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
Rapid and reliable onboard optimization of bank angle profiles is crucial for mitigating uncertainties during Mars atmospheric entry.This paper presents a neural-network-accelerated methodology for optimizing parametr...Rapid and reliable onboard optimization of bank angle profiles is crucial for mitigating uncertainties during Mars atmospheric entry.This paper presents a neural-network-accelerated methodology for optimizing parametric bank angle profiles in Mars atmospheric entry missions.The methodology includes a universal approach to handling path constraints and a reliable solution method based on the Particle Swarm Optimization(PSO)algorithm.For illustrative purposes,a mission with the objective of maximizing terminal altitude is considered.The original entry optimization problem is converted into optimizing three coefficients for the bank angle profiles with terminal constraints by formulating a parametric Mars entry bank angle profile and constraint handling methods.The parameter optimization problem is addressed using the PSO algorithm,with reliability enhanced by increasing the PSO swarm size.To improve computational efficiency,an enhanced Deep Operator Network(Deep ONet)is used as a dynamics solver to predict terminal states under various bank angle profiles rapidly.Numerical simulations demonstrate that the proposed methodology ensures reliable convergence with a sufficiently large PSO swarm while maintaining high computational efficiency facilitated by the neural-network-based dynamics solver.Compared to the existing methodologies,this methodology offers a streamlined process,the reduced sensitivity to initial guesses,and the improved computational efficiency.展开更多
Atmospheric escape plays a critical role in shaping the long-term climate evolution of Mars.Among the various escape mechanisms,energetic neutral atoms(ENAs)generated through charge exchange between solar wind ions an...Atmospheric escape plays a critical role in shaping the long-term climate evolution of Mars.Among the various escape mechanisms,energetic neutral atoms(ENAs)generated through charge exchange between solar wind ions and exospheric neutrals serve as an important diagnostic for ion-neutral interactions and upper atmospheric loss.This study presents direct observations of hydrogen ENAs(H-ENAs)on the dayside of Mars by using the Mars Ion and Neutral Particle Analyzer(MINPA)onboard China’s Tianwen-1 orbiter.By analyzing H-ENA data during a coronal mass ejection and a stream interaction region from December 29,2021,to January 1,2022,and comparing these data with MAVEN/SWIA(Mars Atmosphere and Volatile EvolutioN/Solar Wind Ion Analyzer)solar wind measurements,we examine the temporal evolution of H-ENA flux and the associated sputtered escape of atmospheric constituents.The observed H-ENA velocity is consistent with upstream solar wind ions,and the H-ENA-to-ion intensity ratio is used to infer variations in exospheric density,revealing a delayed response to enhanced solar wind activity.Penetrating H-ENA intensities reach up to 5.3×10^(6)s^(−1) cm^(−2),with energy fluxes on the order of(0.5-8.1)×10^(−3) mW/m^(2).The estimated oxygen sputtered escape rate driven by penetrating H-ENAs ranges from 5.5×10^(23)s^(−1) to 5.2×10^(24)s^(−1),comparable to or exceeding previous estimates based on penetrating ions.The findings highlight the need for low-altitude H-ENA observations to better quantify their atmospheric interactions and refine our understanding of nonthermal escape processes at Mars.展开更多
The polar layered deposits(PLD) of Mars can provide deep insight into paleoclimate changes over the planet's last several million years. Since the 1960s, researchers have studied almost all aspects of Martian PLD ...The polar layered deposits(PLD) of Mars can provide deep insight into paleoclimate changes over the planet's last several million years. Since the 1960s, researchers have studied almost all aspects of Martian PLD properties, searching for patterns that might reveal periodic characteristics of the planet's climate history. Although much progress has been made in our understanding of orbital periodicities reflected in the PLD, questions remain regarding how Martian orbital changes have affected the formation of the PLD and regarding the extent of climate information that is recorded in the PLD. Future studies of PLD should be carried out via integrated research that targets multi-profiles throughout the entire Martian polar regions that would clarify their general features at the hemisphere scale. Numerical modeling, coupled with modern observations of dust and water vapor transportation, should greatly advance our understanding of planetary climate evolution. Furthermore, future landing missions may help to clarify the paleoclimatic characteristics reflected in the PLD by drilling into these layered deposits and measuring mineralogical and geochemical compositions of the drilled samples.展开更多
In this study, we present an innovative Mars Ionosphere-Thermosphere Model(MITM), which is a time-dependent, threedimensional(3-D) model that comprehensively represents the self-consistently coupled thermosphere and i...In this study, we present an innovative Mars Ionosphere-Thermosphere Model(MITM), which is a time-dependent, threedimensional(3-D) model that comprehensively represents the self-consistently coupled thermosphere and ionosphere of Mars within the altitude range of 70-300 km. The model incorporates an extensive range of parameters, including neutral number densities of CO_(2), CO,O, O_(2), N_(2), NO, N(^(2)D), N(^(4)S), Ar, and He;ion number densities of CO_(2)^(+), CO^(+), O^(+), O_(2)^(+), N_(2)^(+), NO^(+), N^(+) ions, and electrons;neutral temperature;and neutral wind fields. The MITM code employs a high-resolution grid system in a spherical geographical coordinate system, with a horizontal resolution of 5° latitude by 7.5° longitude. This altitude-resolved grid system enables accurate depiction of spatial variations in the Martian thermosphere and ionosphere. To showcase the capabilities of the MITM, we present two simulation cases: one during the equinox and another during the solstice. Both simulations reproduce key features of the Martian thermosphere and ionosphere including the characteristics of horizontal circulation, diurnal variations in chemical composition, and distribution of electron density. The MITM offers a robust framework for understanding the intricate interactions and processes that shape the Mars thermosphere and ionosphere,which are crucial for enhancing our understanding of Martian upper atmosphere and ionosphere.展开更多
Magnetite-ilmenite pairs in meteorites serve as reliable thermometers and oxygen fugacity (fO_(2)) indicators for constraining both nebular conditions and thermal metamorphic histories.While CK and CV chondrites exhib...Magnetite-ilmenite pairs in meteorites serve as reliable thermometers and oxygen fugacity (fO_(2)) indicators for constraining both nebular conditions and thermal metamorphic histories.While CK and CV chondrites exhibit nearly identical petrological characteristics and oxygen isotope compositions,our analysis of NWA 16813 reveals it records the highest fO_(2)(log fO_(2)=-20.51 (589.34°C)-log fO_(2)=-14.21 (608.63°C))yet measured among these meteorites.This finding provides critical evidence that CK and CV chondrites experienced fundamentally different redox conditions during their formation.The fO_(2)data from NWA16813,combined with its distinct petrological and mineralogical features,strongly suggest that CK and CV chondrites originated from chemically separate reservoirs in the protoplanetary disk despite their apparen similarities.展开更多
Ultra-low-frequency(ULF) waves are ubiquitous in terrestrial and planetary environments, playing a crucial role in energy transfer and dissipation through wave–particle interactions within space plasmas. By performin...Ultra-low-frequency(ULF) waves are ubiquitous in terrestrial and planetary environments, playing a crucial role in energy transfer and dissipation through wave–particle interactions within space plasmas. By performing a detailed event study in terms of particle distribution maps and wave–particle variable correlation maps, we report that ULF waves observed by the Mars Atmosphere and Volatile EvolutioN(MAVEN) spacecraft in the Martian foreshock can effectively modulate the suprathermal electron fluxes by the magnetic field fluctuations. In particular, the variations in electron fluxes at energies of ~10–100 eV are significant in the perpendicular direction, showing good relationships with changes in the wave field strength characterized by a correlation coefficient ~0.8. These findings demonstrate the generality of interactions of ULF waves with electrons, even at these low energies, highlighting the importance of such processes throughout the heliosphere.展开更多
The strong crustal magnetic fields significantly alter the structure of the Martian space environment,including all plasma boundaries.The stretches of mini-magnetospheres formed by crustal fields from the location of ...The strong crustal magnetic fields significantly alter the structure of the Martian space environment,including all plasma boundaries.The stretches of mini-magnetospheres formed by crustal fields from the location of the Martian bow shocks were first found from the Mars Atmosphere and Volatile EvolutioN(MAVEN)observations.The present study aims to test whether this effect is also present in the shocks observed by Mars Express(MEX).We find that the bow shocks above the crustal field regions are enlarged,resulting in a north−south asymmetry and a longitude dependence in the shock size.The longitude dependence is more pronounced for near-subsolar shocks,and more dispersed for near-terminator shocks.The enlarged shocks are also observed to have shifted tailward from the longitudes of the strongest crustal fields.Due to a dawnside bias in MEX shock crossings,the enlarged shocks generally display a westward shift from the strongest crustal field region.These results confirm that stretches of the mini-magnetosphere are also present in the MEX shock observations.展开更多
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。
基金supported in part by the National Defense Basic Scientific Research Program of China(No.JCKY2021603B030)the Shenzhen Fundamental Research Program,China(No.JCYJ20220818102601004)the Science Center Program of National Natural Science Foundation of China(No.62188101)。
文摘Rapid and reliable onboard optimization of bank angle profiles is crucial for mitigating uncertainties during Mars atmospheric entry.This paper presents a neural-network-accelerated methodology for optimizing parametric bank angle profiles in Mars atmospheric entry missions.The methodology includes a universal approach to handling path constraints and a reliable solution method based on the Particle Swarm Optimization(PSO)algorithm.For illustrative purposes,a mission with the objective of maximizing terminal altitude is considered.The original entry optimization problem is converted into optimizing three coefficients for the bank angle profiles with terminal constraints by formulating a parametric Mars entry bank angle profile and constraint handling methods.The parameter optimization problem is addressed using the PSO algorithm,with reliability enhanced by increasing the PSO swarm size.To improve computational efficiency,an enhanced Deep Operator Network(Deep ONet)is used as a dynamics solver to predict terminal states under various bank angle profiles rapidly.Numerical simulations demonstrate that the proposed methodology ensures reliable convergence with a sufficiently large PSO swarm while maintaining high computational efficiency facilitated by the neural-network-based dynamics solver.Compared to the existing methodologies,this methodology offers a streamlined process,the reduced sensitivity to initial guesses,and the improved computational efficiency.
基金supported by the National Natural Science Foundation of China (Grant Nos. 42188101, 42274211, 41974170, 42374184, 42122032, and 41974196)the Chinese Academy of Sciences (Grant Nos. QYZDJSSW-JSC028, XDA15052500, XDA17010301, and XDB41000000)+3 种基金the CNSA (Grant No. D050103)the Specialized Research Fund for State Key Laboratories of Chinathe Specialized Research Fund for Laboratory of Geospace Environment of the University of Science and Technology of Chinasupported by the International Space Science Institute (ISSI) in Bern and Beijing through the ISSI/ISSI-BJ International Team Project titled “Understanding the Mars Space Environment Through Multi-Spacecraft Measurements” (ISSI Team Project No. 23-582 and ISSI-BJ Team Project No. 58)
文摘Atmospheric escape plays a critical role in shaping the long-term climate evolution of Mars.Among the various escape mechanisms,energetic neutral atoms(ENAs)generated through charge exchange between solar wind ions and exospheric neutrals serve as an important diagnostic for ion-neutral interactions and upper atmospheric loss.This study presents direct observations of hydrogen ENAs(H-ENAs)on the dayside of Mars by using the Mars Ion and Neutral Particle Analyzer(MINPA)onboard China’s Tianwen-1 orbiter.By analyzing H-ENA data during a coronal mass ejection and a stream interaction region from December 29,2021,to January 1,2022,and comparing these data with MAVEN/SWIA(Mars Atmosphere and Volatile EvolutioN/Solar Wind Ion Analyzer)solar wind measurements,we examine the temporal evolution of H-ENA flux and the associated sputtered escape of atmospheric constituents.The observed H-ENA velocity is consistent with upstream solar wind ions,and the H-ENA-to-ion intensity ratio is used to infer variations in exospheric density,revealing a delayed response to enhanced solar wind activity.Penetrating H-ENA intensities reach up to 5.3×10^(6)s^(−1) cm^(−2),with energy fluxes on the order of(0.5-8.1)×10^(−3) mW/m^(2).The estimated oxygen sputtered escape rate driven by penetrating H-ENAs ranges from 5.5×10^(23)s^(−1) to 5.2×10^(24)s^(−1),comparable to or exceeding previous estimates based on penetrating ions.The findings highlight the need for low-altitude H-ENA observations to better quantify their atmospheric interactions and refine our understanding of nonthermal escape processes at Mars.
基金supported financially by the Key Research Program of the Institute of Geology and Geophysics, CAS (Grant No. IGGCAS-202102 and IGGCAS-201905)。
文摘The polar layered deposits(PLD) of Mars can provide deep insight into paleoclimate changes over the planet's last several million years. Since the 1960s, researchers have studied almost all aspects of Martian PLD properties, searching for patterns that might reveal periodic characteristics of the planet's climate history. Although much progress has been made in our understanding of orbital periodicities reflected in the PLD, questions remain regarding how Martian orbital changes have affected the formation of the PLD and regarding the extent of climate information that is recorded in the PLD. Future studies of PLD should be carried out via integrated research that targets multi-profiles throughout the entire Martian polar regions that would clarify their general features at the hemisphere scale. Numerical modeling, coupled with modern observations of dust and water vapor transportation, should greatly advance our understanding of planetary climate evolution. Furthermore, future landing missions may help to clarify the paleoclimatic characteristics reflected in the PLD by drilling into these layered deposits and measuring mineralogical and geochemical compositions of the drilled samples.
基金This work is supported by the B-type Strategic Priority Program of the Chinese Academy of Sciences (Grant No. XDB4100000)the pre-research Project on Civil Aerospace Technologies No. D020105 funded by CNSAthe Strategic Priority Research Program of Chinese Academy of Sciences (Grant XDA17010404, XDA17010201)。
文摘In this study, we present an innovative Mars Ionosphere-Thermosphere Model(MITM), which is a time-dependent, threedimensional(3-D) model that comprehensively represents the self-consistently coupled thermosphere and ionosphere of Mars within the altitude range of 70-300 km. The model incorporates an extensive range of parameters, including neutral number densities of CO_(2), CO,O, O_(2), N_(2), NO, N(^(2)D), N(^(4)S), Ar, and He;ion number densities of CO_(2)^(+), CO^(+), O^(+), O_(2)^(+), N_(2)^(+), NO^(+), N^(+) ions, and electrons;neutral temperature;and neutral wind fields. The MITM code employs a high-resolution grid system in a spherical geographical coordinate system, with a horizontal resolution of 5° latitude by 7.5° longitude. This altitude-resolved grid system enables accurate depiction of spatial variations in the Martian thermosphere and ionosphere. To showcase the capabilities of the MITM, we present two simulation cases: one during the equinox and another during the solstice. Both simulations reproduce key features of the Martian thermosphere and ionosphere including the characteristics of horizontal circulation, diurnal variations in chemical composition, and distribution of electron density. The MITM offers a robust framework for understanding the intricate interactions and processes that shape the Mars thermosphere and ionosphere,which are crucial for enhancing our understanding of Martian upper atmosphere and ionosphere.
基金supported by the Science and Technology Development Fund of Macao (FDCT)(grant 002/2024/SKL)。
文摘Magnetite-ilmenite pairs in meteorites serve as reliable thermometers and oxygen fugacity (fO_(2)) indicators for constraining both nebular conditions and thermal metamorphic histories.While CK and CV chondrites exhibit nearly identical petrological characteristics and oxygen isotope compositions,our analysis of NWA 16813 reveals it records the highest fO_(2)(log fO_(2)=-20.51 (589.34°C)-log fO_(2)=-14.21 (608.63°C))yet measured among these meteorites.This finding provides critical evidence that CK and CV chondrites experienced fundamentally different redox conditions during their formation.The fO_(2)data from NWA16813,combined with its distinct petrological and mineralogical features,strongly suggest that CK and CV chondrites originated from chemically separate reservoirs in the protoplanetary disk despite their apparen similarities.
基金supported by the National Natural Science Foundation of China (Grant Nos. 42188101, 42174188, 42474217, 42330207, 42374193, 42241143, and 42025404)the National Key R&D Program of China (Grant Nos. 2022YFF0503700 and 2022YFF0503900)。
文摘Ultra-low-frequency(ULF) waves are ubiquitous in terrestrial and planetary environments, playing a crucial role in energy transfer and dissipation through wave–particle interactions within space plasmas. By performing a detailed event study in terms of particle distribution maps and wave–particle variable correlation maps, we report that ULF waves observed by the Mars Atmosphere and Volatile EvolutioN(MAVEN) spacecraft in the Martian foreshock can effectively modulate the suprathermal electron fluxes by the magnetic field fluctuations. In particular, the variations in electron fluxes at energies of ~10–100 eV are significant in the perpendicular direction, showing good relationships with changes in the wave field strength characterized by a correlation coefficient ~0.8. These findings demonstrate the generality of interactions of ULF waves with electrons, even at these low energies, highlighting the importance of such processes throughout the heliosphere.
基金supported by the National Key Research and Development Program of China(Grant No.2022YFF0503204)the National Natural Science Foundation of China(Grant No.42388101)+3 种基金Youth Innovation Promotion Association CAS(2020065)Young Elite Scientist Sponsorship Program by CAST(YESS20200152)the Key Research Program of the Institute of Geology&Geophysics,CAS(IGGCAS-202102)the Key Research Program of Chinese Academy of Sciences(Grant ZDB-SSW-TLC00103).
文摘The strong crustal magnetic fields significantly alter the structure of the Martian space environment,including all plasma boundaries.The stretches of mini-magnetospheres formed by crustal fields from the location of the Martian bow shocks were first found from the Mars Atmosphere and Volatile EvolutioN(MAVEN)observations.The present study aims to test whether this effect is also present in the shocks observed by Mars Express(MEX).We find that the bow shocks above the crustal field regions are enlarged,resulting in a north−south asymmetry and a longitude dependence in the shock size.The longitude dependence is more pronounced for near-subsolar shocks,and more dispersed for near-terminator shocks.The enlarged shocks are also observed to have shifted tailward from the longitudes of the strongest crustal fields.Due to a dawnside bias in MEX shock crossings,the enlarged shocks generally display a westward shift from the strongest crustal field region.These results confirm that stretches of the mini-magnetosphere are also present in the MEX shock observations.
