Magma eruption ages and fluxes in the Rembrandt and Caloris interior plains on Mercury: Implications for the north-south smooth plains asymmetry
Magma eruption ages and fluxes in the Rembrandt and Caloris interior plains on Mercury: Implications for the north-south smooth plains asymmetry
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水星伦勃朗和卡洛里斯内陆平原的岩浆喷发年龄和通量：对南北平滑平原不对称性的影响
DOI：
10.1016/j.icarus.2022.115034
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发表时间：
2022
期刊：
影响因子：
3.2
通讯作者：
Usui Tomohiro
中科院分区：
文献类型：
--
作者：
Hirata Kaori;Morota Tomokatsu;Sugita Seiji;Ernst Carolyn M.;Usui Tomohiro
美国国家航空航天局的水星表面、空间环境、地球化学和测距（信使）使命显示，水星表面约27%被可能由岩浆喷发形成的平滑平原所占据。这些平滑的平原单元大多位于撞击盆地的地面上;这些平原在北方半球的表面积大约是南半球的7倍。这表明地幔的热条件和/或两个半球之间岩浆喷发的难易程度存在差异。这项研究重新估计岩浆喷发的年龄和体积内的伦勃朗和Caloris盆地，这些是代表性的影响盆地在南半球和北方半球，分别。通过测量火山口的大小-频率分布和部分掩埋的火山口的直径，对喷发年龄和喷发量进行了估计。采用孔隙-靶体年代学模型估算了伦勃朗盆地和卡洛里斯盆地的形成和喷发年龄;其形成年龄分别为3.93 ± 0.06和3.94 ± 0.04戈伊，其发疹年龄分别为3.87 ± 0.04 ~ 3.76 ± 0.01戈伊和3.88 ± 0.03 ~ 3.74 ± 0.01戈伊，分别在这两个盆地中观察到的火山口的大小频率分布可能会显示多个重新浮出水面的幕式喷发，建议由以前的数值模拟水星热演化。Caloris盆地的岩浆喷发通量（9.3-15.1 km/戈伊）最大，是伦勃朗盆地（5.2-12.3 km/戈伊）的3倍。考虑到它更大的直径，Caloris盆地下面的地壳可能比伦勃朗盆地下面的地壳薄1.8倍。这将使岩浆更容易上升到Caloris下面的表面，而不是伦勃朗下面的表面;因此，两个盆地下面地幔中的岩浆生产量不应该相差小于3倍。这些结果表明，水星地幔和下地壳中产热元素的丰度没有大的空间变化，这与月球近侧产热元素的浓度不同。
The MErcury Surface, Space ENvironment, GEochemistry and Ranging (MESSENGER) mission by the National Aeronautics and Space Administration revealed that ~27% of the surface of Mercury is occupied by smooth plains potentially formed by magma eruptions. Most of these smooth plain units are located on the floors of the impact basins; these plains occupy a surface area that is approximately seven times larger in the northern hemisphere than in the southern hemisphere. This suggests a difference in thermal conditions in the mantle and/or the ease of magma eruption between hemispheres. This study re-estimated magma eruption ages and volumes within the Rembrandt and Caloris basins; these are representative impact basins in the southern and northern hemispheres, respectively. The estimations of eruption ages and volumes were carried out by measuring crater size-frequency distributions and the diameters of partially buried craters. The formation and eruption ages of the Rembrandt and the Caloris basins were estimated by adopting the porous-target chronology model; the formation ages were estimated as 3.93 ± 0.06 and 3.94 ± 0.04 Gy, while their eruption ages were from 3.87 ± 0.04 to 3.76 ± 0.01 Gy and 3.88 ± 0.03 to 3.74 ± 0.01 Gy, respectively. The observed crater size-frequency distributions in both basins might show multiple resurfacing from episodic eruptions, as suggested by previous numerical simulations of Mercurian thermal evolution. The estimated magma eruption fluxes in the Caloris basin (9.3–15.1 km/Gy) were at most, three times larger than that in the Rembrandt basin (5.2–12.3 km/Gy). Given its larger diameter, the crust beneath the Caloris basin is likely to be ~1.8 times thinner than the crust beneath the Rembrandt basin. This will make it easier for magma to ascend to the surface beneath Caloris than beneath Rembrandt; as such, quantities of magma production in the mantle beneath the two basins should not differ by a factor of <3. These results suggest that there are no large spatial variations in the abundance of heat-producing elements in the mantle and lower crust of Mercury unlike the concentration of heat-production elements on the nearside of the Moon.
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影响因子：
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作者：
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DOI：
--
发表时间：
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