Predicting the probability distribution of Martian rocks mechanical property based on microscale rock mechanical experiments and accurate grain-based modeling

The exploration of Mars would heavily rely on Martian rocks mechanics and engineering technology.As the mechanical property of Martian rocks is uncertain,it is of utmost importance to predict the probability distribution of Martian rocks mechanical property for the success of Mars exploration.In this paper,a fast and accurate probability distribution method for predicting the macroscale elastic modulus of Martian rocks was proposed by integrating the microscale rock mechanical experiments(micro-RME),accurate grain-based modeling(AGBM)and upscaling methods based on reliability principles.Firstly,the microstructure of NWA12564 Martian sample and elastic modulus of each mineral were obtained by micro-RME with TESCAN integrated mineral analyzer(TIMA)and nanoindentation.The best probability distribution function of the minerals was determined by Kolmogorov-Smirnov(K-S)test.Secondly,based on best distribution function of each mineral,the Monte Carlo simulations(MCS)and upscaling methods were implemented to obtain the probability distribution of upscaled elastic modulus.Thirdly,the correlation between the upscaled elastic modulus and macroscale elastic modulus obtained by AGBM was established.The accurate probability distribution of the macroscale elastic modulus was obtained by this correlation relationship.The proposed method can predict the probability distribution of Martian rocks mechanical property with any size and shape samples.

Formation of Tianwen-1 landing crater and mechanical properties of Martian soil near the landing site

After landing in the Utopia Planitia,Tianwen-1 formed the deepest landing crater on Mars,approximately 40 cm deep,exposing precious information about the mechanical properties of Martian soil.We established numerical models for the plume-surface interaction(PSI)and the crater formation based on Computational Fluid Dynamics(CFD)methods and the erosion model modified from Roberts’Theory.Comparative studies of cases were conducted with different nozzle heights and soil mechanical properties.The increase in cohesion and internal friction angle leads to a decrease in erosion rate and maximum crater depth,with the cohesion having a greater impact.The influence of the nozzle height is not clear,as it interacts with the position of the Shock Diamond to jointly control the erosion process.Furthermore,we categorized the evolution of landing craters into the dispersive and the concentrated erosion modes based on the morphological characteristics.Finally,we estimated the upper limits of the Martian soil’s mechanical properties near Tianwen-1 landing site,with the cohesion ranging from 2612 to 2042 Pa and internal friction angle from 25°to 41°.

Parameter optimization for Rayleigh-Mie lidar under different dust conditions for the landing area of Martian Tianwen-1

Mars is the terrestrial planet in the solar system that is closest to the Earth.Studying the atmospheric parameters of Mars and studying the evolutionary history of the Martian environment on this basis is helpful for people to discover signs of extraterrestrial life and to study the trend of climate change on Earth.Mie–Rayleigh scattering lidar is an important technology for detecting parameters from the surface to the middle and upper atmosphere.Because of the different aerosol distributions,Mie scattering and Rayleigh scattering have their own optimal detection ranges.Given the long period and high cost of any deep space exploration program,it is important to conduct sufficient feasibility studies and parameter simulations before the payload is launched.In this study,a parameterized lidar mathematical model and Earth’s atmospheric mode are used to compare with the measured signals of ground-based Mie–Rayleigh scattering lidar,and the correctness of the lidar mathematical model is verified.Using the model,we select the landing area of Tianwen-1 and substitute it into the Martian atmospheric mode,and then the Mie–Rayleigh lidar backscattering signal and the key parameters of the lidar system are systematically analyzed under the conditions of a clean Martian atmosphere and a global sandstorm.In addition,the optimal detection altitude ranges of Mie scattering and Rayleigh scattering on Mars under different atmospheric conditions are obtained,which provides a reference for the practical design and development of the subsequent lidar system for the Martian atmospheric environment.

MAVEN observation of magnetosonic waves in the Martian magnetotail region

Magnetosonic waves are an important medium for energy transfer in collisionless space plasma.Magnetosonic waves have been widely investigated in the upstream of the bow shock at Mars.These waves are believed to originate from pickup ions or reflected particles.By utilizing MAVEN spacecraft data,we have observed the occurrence of quasi-perpendicularly propagating magnetosonic emissions near the proton gyrofrequency in the Martian magnetotail region.These plasma waves are associated with a significant enhancement of proton and oxygen flux.The excited magnetosonic waves could possibly heat the protons through resonance and facilitate the ionospheric plasma escape.Our results could be helpful to better understand the Mars’magnetospheric dynamics and offer insights into possible energy redistribution between waves and plasma in the Martian nightside magnetosphere.

Influence of upstream solar wind on magnetic field distribution in the Martian nightside ionosphere

Using over eight years of Mars Atmosphere and Volatile Evolutio N(MAVEN)data,from November 2014 to May 2023,we have investigated the Martian nightside ionospheric magnetic field distribution under the influence of upstream solar wind drivers,including the interplanetary magnetic field intensity(∣BIMF∣),solar wind dynamic pressure(PS W),solar extreme ultraviolet flux(EUV),and Martian seasons(L s).Our analysis reveals pronounced correlations between magnetic field residuals and both∣BIMF∣and PS W.Correlations observed with EUV flux and Ls were weaker—notably,magnetic field residuals increased during periods of high EUV flux and at Mars perihelion.We find that the IMF penetrates to an altitude of 200 km under a wide range of upstream conditions,penetrating notably deeper under high∣BIMF∣andPSWconditions.Our analysis also indicates that EUV flux and IMF cone angle have minimal impact on IMF penetration depth.Those findings provide useful constraints on the dynamic nature of Martian atmospheric escape processes and their evolution,suggesting that historical solar wind conditions may have facilitated deeper IMF penetration and higher rates of ionospheric escape than are observed now.Moreover,by establishing criteria for magnetic‘quiet’conditions,this study offers new insights into the planet’s magnetic environment under varying solar wind influences,knowledge that should help refine models of the Martian crustal magnetic field.

Proton pitch angle distributions in the Martian induced magnetosphere: A survey of Tianwen-1 Mars Ion and Neutral Particle Analyzer observations

The pitch angle distributions of ions and electrons can be affected by various processes;thus,they can serve as an important indicator of the physical mechanisms driving the dynamics of space plasmas.From observations from the Mars Ion and Neutral Particle Analyzer onboard the Tianwen-1 orbiter,we calculated the pitch angle distributions of protons in the Martian induced magnetosphere by using information from the magnetohydrodynamically simulated magnetic field,and we statistically analyzed the spatial occurrence pattern of different types of pitch angle distributions.Even though no symmetrical features were seen in the dataset,we found the dominance of the field-aligned distribution type over the energy range from 188 to 6232 eV.Maps of the occurrence rate showed the preferential presence of a trapped-like distribution at the lower altitudes of the surveyed nightside region.Although our results are more or less restricted by the adopted magnetic field,they indicate the complexity of the near-Mars proton pitch angle distributions and infer the possibility of wave–particle interactions in the Martian induced magnetosphere.

Direct evidence for efficient scattering of suprathermal electrons by whistler mode waves in the Martian magnetosphere

Whistler mode waves are critical emissions in magnetized plasmas that usually influence the electron dynamics in a planetary magnetosphere.In this paper,we present a unique event in the Martian magnetosphere in which enhanced whistler mode waves(~10^(−11) V^(2)/m^(2)/Hz)with frequency of 0.1 f_(ce)-0.5 f_(ce) occurred,based on MAVEN data,exactly corresponding to a significant decrease of suprathermal electron fluxes.The diffusion coefficients are calculated by using the observed electric field wave spectra.The pitch angle diffusion coefficient can approach 10^(−2) s^(−1),which is much larger,by~100 times,than the momentum diffusion coefficient,indicating that pitch angle scattering dominates the whistler-electron resonance process.The current results can successfully explain the dropout of the suprathermal electrons in this event.This study provides direct evidence for whistler-driven electron losses in the Martian magnetosphere.

基于非监督对比学习的火星地形特征提取方法

火星表面地形智能识别对火星车自主探测具有重要意义,火星地形图像的特征提取方法目前主要分为传统的浅层视觉特征提取和基于监督学习的深层特征提取2类。找回丢失图像信息、获取大量带标签数据是要解决的关键问题。为此,提出一种基于非监督对比学习的火星地形特征识别方法,通过建立图像字典数据集,用“问询”和“编码”2组神经网络分别将单个图像与“字典”数据集中其他图像进行对比,用相似度泛函作为损失函数对网络进行训练,从而实现对火星地形图像的特征识别。所提方法还具有对训练数据集之外的新类型地形图像识别能力,后续识别分类优越性突出。仿真结果表明:所提方法识别准确率为85.4%,对新类型地形图像的识别准确率为84.5%。

基于热模型相关性验证的火面环境热平衡试验

针对热平衡试验中难以综合模拟火面复杂多变服役热环境的困难,建立一种基于热模型相关性验证的热平衡试验方法。采用真空、低压变温自然对流和低压定温强迫对流验证相结合的方式,验证高低温条件下热分析模型的对流、导热、辐射网络系数和热容等参数,并由相关性检验后的热分析模型验证设计的正确性。结果表明,板温度高于气温11~86℃条件下(气温-91℃)的自然对流传热系数为0.19~0.57 W/(m^(2)·K),4~15 m/s风速下的强迫对流换热系数为1.24~2.4 W/(m^(2)·K)修正后的热分析模型与试验结果偏差在±3.5℃以内。该方法在不完全模拟服役热环境条件下实现航天器热设计验证,提供有效的热分析模型,已成功应用于祝融号火星车热平衡试验。

火星原位建造材料研究进展与展望

火星风化层作为一种重要的原位自然资源,在火星基础设施建设上具有重要作用.基于与地球上不同的火星极端环境与火壤特殊性质,系统研究了火星原位建造材料的物理特征与机械性质,重点分析了火壤类混凝土材料(具体包括含硫混凝土、聚合物混凝土、地聚物混凝土与水凝胶基混凝土)、火壤熔融与烧结原位固化材料两个方面的最新研究进展.尽管目前火星原位建造材料的研究已取得一定成果,但仍面临诸如聚合物混凝土原位制备困难、熔融与烧结过程能耗较大,以及在火星环境下建造材料服役性能不足等局限问题.根据火星原位建造材料在未来的发展方向,研究结果旨在积极推进对火星原位建造材料的深入研究,为实现火星原位建造提供借鉴与参考.

火星陨石NWA 13763矿物岩石学特征及其岩浆演化

NWA 13763陨石为一块新发现的辉长质辉玻无球粒火星陨石,辉长结构和次辉绿结构,主要矿物组成为辉石(45.1%,其中普通辉石36.1%,易变辉石9.0%)和斜长石(42.3%,几乎全部熔长石化),次要矿物组成为富硅相(5.1%)、橄榄石(2.7%)、磷酸盐矿物(2.4%)、钛铁矿(2.2%),含极少量钛磁铁矿和斜锆石。陨石中广泛发育“铁橄榄石+富硅相”二相后成合晶和“钙铁辉石+铁橄榄石+富硅相”三相后成合晶。辉石主晶核部贫铁富镁(Fs_(24.7-55.3)),边部富铁贫镁(Fs_(61.5-86.1));熔长石成分均一(An_(44.4-54.6Ab43.7-53.7));铁橄榄石(Fa_(84.5-97.7))全部以细粒状分布于后成合晶中。由钛铁氧化物固溶体计算得到岩浆结晶的氧逸度(FMQ)f_(O_(2))=-0.045,钛铁矿结晶温度约975℃。利用全岩成分和MELTS程序模拟计算表明,NWA 13763陨石的母岩浆液相线温度范围可能为1190~830℃,矿物结晶顺序由早到晚可能为:培长石→拉长石→橄榄石→单斜辉石→中长石→磷酸盐矿物→钛铁矿→富硅残余相。

基于进入圆球的火星大气密度与风速反演方法

针对现有火星大气密度和风速探测方法的不足,提出了一种基于进入圆球的火星大气密度和风速反演方法。圆球携带加速度计和陀螺仪测量大气阻力加速度和姿态。基于圆球阻力加速度方向实现风速与密度解耦,设计了风速独立求解算法和基于高精度风速反演结果的密度求解算法,并通过理论分析和数值仿真对反演算法的误差进行了分析计算。仿真结果表明该方法可有效反演得到高精度火星中低层大气密度和风速,在80 km以下,横向风速误差在8%以内,密度误差7%以内。

火星表面上升轨迹映射伪谱凸优化方法

针对火星表面上升轨迹优化问题,提出了映射Chebyshev伪谱凸优化方法。首先采用无损凸化方法对火星表面上升燃耗最优问题进行凸松弛,然后将凸化后的问题在映射Chebyshev-Gauss-Lobatto点处离散,利用重心有理Lagrange插值技术进行插值,最后使用序列凸优化方法迭代求解,得到数值最优解。仿真对比了本文方法、一般伪谱凸优化方法和经典的序列凸优化方法,证明了本文方法在计算效率方面存在优势,并有效改善了标准Chebyshev微分矩阵的病态特性。

Snow and regolith albedo variations using CRISM data at McMurdo crater,Mars

The cryosphere component provides the most reliable and insightful indications of any planet’s climate dynamics.Using data from the Compact Reconnaissance Imaging Spectrometer for Mars(CRISM),we develop a novel approach to determining the broadband Visible and Near Infrared(VNIR)albedo of the Martian surface.This study focuses on albedo changes in the McMurdo crater,part of Mars’s south polar layer deposits.We compare seasonal and interannual variations of the McMurdo surface albedo before,during,and after the Global Dust Storm(GDS)of Martian Year(MY)34.As the seasons progressed from spring to summer,the mean albedo in MY 32 and 34 plunged by over 40%,by about 35%in MY 33,and by slightly more than 30%in MY 35.Compared interannually,however,mean albedo values within both seasons(spring and summer)exhibited no significant differences in those same years.Notably,interannual albedo difference maps reveal albedo variation of more than±0.3 in certain regions of the crater.Considering only snow-covered pixels,interannual albedo differences suggest that Mars dust had a pervasive impact on Mars’s cryosphere.Variations in maximum and minimum albedo values as high as 0.5 were observed,depending upon differences in the dust levels in Martian snow/ice.The maximum and the minimum snow albedo values were lowest in MY 34,indicating the effect of the intense dust storm event that year.The average snow albedo decreased from 0.45 in MY 32 to 0.40 in MY 33 and to 0.33 in MY 34,and then rose back to 0.40 in MY 35.This trajectory suggests a temporary deposition of dust,partially reversed after the GDS by self-cleaning mechanisms(local aeolian process and CO_(2)sublimation/deposition cycle).

火星表面微生物存活的潜力和限制因素分析

评估微生物在地外行星表面的存活状况是深空探测活动中实施地外生命探测和行星保护的前提条件之一。文章分析了火星表面环境特征及其对微生物存活的影响,以及在火星探测活动中微生物存活的潜力;归整出可用于微生物对火星环境适应性研究的空间模拟平台和地面环境模拟设备,并指出要模拟真实火星环境仍需改进多功能模拟设备。研究微生物在火星环境中存活和适应机制对于地外生命探测、地外生物安全风险评估以及深空探测工程应用有重要意义。

火星大气环境下发动机喷流对飞行器气动特性的影响分析

本文采用计算流体力学(CFD)方法模拟火星大气参数和发动机喷流,研究火星大气对飞行器气动特性的影响,针对发动机喷流对火星大气环境下细长体飞行器的气动特性影响开展了研究。计算结果表明:相较地球大气,火星大气环境计算出的轴向力系数更大,压心系数在跨声速段波动更小。为了进行精细化的火星飞行器气动外形设计,需要进一步优化火星大气计算模型,更加真实地模拟火星大气环境带来的影响。火星大气环境下的发动机喷流也会显著改变上升飞行器的全箭气动特性,影响飞行器表面的压力分布和下游流场区域。火星飞行器受到喷流影响,轴向力系数在Ma=5前变小,在Ma=5后变大,法向力系数以及压心系数在跨声速段会突然减小。

SN 1054,SN 1006,&Nova WZ Sagittae Calving Antarctic Ice Cap—Global Warming&Moose Die Off Longitude Relationship Deflection Area in Antarctica and USA—WZ Sagittae Impact and Martian Dust Storms

The SNIT theory proposes the effects of exploding stars,supernova and nova,on the biosphere of Earth.The feature on our planet that is most sensitive to the incoming energy of an exploding star is sea ice at the poles and this brings in the concept of global warming.The incoming particle streams for SN 1054,SN 1006,and Nova WZ Sagittae have left easily interpreted data noted as calving under the Antarctic ice cap that matches previously predicted longitude locations for the local heat input of the particle streams of the exploding stars.Animal die offs are also caused by the incoming particle streams.The deflection area longitude range for SN 1054 calving produces the correct longitude range for the moose die off beginning in the northern USA in 2006.Some Martian dust storms are created by the wave front of the exploding star debris streams.The explanation of these exploding stars effects using the SNIT theory is the object of this work.

YingHuo-1——Martian Space Environment Exploration Orbiter

This paper gives a brief introduction of YingHuo-1(YH-1),a Chinese Martian Space Environment Exploration Orbiter.YH-1 is a micro-satellite developed by Chinese Aerospace Industry,and will be launched together with Russian spacecraft,Phobos-Grunt,to orbit Mars in September,2009.Four payloads are selected for the mission,plasma package,including of electron analyzer,ion energy and mass analyzer;sat-sat occultation receiver;flux-gate magnetometer;and optical monitor.YH-1 mission focus on the investigation of the characteristics and its evolution of the Martian space Environment,and identifying major plasma processes,which provide channels for Martian volatiles escaping.

Bidirectional electron conic observations for photoelectrons in the Martian ionosphere

Electron pitch angle distributions similar to bidirectional electron conics(BECs)have been reported at Mars in previous studies based on analyses of Mars Global Surveyor measurements.BEC distribution,also termed“butterfly”distribution,presents a local minimum flux at 90°and a maximum flux before reaching the local loss cone.Previous studies have focused on 115 eV electrons that were produced mainly via solar wind electron impact ionization.Here using Solar Wind Electron Analyzer measurements made onboard the Mars Atmosphere and Volatile Evolution spacecraft,we identify 513 BEC events for 19-55 eV photoelectrons that were generated via photoionization only.Therefore,we are investigating electrons observed in regions well away from their source regions,to be distinguished from 115 eV electrons observed and produced in the same regions.We investigate the spatial distribution of the 19-55 eV BECs,revealing that they are more likely observed on the nightside as well as near strong crustal magnetic anomalies.We propose that the 19-55 eV photoelectron BECs are formed due to day-to-night transport and the magnetic mirror effect of photoelectrons moving along cross-terminator closed magnetic field lines.

Preparation and characterization of Martian soil simulant NEU Mars-1

To develop Martian soil simulant,basalts of the Chahar volcanic group in Wulanchabu,Inner Mongolia,China were selected as the simulant initial materials,which were ground and sorted to a predetermined particle size ratio,and small amounts of magnetite and hematite were added.The main phases of NEU Mars-1 simulant were plagioclase,augite and olivine.The glass transition and crystallization temperatures of NEU Mars-1 were 547.8 and 795.7°C,respectively.The complex dielectric constant,magnetic conductivity(0.99-1.045),and dielectric loss tangent angles(0.0025-0.030)of NEU Mars-1 were all stable in the frequency range of 2-18 GHz.Mossbauer spectroscopy results showed that the mass ratio of Fe2+to Fe3+in the simulant was 77.6:22.4.The NEU Mars-1 Martian soil simulant demonstrated particle size ratio,chemical composition,phase composition,thermal stability,and dielectric property similar to Martian soil,and can be used as the substitute material to extract oxygen and metals with in-situ resource utilization technologies.