Oxygen(O_(2))is essential for life support and rocket propulsion in Mars exploration missions,and in situ oxygen production from the Martian atmosphere is of profound scientific and engineering significance.In this ar...Oxygen(O_(2))is essential for life support and rocket propulsion in Mars exploration missions,and in situ oxygen production from the Martian atmosphere is of profound scientific and engineering significance.In this article,we propose a novel method for O_(2) production from the Martian atmosphere by using glow discharge ionization combined with a self-developed oxygen-permeable membrane(OPM).Experiments under simulated Martian atmospheric conditions examined parameter impacts on the O_(2) production rate and assessed the operating characteristics and glow discharge plasma tolerance of the OPM.Results indicate that(1)the proportion of O_(2) produced positively correlates with the ionization voltage under fixed discharge electrode spacing,pressure,and flow rate,reaching a maximum of 8.18%(saturating at 4600–5400 V);(2)O_(2) yield rises with the carbon dioxide(CO_(2))flow rate at a constant pressure,with the maximum value reaching 0.5 g/h;(3)titanium(Ti)and molybdenum(Mo)electrodes exhibit higher application potential under high voltage conditions;(4)the OPM operates at temperatures above 800℃ and shows few changes in the main body sections after 24 h of plasma tolerance testing.This study lays the foundation for future development of a mature Mars oxygen production prototype with lower energy consumption and higher efficiency.展开更多
The Martian core mainly contains iron,nickel and some light elements.However,controversies remain about the structure and chemical composition of the Martian core due to a lack of samples and marsquake data.Recently,t...The Martian core mainly contains iron,nickel and some light elements.However,controversies remain about the structure and chemical composition of the Martian core due to a lack of samples and marsquake data.Recently,the InSight lander collected long-term marsquake data,which improved the Martian interior structure model.B ased on the preliminary analysis of marsquake data,Mars has a molten liquid core with a radius of around 1700 km.As the Martian core has a smaller density and lower temperature than pure iron at corresponding pressure and temperature conditions,some light elements are introduced to reduce the density and liquidus temperature.With various methods for seismic analysis,in-situ high-pressure and high-temperature experiments,and first-principal calculations,the Martian core composition and evolution models have been updated in the past few years.Here,we review those studies on the light elements in the Martian core from four aspects including(1)high-temperature and high-pressure experiments,(2)marsquake data,(3)mineral physics model with molecular dynamics simulations and(4)cosmochemistry investigation.We discussed the effect of different light elements on the Martian core s density,sound velocity and liquidus temperature.Moreover,the review examines the varieties,abundances and forms of light elements in the Martian core.展开更多
The dust cycle is a crucial component of the present-day Martian climate system.This study examines its multitimescale variability using an optimized 50-year simulation with the fully interactive scheme from the Globa...The dust cycle is a crucial component of the present-day Martian climate system.This study examines its multitimescale variability using an optimized 50-year simulation with the fully interactive scheme from the Global Open Planetary Atmospheric Model for Mars(GoMars),a newly developed Mars General Circulation Model(MGCM).GoMars is able to reproduce the diurnal,seasonal,and interannual characteristics of the dust cycle in several key aspects,with high repeatability in diurnal and seasonal variations during non-global dust storm(non-GDS)years.The model’s“climatology”(non-GDS years ensemble mean)captures the seasonal pattern and magnitude of the vertical–meridional dust distribution,validated against Mars Climate Database and Mars Climate Sounder observations.In the absence of direct observations,the GoMars-simulated near-surface wind stress lifting flux is evaluated through comparisons with other MGCMs(e.g.,MarsWRF),revealing consistent seasonal and spatial patterns.As for the diurnal cycle,the peak dust devil lifting flux occurs at 1200–1300 local time,matching the Mars Pathfinder measurements.The model also successfully captures the intense dust devil activity in Amazonis,a region identified as a major dust devil hotspot based on observational data.In GDS years,GoMars effectively reproduces spontaneous GDSs,capturing their observed onset times,locations,and dust transport patterns as exhibited in specific Martian years.The model also simulates significant interannual variability,with irregular GDS intervals along with reasonable dust–atmosphere interactions.展开更多
Methane is considered a potential biosignature gas.The Mars Science Laboratory(MSL)Curiosity rover has observed seasonal variations in atmospheric methane within Gale Crater,suggesting possible microbial activity.The ...Methane is considered a potential biosignature gas.The Mars Science Laboratory(MSL)Curiosity rover has observed seasonal variations in atmospheric methane within Gale Crater,suggesting possible microbial activity.The origin of this methane could be either biological or abiotic or a combination of the two.Different physical mechanisms,involving distinct environmental variables,produce varying concentrations of methane.By analyzing the influence of various environmental variables on methane partial pressures and comparing differences between physical models and empirical measurements,we can better discern methane production mechanisms.This study investigates factors affecting methane cycling.We find that temperature and pressure strongly correlate with Martian atmospheric methane,while Ultraviolet(UV)radiation at the atmospheric boundary and surface UV radiation exhibit weaker correlations.Using Fuller’s method,we successfully reproduce the seasonal methane cycle in Gale Crater.Several potential physical models suggest that gas diffusion driven by variations in pressure and temperature within the shallow subsurface regolith may represent a primary mechanism determining methane concentrations observed in Gale Crater.However,errors in the pressure-dominated model cannot be neglected.As Curiosity enters its uphill exploration phase,we suggest that atmospheric pressure will play a significant role in predicting the methane concentrations that it will detect.展开更多
类火星地貌识别分类旨在通过分析类火星地貌图像,模拟研究火星环境,对火星形成演化及潜在宜居环境探索等科学问题具有重要研究意义。针对目前火星地貌分类算法难以平衡模型分类效果和轻量化程度的问题,提出一种轻量化类火星地貌快速识...类火星地貌识别分类旨在通过分析类火星地貌图像,模拟研究火星环境,对火星形成演化及潜在宜居环境探索等科学问题具有重要研究意义。针对目前火星地貌分类算法难以平衡模型分类效果和轻量化程度的问题,提出一种轻量化类火星地貌快速识别分类方法(Lightweight Rapid Recognition and Classification for Mars Analog Terrain,LWNet),构建双分支教师-学生网络,利用知识蒸馏技术减少模型参数量与计算量,并嵌入注意力机制提高对地貌类型的分类识别能力,实现分类模型的高精度和轻量化。为验证所提方法的分类性能表现,通过采集地球上相似地貌,构建了包括悬崖断面、沙漠、河道及雅丹在内的4种典型类火星地貌数据集,每种地貌类型各获取800张图像,用于LWNet开展快速识别分类实验。结果表明,LWNet总体分类精度达到97.81%,相较于精度最高的Swin-Transformer仅下降了1.25%,而其参数量和计算量却只有Swin-Transformer的1.3%和4.8%,验证了所提轻量化类火星地貌快速识别分类方法的有效性和优越性。展开更多
基金supported by the Open Fund of the National Key Laboratory of Deep Space Exploration(No.NKDSEL2024004-2)the National Natural Science Foundation of China(No.42173045)supported by the Shandong Provincial Natural Science Foundation(No.ZR2025QC448).
文摘Oxygen(O_(2))is essential for life support and rocket propulsion in Mars exploration missions,and in situ oxygen production from the Martian atmosphere is of profound scientific and engineering significance.In this article,we propose a novel method for O_(2) production from the Martian atmosphere by using glow discharge ionization combined with a self-developed oxygen-permeable membrane(OPM).Experiments under simulated Martian atmospheric conditions examined parameter impacts on the O_(2) production rate and assessed the operating characteristics and glow discharge plasma tolerance of the OPM.Results indicate that(1)the proportion of O_(2) produced positively correlates with the ionization voltage under fixed discharge electrode spacing,pressure,and flow rate,reaching a maximum of 8.18%(saturating at 4600–5400 V);(2)O_(2) yield rises with the carbon dioxide(CO_(2))flow rate at a constant pressure,with the maximum value reaching 0.5 g/h;(3)titanium(Ti)and molybdenum(Mo)electrodes exhibit higher application potential under high voltage conditions;(4)the OPM operates at temperatures above 800℃ and shows few changes in the main body sections after 24 h of plasma tolerance testing.This study lays the foundation for future development of a mature Mars oxygen production prototype with lower energy consumption and higher efficiency.
基金financially supported by the National Natural Science Foundation of China(grant no.42120104005)Guizhou Provincial 2021 Science and Technology Subsidies(grant no.GZ2021SIG)+1 种基金Guizhou Provincial Science and Technology Projects(grant nos.ZK[2024]087GCC[2023]060)。
文摘The Martian core mainly contains iron,nickel and some light elements.However,controversies remain about the structure and chemical composition of the Martian core due to a lack of samples and marsquake data.Recently,the InSight lander collected long-term marsquake data,which improved the Martian interior structure model.B ased on the preliminary analysis of marsquake data,Mars has a molten liquid core with a radius of around 1700 km.As the Martian core has a smaller density and lower temperature than pure iron at corresponding pressure and temperature conditions,some light elements are introduced to reduce the density and liquidus temperature.With various methods for seismic analysis,in-situ high-pressure and high-temperature experiments,and first-principal calculations,the Martian core composition and evolution models have been updated in the past few years.Here,we review those studies on the light elements in the Martian core from four aspects including(1)high-temperature and high-pressure experiments,(2)marsquake data,(3)mineral physics model with molecular dynamics simulations and(4)cosmochemistry investigation.We discussed the effect of different light elements on the Martian core s density,sound velocity and liquidus temperature.Moreover,the review examines the varieties,abundances and forms of light elements in the Martian core.
基金jointly supported by the National Natural Science Foundation of China(Grant No.42475135)the Key Technology Research Project of TW-3(TW3006)the IAP’s basic scientific research project during the 14th Five-Year Plan Period.
文摘The dust cycle is a crucial component of the present-day Martian climate system.This study examines its multitimescale variability using an optimized 50-year simulation with the fully interactive scheme from the Global Open Planetary Atmospheric Model for Mars(GoMars),a newly developed Mars General Circulation Model(MGCM).GoMars is able to reproduce the diurnal,seasonal,and interannual characteristics of the dust cycle in several key aspects,with high repeatability in diurnal and seasonal variations during non-global dust storm(non-GDS)years.The model’s“climatology”(non-GDS years ensemble mean)captures the seasonal pattern and magnitude of the vertical–meridional dust distribution,validated against Mars Climate Database and Mars Climate Sounder observations.In the absence of direct observations,the GoMars-simulated near-surface wind stress lifting flux is evaluated through comparisons with other MGCMs(e.g.,MarsWRF),revealing consistent seasonal and spatial patterns.As for the diurnal cycle,the peak dust devil lifting flux occurs at 1200–1300 local time,matching the Mars Pathfinder measurements.The model also successfully captures the intense dust devil activity in Amazonis,a region identified as a major dust devil hotspot based on observational data.In GDS years,GoMars effectively reproduces spontaneous GDSs,capturing their observed onset times,locations,and dust transport patterns as exhibited in specific Martian years.The model also simulates significant interannual variability,with irregular GDS intervals along with reasonable dust–atmosphere interactions.
基金supported by the National Natural Science Foundation of China NSFC(Grant No.42330602,42275139)the National Key Research and Development Program of China(Grant No.2024YFF0809401)+2 种基金the Anhui Provincial Natural Science Foundation(Grant No.2208085UQ02)Innovation Center for Fengyun Meteorological Satellite Special Project(Grant No.FY-APP-ZX-2022.0211)the Joint Laboratory of Fengyun Remote Sensing.
文摘Methane is considered a potential biosignature gas.The Mars Science Laboratory(MSL)Curiosity rover has observed seasonal variations in atmospheric methane within Gale Crater,suggesting possible microbial activity.The origin of this methane could be either biological or abiotic or a combination of the two.Different physical mechanisms,involving distinct environmental variables,produce varying concentrations of methane.By analyzing the influence of various environmental variables on methane partial pressures and comparing differences between physical models and empirical measurements,we can better discern methane production mechanisms.This study investigates factors affecting methane cycling.We find that temperature and pressure strongly correlate with Martian atmospheric methane,while Ultraviolet(UV)radiation at the atmospheric boundary and surface UV radiation exhibit weaker correlations.Using Fuller’s method,we successfully reproduce the seasonal methane cycle in Gale Crater.Several potential physical models suggest that gas diffusion driven by variations in pressure and temperature within the shallow subsurface regolith may represent a primary mechanism determining methane concentrations observed in Gale Crater.However,errors in the pressure-dominated model cannot be neglected.As Curiosity enters its uphill exploration phase,we suggest that atmospheric pressure will play a significant role in predicting the methane concentrations that it will detect.
文摘类火星地貌识别分类旨在通过分析类火星地貌图像,模拟研究火星环境,对火星形成演化及潜在宜居环境探索等科学问题具有重要研究意义。针对目前火星地貌分类算法难以平衡模型分类效果和轻量化程度的问题,提出一种轻量化类火星地貌快速识别分类方法(Lightweight Rapid Recognition and Classification for Mars Analog Terrain,LWNet),构建双分支教师-学生网络,利用知识蒸馏技术减少模型参数量与计算量,并嵌入注意力机制提高对地貌类型的分类识别能力,实现分类模型的高精度和轻量化。为验证所提方法的分类性能表现,通过采集地球上相似地貌,构建了包括悬崖断面、沙漠、河道及雅丹在内的4种典型类火星地貌数据集,每种地貌类型各获取800张图像,用于LWNet开展快速识别分类实验。结果表明,LWNet总体分类精度达到97.81%,相较于精度最高的Swin-Transformer仅下降了1.25%,而其参数量和计算量却只有Swin-Transformer的1.3%和4.8%,验证了所提轻量化类火星地貌快速识别分类方法的有效性和优越性。
