南海地区玄武岩厚度估算
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摘要
月海玄武岩是月幔部分熔融喷出月表而形成的,其厚度可以反映月海玄武岩源区的深度。研究月海玄武岩厚度,对进一步认识月球区域岩浆作用或火山作用的演化历史具有不可替代的作用,也能够为整个月球的热演化和岩浆演化提供基本的约束条件。同时,玄武岩厚度可以用以推测月球内部产生玄武岩岩浆的体积,对月球火山作用的岩浆喷发总量以及月球内部的热状态具有指示作用。本文基于多源遥感数据,综合利用撞击坑的形貌特征与月坑挖掘深度法对南海地区撞击坑内(crater)和撞击坑间(intercrater)两类玄武岩地层的厚度进行了估算,并对玄武岩的面积、体积、年龄及岩浆活动做了简单分析。研究结果表明:南海地区撞击坑内的玄武岩厚度变化范围为0.11～4.75km,平均值约为1.32km,玄武岩的出露面积和出露体积分别为57.06～10 791.66km~2和10.25～51 260.38km~3;撞击坑间的玄武岩厚度变化范围为0.01～2.18km,平均值约为0.34km,玄武岩的出露面积和出露体积分别为6 487.89～33 170.55km~2和2 711.97～11 609.69km~3。因此,南海地区玄武岩厚度的变化范围分布在0.01～4.75km,平均厚度约为600m,出露的玄武岩总面积约为2.12×10~5 km~2,总体积约为2.71×10~5 km~3。通过分析南海地区的玄武岩年龄及分布特征,发现南海地区内的岩浆喷发活动主要集中发生在雨海纪至爱拉托逊纪时期,且其局部区域存在多次岩浆喷发及充填过程,但由于晚期玄武岩岩浆的喷发总量不足以覆盖早期已形成的玄武岩,导致晚期玄武岩与早期玄武岩同时存在于同一个玄武岩单元内。南海地区独特的玄武岩分布特征也与地形有关。
Mare basalts were formed from partial melting mantle followed by volcanic eruption to the lunar surface.The thickness of mare basalt plays an important role in the study of magmatic process during Moon's evolution and can reflect the depths of the mare basalts source region.It can help us understand the regional volcanism and provide the basic constraints for the thermal and/or magma evolution of entire Moon.Also,the thickness of mare basalt can be used to estimate basalt volumes and indicate the total amount of magma eruption and the thermal state of the Moon.In this paper,by using multi-source remote sensing data and combing the crater morphological characteristics with crater excavation method,we estimated the thickness of Mare Australe basalts in crater and intercrater and analyzed the area,volume,age and magmatic activities.The results showed that the thickness of basalts in crater ranged between 0.11 and 4.75 km with an average thickness of 1.32 km,and the total area and volume of exposed basalts were approximately 57.06-10791.66 km~2 and 10.25- 51260.38 km~3,respectively.The thickness of basalts in intercrater was found to be0.01-2.18 km with an average thickness of 0.34 km,and the total area and volume of exposed basalts were about 6487.89-33170.55 km~2 and 2711.97-11609.69 km~3,respectively.As a result,we estimated the thickness of basalts in Mare Australe to be 0.01-4.75 km and averaged at 600 m,and the total area and volume of exposed basalts to be approximately 2.12×10~5 km~2 and 2.71×10~5 km~3,respectively.By analyzing the ages and distribution characteristics of basalts,we found that the magma eruption activities were mainly concentrated between the Imbrian and Eratosthenian era,along with many localized multi-stage magmatic eruptions and filling processes in Mare Australe,which led to coexistence of the early and late stage basalt in a same basalt unit simultaneously,and the unique distribution characteristics of Mare Australe basalts are related to their topography.
Mare basalts were formed from partial melting mantle followed by volcanic eruption to the lunar surface.The thickness of mare basalt plays an important role in the study of magmatic process during Moon's evolution and can reflect the depths of the mare basalts source region.It can help us understand the regional volcanism and provide the basic constraints for the thermal and/or magma evolution of entire Moon.Also,the thickness of mare basalt can be used to estimate basalt volumes and indicate the total amount of magma eruption and the thermal state of the Moon.In this paper,by using multi-source remote sensing data and combing the crater morphological characteristics with crater excavation method,we estimated the thickness of Mare Australe basalts in crater and intercrater and analyzed the area,volume,age and magmatic activities.The results showed that the thickness of basalts in crater ranged between 0.11 and 4.75 km with an average thickness of 1.32 km,and the total area and volume of exposed basalts were approximately 57.06-10791.66 km~2 and 10.25- 51260.38 km~3,respectively.The thickness of basalts in intercrater was found to be0.01-2.18 km with an average thickness of 0.34 km,and the total area and volume of exposed basalts were about 6487.89-33170.55 km~2 and 2711.97-11609.69 km~3,respectively.As a result,we estimated the thickness of basalts in Mare Australe to be 0.01-4.75 km and averaged at 600 m,and the total area and volume of exposed basalts to be approximately 2.12×10~5 km~2 and 2.71×10~5 km~3,respectively.By analyzing the ages and distribution characteristics of basalts,we found that the magma eruption activities were mainly concentrated between the Imbrian and Eratosthenian era,along with many localized multi-stage magmatic eruptions and filling processes in Mare Australe,which led to coexistence of the early and late stage basalt in a same basalt unit simultaneously,and the unique distribution characteristics of Mare Australe basalts are related to their topography.
引文
[1]HEAD J W.Lunar volcanism in space and time[J].Reviews of Geophysics,1976,14(2):265-300.
[2]SOLOMON S C,HEAD J W.Lunar Mascon Basins:lava filling,tectonics,and evolution of the lithosphere[J].Reviews of Geophysics&Space Physics,1980,18(1):107-141.
[3]DEHON R A.Thickness of western mare basalts[C]∥The Woodlands.Tou Texas,USA:LPSC,1979:2935-2955.
[4]WHITFORDSTARK J L.Charting the Southern Seas:the evolution of the Lunar Mare Australe[J].Lunar&Planetary,1979,10:2975-2994.
[5]HEAD J W.Lava flooding of ancient planetary crusts:geometry,thickness,and volumes of flooded lunar impact basins[J].Moon&the Planets,1982,26(1):61-88.
[6]YINGST R A,HEAD J W.Volumes of lunar lava ponds in South Pole-Aitken and Orientale Basins:implications for eruption conditions transport mechanisms,and magma source regions[J].Journal of Geophysical Research,1997,102(E5):10909-10931.
[7]BUDNEY C J,LUCEY P G.Basalt thickness in Mare Humorum:the crater excavation method[J].Journal of Geophysical Research Planets,1998,103(E7):16855-16870.
[8]HIESINGER H,HEAD J W,WOLF U,et al.Lunar mare basalt flow units:thicknesses determined from crater sizefrequency distributions[J].Geophysical Research Letters,2002,29(8):891-894.
[9]THOMSON B J,GROSFILS E B,BUSSEY D B J,et al.Anew technique for estimating the thickness of mare basalts in Imbrium Basin[J].Geophysical Research Letters,2009,36,L12201.
[10]TALWANI M,THOMPSON G,DENT B,et al.Traverse gravimeter experiment[C]∥Apollo 17:preliminary science report.Washington DC:NASA,1973:13.
[11]SHARPTON V L,HEAD J W.Stratigraphy and structural evolution of Southern Mare Serenitatis:a reinterpretation based on Apollo Lunar Sounder experiment data[J].Journal of Geophysical Research:Solid Earth,1982,87(B13):10983-10998.
[12]刘万崧,陈圣波,于岩,等.月球风暴洋地区玄武岩厚度的重力研究[J].地学前缘,2014,21(6):102-106.
[13]EVANS A J,SODERBLOM J M,ANDREWS-HANNA JC,et al.Identification of buried lunar impact craters from GRAIL data and implications for the nearside maria[J].Geophysical Research Letters,2016,43(6):486-494.
[14]GONG S,WIECZOREK M A,NIMMO F,et al.Thicknesses of mare basalts on the Moon from gravity and topography[J].Journal of Geophysical Research Planets,2016,121(5):854-870.
[15]陈媛,蒋云,张迅与,等.雨海晚期玄武岩的规模研究[J].中国科学:物理学力学天文学,2016,46(2):29604.
[16]WILHELMS D E,MCCAULEY J F,TRASK N J.The geologic history of the Moon[M].Washington DC:US Geological Survey,1987.
[17]GILLIS J J,JOLLIFF B L.An analysis of remotely sensed data of Mare Australe[R]∥The Moon beyond 2002:next steps in lunar science and exploration.New Mexico:Lunar and Planetary Institute,2002.
[18]STUART-ALEXANDER D E,HOWARD K A.Lunar Maria and circular basins:a review[J].Icarus,1970,12(3):440-456.
[19]WILHELMS D E,EL-BAZ F.Geologic map of the eastern limb of the Moon[CM]∥USGS Map I-948.Washington DC:Department of the Interior United States Geological Survey,1977:134-157.
[20]GILLIS J J.The composition and geologic setting of mare deposits on the far side of the Moon[D].Houston,Texas:Rice University,1998.
[21]ROBINSON M S,BRYLOW S M,TSCHIMMEL M,et al.Lunar Reconnaissance Orbiter Camera(LROC)instrument overview[J].Space Science Reviews,2010,150(1/2/3/4):81-124.
[22]SMITH D E,ZUBER M T,NEUMANN G A,et al.Initial observations from the Lunar Orbiter Laser Altimeter(LOLA)[J].Geophysical Research Letters,2015,37(18):109-118.
[23]NOZETTE S,RUSTAN P,PLEASANCE L P,et al.The Clementine mission to the Moon:scientific overview[J].Science,1994,266(5192):1835-1839.
[24]LUCEY P G,BLEWETT D T,JOLLIFF B L.Lunar iron and titanium abundance algorithms based on final processing of Clementine ultraviolet-visible images[J].Journal of Geophysical Research Atmospheres,2000,105(E8):20297-20305.
[25]WILLIAMS K K,ZUBER M T.Measurement and analysis of lunar basin depths from Clementine altimetry[J].Icarus,1998,131(1):107-122.
[26]CROFT S K.Cratering flow fields:implications for the excavation and transient expansion stages of crater formation[C]∥The Woodlands.Texas,USA:LPSC,1980:2347-2378.
[27]MELOSH H J.Impact cratering:ageologic process[M].Oxford:Oxford University Press,1989.
[28]LOSIAK A,WILHELMS D E,BYRNE C J,et al.A new lunar impact crater database[C]∥The Woodlands.Houston,Texas,USA:LPSC,2009:1532.
[29]KALYNN J,JOHNSON C L,OSINSKI G R,et al.Topographic characterization of lunar complex craters[J].Geophysical Research Letters,2013,40(1):38-42.
[30]凌宗成,刘建忠,张江,等.基于“嫦娥一号”干涉成像光谱仪数据的月球岩石类型填图:以月球雨海-冷海地区(LQ-4)为例[J].地学前缘,2014,21(6):107-120.
[31]籍进柱,刘建忠,张莉,等.云海地区月海玄武岩厚度估算[C]∥“月球·行星·科学与探测”学术研讨会论文集.贵阳:中国科学院地球化学研究所,2014:48-50.
[32]籍进柱,刘建忠,郭弟均,等.云海撞击盆地的恢复及其地质演化研究[J].岩石学报,2016,32(1):127-134.
[33]HIESINGER H,JAUMANN R,NEUKUM G,et al.Ages of mare basalts on the lunar nearside[J].Journal of Geophysical Research,2000,105(1959):15-41.
[34]LAWRENCE S J,STOPAR J D,OSTRACH L R,et al.Remote sensing and geologic studies of Mare Australe:the North Australe region[C]∥The Woodlands.Houston,Texas,USA:LPSC,2017:1844.
[35]NELSON D M,KOEBER S D,DAUD K,et al.Mapping lunar maria extents and lobate scarps using LROC image products[C]∥The Woodlands.Houston,Texas,USA:LP-SC,2014:2861.
[36]LAWRENCE S J,STOPAR J D,JOLLIFF B L,et al.Characterizing mare deposits in the Australe region[C]∥The Woodlands.Houston,Texas,USA:LPSC,2015:2739.
[37]李珂,陈建平.基于撞击坑自动识别的月球雨海北部地区(LQ-4)月海玄武岩定年研究[J].地学前缘,2012,19(6):47-59.
[38]HIESINGER H,JAUMANN R,NEUKUM G,et al.Mare Australe:new results from Lunar Orbiter and Clementine UV/VIS Imagery[C]∥The woodlands.Houston,Texas,USA:LPSC,1996:545-546.
[39]SPUDIS P D.The geology of multi-ring impact basins[M].Cambridge:Cambridge University Press,1993.
[40]GREELEY R.Modes of emplacement of basalt terrains and an analysis of mare volcanism in the Orientale Basin[C]∥The Woodlands.Houston,Texas,USA:LPSC,1976:2747-2759.
[2]SOLOMON S C,HEAD J W.Lunar Mascon Basins:lava filling,tectonics,and evolution of the lithosphere[J].Reviews of Geophysics&Space Physics,1980,18(1):107-141.
[3]DEHON R A.Thickness of western mare basalts[C]∥The Woodlands.Tou Texas,USA:LPSC,1979:2935-2955.
[4]WHITFORDSTARK J L.Charting the Southern Seas:the evolution of the Lunar Mare Australe[J].Lunar&Planetary,1979,10:2975-2994.
[5]HEAD J W.Lava flooding of ancient planetary crusts:geometry,thickness,and volumes of flooded lunar impact basins[J].Moon&the Planets,1982,26(1):61-88.
[6]YINGST R A,HEAD J W.Volumes of lunar lava ponds in South Pole-Aitken and Orientale Basins:implications for eruption conditions transport mechanisms,and magma source regions[J].Journal of Geophysical Research,1997,102(E5):10909-10931.
[7]BUDNEY C J,LUCEY P G.Basalt thickness in Mare Humorum:the crater excavation method[J].Journal of Geophysical Research Planets,1998,103(E7):16855-16870.
[8]HIESINGER H,HEAD J W,WOLF U,et al.Lunar mare basalt flow units:thicknesses determined from crater sizefrequency distributions[J].Geophysical Research Letters,2002,29(8):891-894.
[9]THOMSON B J,GROSFILS E B,BUSSEY D B J,et al.Anew technique for estimating the thickness of mare basalts in Imbrium Basin[J].Geophysical Research Letters,2009,36,L12201.
[10]TALWANI M,THOMPSON G,DENT B,et al.Traverse gravimeter experiment[C]∥Apollo 17:preliminary science report.Washington DC:NASA,1973:13.
[11]SHARPTON V L,HEAD J W.Stratigraphy and structural evolution of Southern Mare Serenitatis:a reinterpretation based on Apollo Lunar Sounder experiment data[J].Journal of Geophysical Research:Solid Earth,1982,87(B13):10983-10998.
[12]刘万崧,陈圣波,于岩,等.月球风暴洋地区玄武岩厚度的重力研究[J].地学前缘,2014,21(6):102-106.
[13]EVANS A J,SODERBLOM J M,ANDREWS-HANNA JC,et al.Identification of buried lunar impact craters from GRAIL data and implications for the nearside maria[J].Geophysical Research Letters,2016,43(6):486-494.
[14]GONG S,WIECZOREK M A,NIMMO F,et al.Thicknesses of mare basalts on the Moon from gravity and topography[J].Journal of Geophysical Research Planets,2016,121(5):854-870.
[15]陈媛,蒋云,张迅与,等.雨海晚期玄武岩的规模研究[J].中国科学:物理学力学天文学,2016,46(2):29604.
[16]WILHELMS D E,MCCAULEY J F,TRASK N J.The geologic history of the Moon[M].Washington DC:US Geological Survey,1987.
[17]GILLIS J J,JOLLIFF B L.An analysis of remotely sensed data of Mare Australe[R]∥The Moon beyond 2002:next steps in lunar science and exploration.New Mexico:Lunar and Planetary Institute,2002.
[18]STUART-ALEXANDER D E,HOWARD K A.Lunar Maria and circular basins:a review[J].Icarus,1970,12(3):440-456.
[19]WILHELMS D E,EL-BAZ F.Geologic map of the eastern limb of the Moon[CM]∥USGS Map I-948.Washington DC:Department of the Interior United States Geological Survey,1977:134-157.
[20]GILLIS J J.The composition and geologic setting of mare deposits on the far side of the Moon[D].Houston,Texas:Rice University,1998.
[21]ROBINSON M S,BRYLOW S M,TSCHIMMEL M,et al.Lunar Reconnaissance Orbiter Camera(LROC)instrument overview[J].Space Science Reviews,2010,150(1/2/3/4):81-124.
[22]SMITH D E,ZUBER M T,NEUMANN G A,et al.Initial observations from the Lunar Orbiter Laser Altimeter(LOLA)[J].Geophysical Research Letters,2015,37(18):109-118.
[23]NOZETTE S,RUSTAN P,PLEASANCE L P,et al.The Clementine mission to the Moon:scientific overview[J].Science,1994,266(5192):1835-1839.
[24]LUCEY P G,BLEWETT D T,JOLLIFF B L.Lunar iron and titanium abundance algorithms based on final processing of Clementine ultraviolet-visible images[J].Journal of Geophysical Research Atmospheres,2000,105(E8):20297-20305.
[25]WILLIAMS K K,ZUBER M T.Measurement and analysis of lunar basin depths from Clementine altimetry[J].Icarus,1998,131(1):107-122.
[26]CROFT S K.Cratering flow fields:implications for the excavation and transient expansion stages of crater formation[C]∥The Woodlands.Texas,USA:LPSC,1980:2347-2378.
[27]MELOSH H J.Impact cratering:ageologic process[M].Oxford:Oxford University Press,1989.
[28]LOSIAK A,WILHELMS D E,BYRNE C J,et al.A new lunar impact crater database[C]∥The Woodlands.Houston,Texas,USA:LPSC,2009:1532.
[29]KALYNN J,JOHNSON C L,OSINSKI G R,et al.Topographic characterization of lunar complex craters[J].Geophysical Research Letters,2013,40(1):38-42.
[30]凌宗成,刘建忠,张江,等.基于“嫦娥一号”干涉成像光谱仪数据的月球岩石类型填图:以月球雨海-冷海地区(LQ-4)为例[J].地学前缘,2014,21(6):107-120.
[31]籍进柱,刘建忠,张莉,等.云海地区月海玄武岩厚度估算[C]∥“月球·行星·科学与探测”学术研讨会论文集.贵阳:中国科学院地球化学研究所,2014:48-50.
[32]籍进柱,刘建忠,郭弟均,等.云海撞击盆地的恢复及其地质演化研究[J].岩石学报,2016,32(1):127-134.
[33]HIESINGER H,JAUMANN R,NEUKUM G,et al.Ages of mare basalts on the lunar nearside[J].Journal of Geophysical Research,2000,105(1959):15-41.
[34]LAWRENCE S J,STOPAR J D,OSTRACH L R,et al.Remote sensing and geologic studies of Mare Australe:the North Australe region[C]∥The Woodlands.Houston,Texas,USA:LPSC,2017:1844.
[35]NELSON D M,KOEBER S D,DAUD K,et al.Mapping lunar maria extents and lobate scarps using LROC image products[C]∥The Woodlands.Houston,Texas,USA:LP-SC,2014:2861.
[36]LAWRENCE S J,STOPAR J D,JOLLIFF B L,et al.Characterizing mare deposits in the Australe region[C]∥The Woodlands.Houston,Texas,USA:LPSC,2015:2739.
[37]李珂,陈建平.基于撞击坑自动识别的月球雨海北部地区(LQ-4)月海玄武岩定年研究[J].地学前缘,2012,19(6):47-59.
[38]HIESINGER H,JAUMANN R,NEUKUM G,et al.Mare Australe:new results from Lunar Orbiter and Clementine UV/VIS Imagery[C]∥The woodlands.Houston,Texas,USA:LPSC,1996:545-546.
[39]SPUDIS P D.The geology of multi-ring impact basins[M].Cambridge:Cambridge University Press,1993.
[40]GREELEY R.Modes of emplacement of basalt terrains and an analysis of mare volcanism in the Orientale Basin[C]∥The Woodlands.Houston,Texas,USA:LPSC,1976:2747-2759.
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