湖冰是冰冻圈水文学的重要研究对象,湖冰的生消对气候变化极其敏感,可以作为气候变化的指示因子,并通过影响湖泊与大气之间的物质能量交换,调节区域气候和湖泊生态系统。湖冰厚度是研究湖冰生消过程的关键变量,明晰其生消特征对于揭示气候变化下湖泊响应过程具有重要的理论价值和现实意义。本文以内蒙古南湖湖冰为研究对象,基于2013—2017年和2022—2023年原型测冰数据,利用ERA5-Land再分析数据作为大气强迫场,通过SIMSTRAT湖泊过程模型重建2003—2022年内蒙古南湖完整冰厚生消过程并分析其变化特征。结果表明:1) SIMSTRAT模型模拟与原型观测得到的初冰日和终冰日平均偏差为3.40 d,冰厚数据平均偏差为1.29 cm,平均绝对误差为1.29 cm,均方根误差为1.90 cm。模拟结果与现场观测结果具有较高的一致性。2)2003—2022年南湖封冻期平均持续119 d,冰厚生长期、平衡期、融化期平均日数分别为64、34、21d。南湖封冻期整体呈缩短趋势,缩短率为4.27 d/10 a;其中,融化期年际变化幅度较大,缩短率为3.67 d/10 a。3)近20年,南湖年均冰厚介...

湖冰是冰冻圈水文学的重要研究对象,湖冰的生消对气候变化极其敏感,可以作为气候变化的指示因子,并通过影响湖泊与大气之间的物质能量交换,调节区域气候和湖泊生态系统。湖冰厚度是研究湖冰生消过程的关键变量,明晰其生消特征对于揭示气候变化下湖泊响应过程具有重要的理论价值和现实意义。本文以内蒙古南湖湖冰为研究对象,基于2013—2017年和2022—2023年原型测冰数据,利用ERA5-Land再分析数据作为大气强迫场,通过SIMSTRAT湖泊过程模型重建2003—2022年内蒙古南湖完整冰厚生消过程并分析其变化特征。结果表明:1) SIMSTRAT模型模拟与原型观测得到的初冰日和终冰日平均偏差为3.40 d,冰厚数据平均偏差为1.29 cm,平均绝对误差为1.29 cm,均方根误差为1.90 cm。模拟结果与现场观测结果具有较高的一致性。2)2003—2022年南湖封冻期平均持续119 d,冰厚生长期、平衡期、融化期平均日数分别为64、34、21d。南湖封冻期整体呈缩短趋势,缩短率为4.27 d/10 a;其中,融化期年际变化幅度较大,缩短率为3.67 d/10 a。3)近20年,南湖年均冰厚介...

湖冰是冰冻圈水文学的重要研究对象,湖冰的生消对气候变化极其敏感,可以作为气候变化的指示因子,并通过影响湖泊与大气之间的物质能量交换,调节区域气候和湖泊生态系统。湖冰厚度是研究湖冰生消过程的关键变量,明晰其生消特征对于揭示气候变化下湖泊响应过程具有重要的理论价值和现实意义。本文以内蒙古南湖湖冰为研究对象,基于2013—2017年和2022—2023年原型测冰数据,利用ERA5-Land再分析数据作为大气强迫场,通过SIMSTRAT湖泊过程模型重建2003—2022年内蒙古南湖完整冰厚生消过程并分析其变化特征。结果表明:1) SIMSTRAT模型模拟与原型观测得到的初冰日和终冰日平均偏差为3.40 d,冰厚数据平均偏差为1.29 cm,平均绝对误差为1.29 cm,均方根误差为1.90 cm。模拟结果与现场观测结果具有较高的一致性。2)2003—2022年南湖封冻期平均持续119 d,冰厚生长期、平衡期、融化期平均日数分别为64、34、21d。南湖封冻期整体呈缩短趋势,缩短率为4.27 d/10 a;其中,融化期年际变化幅度较大,缩短率为3.67 d/10 a。3)近20年,南湖年均冰厚介...

湖冰是冰冻圈水文学的重要研究对象,湖冰的生消对气候变化极其敏感,可以作为气候变化的指示因子,并通过影响湖泊与大气之间的物质能量交换,调节区域气候和湖泊生态系统。湖冰厚度是研究湖冰生消过程的关键变量,明晰其生消特征对于揭示气候变化下湖泊响应过程具有重要的理论价值和现实意义。本文以内蒙古南湖湖冰为研究对象,基于2013—2017年和2022—2023年原型测冰数据,利用ERA5-Land再分析数据作为大气强迫场,通过SIMSTRAT湖泊过程模型重建2003—2022年内蒙古南湖完整冰厚生消过程并分析其变化特征。结果表明:1) SIMSTRAT模型模拟与原型观测得到的初冰日和终冰日平均偏差为3.40 d,冰厚数据平均偏差为1.29 cm,平均绝对误差为1.29 cm,均方根误差为1.90 cm。模拟结果与现场观测结果具有较高的一致性。2)2003—2022年南湖封冻期平均持续119 d,冰厚生长期、平衡期、融化期平均日数分别为64、34、21d。南湖封冻期整体呈缩短趋势,缩短率为4.27 d/10 a;其中,融化期年际变化幅度较大,缩短率为3.67 d/10 a。3)近20年,南湖年均冰厚介...

The particle breakage effect in sand exerts a significant influence on the design of underground space structure. However, the existing theories seldom consider the breakage effect and often lack accurate descriptions of void ratio changes, leading to substantial errors in the numerical calculations compared to the actual scenario. This study employs the simple critical state sand model (SIMSAND) to account for the particle breakage effect and transforms the drained cylindrical cavity expansion problem into a set of first-order ordinary differential equations described by the Lagrangian method. The analytical solution of the cylindrical cavity expansion problem is calculated using Matlab programming codes. Firstly, Fontainebleau sand is investigated to analyse the influence of initial stress, void ratio and specific volume around the cavity. The combined effects of initial stress and particle breakage on the soil around the cavities result in dilatancy characteristics and a reduction in void ratio. The stress path analysis reveals that the soil around the cavities only reaches a critical state under high initial stresses. Secondly, a plane strain numerical model is established for twice expansion to verify the calculation outcomes from the cylindrical cavity expansion theory. Finally, an axisymmetric cone penetration test (CPT) model is developed to analyse the theoretical and numerical solutions for expansion stress and sleeve friction. The research results indicate that the CPT in sand need to consider the particle breakage effect, especially under high stress conditions. Without considering particle breakage, the sleeve friction is overestimated. These research findings can offer guidance for geotechnical engineering applications, such as CPT, pressuremeter tests and predictions of bearing capacity for pile foundations in sand. Based on the cavity expansion theory and numerical simulations, particle breakage effect of sand is studied. The findings reveal that neglecting the particle breakage effect leads to a marked increase in the calculation results.image

The isotopes of chlorine (Cl-37 and Cl-35) are highly fractionated in lunar samples compared to most other Solar System materials. Recently, the chlorine isotope signatures of lunar rocks have been attributed to large-scale degassing processes that occurred during the existence of a magma ocean. In this study we investigated how well a suite of lunar basalts, most of which have not previously been analyzed, conform to previous models. The Cl isotope compositions (delta Cl-37 (parts per thousand) = [(Cl-37/Cl-35(sample)/Cl-37/Cl-35(SMOC)) - 1] x 1000, where SMOC refers to standard mean ocean chloride) recorded range from similar to+7 to +14 parts per thousand (Apollo 15), +10 to +19 parts per thousand (Apollo 12), +9 to +15 parts per thousand (70017), +4 to +8 parts per thousand (MIL 05035), and +15 to +22 parts per thousand (Kalahari 009). The Cl isotopic data from the present study support the mixing trends previously reported by Boyce et al. (2015) and Barnes et al. (2016), as the Cl isotopic composition of apatites are positively correlated with bulk-rock incompatible trace element abundances in the low-Ti basalts, inclusive of low-Ti and KREEP basalts. This trend has been interpreted as evidence that incompatible trace elements, including Cl, were concentrated in the urKREEP residual liquid of the lunar magma ocean, rather than the mantle cumulates, and that urKREEP Cl had a highly fractionated isotopic composition. The source regions for the basalts were thus created by variable mixing between the mantle (Cl-poor and relatively unfractionated) and urKREEP. The high-Ti basalts show much more variability in measured Cl isotope ratios and scatter around the trend formed by the low-Ti basalts. Most of the data for lunar meteorites also fits the mixing of volatiles in their sources, but Kalahari 009, which is highly depleted in incompatible trace elements, contains apatites with heavily fractionated Cl isotopic compositions. Given that Kalahari 009 is one of the oldest lunar basalts and ought to have been derived from very early-formed mantle cumulates, a heavy Cl isotopic signature is likely not related to its mantle source, but more likely to magmatic or secondary alteration processes, perhaps via impact-driven vapor metasomatism of the lunar crust. (C) 2019 The Authors. Published by Elsevier Ltd.

While it is now recognized that the Moon has indigenous water and volatiles, their total abundances are unclear, with current literature estimates ranging from nearly absent to Earth-like levels. Similarly unconstrained is the source of the Moon's water, which could be cometary, chondritic, or the primordial nebula. Here we measure H2O and D/H in olivine-hosted melt inclusions in lunar mare basalts 12018, 12035, and 12040, part of the consanguineous suite of Apollo 12 olivine basalts that differ primarily because of cooling rate (Walker et al., 1976). We find that the water contents are higher in the more rapidly cooled 12018 (62-740 ppm H2O) compared to the more slowly cooled basalts 12035 (28-156 ppm H2O) and 12040 (27-90 ppm H2O), suggesting that lunar basalts may have been dehydrating during slow cooling. D/H is similar in the olivine-hosted melt inclusions in all three samples, and indistinguishable from terrestrial water (dD = -183 +/- 212% to + 138 +/- 61%). When we compare the D/H of olivine-hosted melt inclusions to D/H of apatite in the same samples, the evolution of dD and water content can be better constrained. We propose that lunar magmas first exchange hydrogen with a low D/H reservoir during cooling, and then ultimately lose their water during extended subsolidus cooling. Due to high diffusion rates of hydrogen in olivine, it is likely that all basaltic olivine-hosted melt inclusions from the Moon exchanged hydrogen with a low D/H reservoir in near-surface magma chambers or lava flows. The most likely source of the low D/H reservoir on the Moon is the lunar regolith, which is known to have a significant solar wind hydrogen component.

In situ measurement of Moon-originating ions picked-up I in orbit round the Moon is expected to provide valuable information regarding the thin lunar atmosphere and surface. Secondary ions sputtered by the solar wind ions reflect the surface abundance. Global composition mapping of the lunar surface may be thus achieved by measuring the sputtered ions as one would perform laboratory SIMS. We studied the dynamics of picked-up lunar ions when the Moon was exposed to the solar wind. Our model's source mechanism involved photoionization of the lunar exospheric atoms, photon-stimulated ion desorption, and ion sputtering. We propose that an intense flux of picked-up lunar ions (10(4)/cm(2)-sec) exists at an altitude of 100 km, for nearly a quarter of the orbit. The ion flux originating from the lunar surface is mono-directional and mono-energetic, and is distinguishable from that of lunar atmospheric origin whose energy spectra correspond to their spatial distribution. Our calculation suggested that ion measurements in orbit round the Moon enable remote SIMS analyses.