In response to the performance impact of long cable signal transmission between the search coil and the preamplifier circuit, this paper establishes for the first time a circuit equivalent model of Search Coil-Cable-Preamplifier Circuit. Through simulation analysis and experimental verification, the influence of cable length on the frequency distribution of sensor noise is revealed. Theoretical analysis indicates that cable length has limited impact on sensor sensitivity, but significantly increases the noise level in the high-frequency band (>1 kHz). Based on a prototype search coil magnetometer with a target specification of 10～1000 Hz bandwidth and 30 fT·Hz^1/2 (1 kHz) noise, the variation law of noise with cable length is validated. Experimental results show that as the cable length increases from 3 m to 39 m, the noise corner frequency shifts forward from 7.5 kHz to 2 kHz, while the high-frequency noise at 10 kHz increases by a factor of six. The study finds that an increase in cable length has a significant impact on the noise of inductive magnetometers, specifically manifested as a slight improvement in low-frequency noise and a sharp deterioration in high-frequency noise. Although cable length has a notable effect on inductive magnetometers, its influence can be predicted and mitigated through theoretical modeling incorporating cable parameters. This research provides critical parameter basis for the engineering implementation of search coil magnetometers in space exploration scenarios requiring long-cable applications.

Due to the inherent limitations of current remote sensing techniques, the actual occurrence and accurate abundance of water ice in lunar regolith cannot be directly identified, making in-situ verification urgently necessary. The Chang’E-7 mission of China’s Lunar Exploration Program plans to conduct water ice detection at the lunar south pole, where an in-situ micro-sampling device mounted on the rover will perform quantitative collection of lunar regolith for the volatiles in-situ measurement instrument. However, the uncertainty of lunar surface conditions leads to considerable dispersion in sampling mass. Moreover, water ice sublimation loss caused by tool-soil temperature difference and mechanical interactions during sampling will further reduce the detection accuracy. To ensure the reliability of detection data from the volatiles measurement instrument, this paper proposes calibration methods for sampling mass and water ice loss. Icy lunar regolith simulant is prepared via vapor deposition during sampling, and sampling mass calibration experiments are carried out using a self-developed calibration device. Preliminary results show that sampling mass varies significantly with regolith particle size distribution. Further research will be conducted on the physical mechanism of icy lunar regolith sampling under multi-factor coupling conditions. This study aims to provide a high-confidence physical response parameter spectrum for accurate interpretation and scientific analysis of Chang’E-7 in-orbit data.

The lunar pole’s water ice is essential for understanding the Moon’s evolution and building future lunar research station. Nevertheless, existing orbital remote-sensing missions and returned samples remain insufficient to resolve the key unknowns of polar water, including its occurrence modes (e.g., adsorbed water/hydroxyl, pore-filling ice, or ice-cemented regolith), its abundance and vertical variability, and its potential origin and evolutionary pathways. To address this gap, the Chang’E-7 mini-flying probe will carry the Lunar soil Water molecule Analyser (LUWA) to conduct in-situ detection of water ice at the permanently shadowed region for the first time. This paper describes the compositional structure of LUWA and the detection approach, comprising drilling, sampling, sealing, heating and analysis. We detail the calibration parameters, apparatus, and procedures for its three core analytical modules: the Tunable Diode Laser Absorption Spectrometer (TDLAS), the Time-of-Flight Mass Spectrometer (TOF-MS), and the Differential optical Absorption Spectrometer (DAS). The operational chain is designed to release water through thermal extraction, quantify water content with high sensitivity across a wide dynamic range, and enable the determination of D/H isotopic signatures. A systematic ground calibration methodology and a unified calibration framework are established for three functional modules dedicated to water measurement. The framework defines calibration objectives, procedures, and traceability pathways to characterize module response functions, assess background and temperature-dependent effects, verify detection limits and linearity, and evaluate accuracy and repeatability, thereby supporting robust conversion from raw observables to calibrated water-content and isotope products in flight. In parallel, a dedicated lunar in-situ exploration test platform is developed to replicate LUWA’s full operational workflow using lunar regolith simulants, including drilling, sampling, sealing, heating, and analysis. Integrated tests validate key performance metrics and the measurement workflow, providing crucial technical support for interpreting Chang’E-7 LUWA data and for assessing the abundance and occurrence of water ice in lunar soil within PSRs.

In order to solve the problem of frequency stability and transmission accuracy decrease caused by temperature fluctuation during on-orbit operation of an extravehicular load equipment, a highly efficient thermal control scheme is proposed which bases on passive thermal control as the main approach and active thermal control as the auxiliary method. The scheme employs a single-phase liquid cold plate as the main heat dissipation surface, and 10-unit multi-layer insulation components for comprehensive encapsulation. High thermal conductivity materials are utilized to achieve efficient heat conduction. Simultaneously, heating sheets and TEC semiconductor ceramic sheets are used for precise temperature control. Through finite element simulation analysis of temperature distribution under both high and low temperature conditions and optimization design, the temperature variation of key components is controlled within ±0.5 K. The ground constant-temperature thermal balance experiment and the in-orbit data results indicate that this scheme effectively suppresses the interference of temperature fluctuations on the load equipment, significantly improves the overall temperature uniformity of the equipment. It enables photodiodes and other sensitive devices to operate within the optimal temperature range (25-50°C). The temperature change rate of temperature-sensitive devices on the extravehicular load equipment is better than 0.1 K·min^–1, meeting the on-orbit stability requirements of high-precision time-frequency transmission systems. It can provide an important reference for the thermal control design of similar space load equipment.

The Chang’E-7 spacecraft is scheduled to be landed in the Aitken Basin region of the lunar south pole to conduct comprehensive exploration and research on the lunar surface environment. As one of the main detectors onboard the Chang’E-7 spacecraft, a lunar dust detector is developed for in-situ measurements of naturally suspended dust in the polar region, key parameters such as the particle size, velocity, and cumulative mass flux will be obtained. To achieve high-precision scientific detection, systematic ground calibration experiments were conducted. For particle size calibration, a single-particle free-fall method combined with an equivalent test scheme using neutral density filters was employed, achieving coverage of the particle size range from 1 µm to 5000 µm. Experimental results demonstrate that the particle size retrieval error does not exceed 17%. Velocity calibration was performed by measuring the time-of-flight of free-falling particles from different heights, yielding a velocity measurement error within 13%. For mass flux calibration, the solution titration method was used to obtain the sensitivity of the Quartz Crystal Microbalances, with sensitivities in three orthogonal directions all on the order of 10^–9 g·Hz^–1·cm^–2 and exhibiting good linearity. Furthermore, temperature-frequency correction curves were established to support the normalization of in-orbit data. The calibration results indicate that the performance indicators of the dust detector meet the requirements for detection in the extreme environment of the lunar south pole. The established calibration methods and retrieval models provide a reliable foundation for the interpretation of subsequent in-orbit scientific data.

The temperature field during solidification has an important influence on the microstructure and properties of the material. Due to the difference of heat convection in space and ground environment, natural convection driven by gravity plays an important role in heat transfer in ground environment. However, in space, the microgravity environment almost eliminates the influence of gravity-dominated natural convection, which will lead to certain differences in the heat transfer characteristics between space and ground, resulting in differences in the temperature field distribution in the material experimental furnace. As a result, the temperature field obtained on the ground is different from that in space under the same temperature control conditions, thus affecting the equivalence of experimental conditions between space and ground materials. The heat transfer characteristics obtained from ground experiments cannot be directly applied to space experiments. This mismatch has a major impact on the space materials experiments. In order to obtain the heat transfer characteristics under microgravity conditions, a three-dimensional numerical model of heat transfer in the high temperature material experimental rack of the space station is established. In the modeling process, reasonable simplification is carried out according to the actual physical conditions, some minor heat transfer factors which have little influence on the overall temperature field are ignored. The temperature field simulation of the ground experiment and the space experiment was carried out respectively, and the temperature distribution of the sample box was obtained. The temperature obtained by simulation was compared with the measured temperature. Through comprehensive analysis of the changes of heat transfer parameters in the space microgravity environment and the normal gravity environment on the ground, the heat transfer law similar to the space condition was obtained. The research results provide a new way to predict the space temperature field distribution based on the ground experiment results of high temperature materials experiment rack and have important guiding significance for the future research of space materials.

The Muon Telescope at Siziwang Station in Inner Mongolia is used to detect the secondary cosmic ray muons reaching the ground. The Muon Telescope began construction in November 2019, was completed in April 2023, and produced scientific data. The muon telescope consists of a scintillator observation stack, an electronics recorder, a monitoring platform, and a power supply. The scintillator observation stack is composed of 48 detector units, divided into upper and lower layers with 24 units in each layer, arranged in a 6×4 array. In each detector unit, the plastic scintillator has dimensions of 50 cm × 50 cm × 5 cm. The distance between the upper and lower layers is 89 cm. A 5cm-thick layer of lead bricks is laid between the upper and lower layers to filter out low-energy cosmic rays and low-energy particles in the surrounding environment. The detectors have a total area of 6 m². Muon signals generated by the 48 detector units of the Muon Telescope are processed through front-end circuits for amplification, discrimination, and shaping, then sent to the FPGA logic circuit for directional coincidence calculation. This produces raw muon counts in 15 directions. After undergoing barometric correction calculation, a dataset of corrected muon counts in 15 directions is formed, with a temporal resolution of 1 hour. The count rate in the vertical direction is the highest, with the 1-hour count rate being around 600000 counts and the relative statistical error approximately 0.13%. The muon data can sensitively reflect diurnal variations, long-term variations of cosmic rays, and short-term Forbush decrease perturbations induced by coronal mass ejections. Spanning from May 2023 to April 2025, this dataset covers the high-activity phase of the 25th solar activity cycle. It provides valuable data resources for research on solar eruptions, their interplanetary disturbance propagation, and geomagnetic response processes, while also supporting space weather early warning efforts.

This review systematically summarizes recent advances in filmwise and dropwise condensation under microgravity, elucidating two-phase heat transfer mechanisms and gravitational influence patterns. For condensing heat transfer in tubes, gravity-independent criterion numbers (Bond number, Froude number, etc.) are used to determine whether gravity affects heat transfer, and the effect of gravity can be attenuated by increasing the mass flow rate of the vapor and reducing the tube diameter. In microgravity environments, dropwise condensation can be achieved through vapor flow acceleration combined with functional surfaces and air-blowing techniques for condensate removal. Current experimental studies on microgravity condensation remain limited due to challenges in obtaining sustained microgravity conditions. The paper emphasizes the necessity of conducting long-term condensation experiments utilizing orbital platforms like the China Space Station and International Space Station to address data reproducibility issues, investigate gravity-dependent mechanisms, and provide theoretical foundations for space two-phase thermal management systems.

The Moon provides a unique and advantageous platform for astronomical observations, particularly in the visible and ultraviolet wavelength ranges, owing to its extremely tenuous exosphere, the absence of atmospheric turbulence, and a stable surface environment. These characteristics enable long-duration, continuous observations free from atmospheric interference. As one of the international payloads aboard the Chang’E-7 mission, the International Lunar Observatory Camera (ILO-C) project aims to exploit these advantages to observe the Milky Way and the broader universe from a distinctive lunar perspective. In addition to its scientific objectives, the project offers unique value for astronomy education and serves as a technology demonstration for future lunar-based astronomical observatories. The ILO-C camera will be mounted on the +y panel of the Chang’E-7 lander and will experience multiple mission phases, including cruise, lunar orbit, and surface operations. This paper systematically investigates the scientific calibration workflow for the ILO-C across these mission phases, with particular emphasis on fundamental calibration, color calibration, and flux calibration, and further presents observational and calibration pathways for cross-validation. The quality of the project’s scientific output will largely depend on the optimized implementation of these calibration schemes. Ideally, in-flight activation and observations are expected to be achieved, allowing coverage of a broader sky area and enabling cross-comparison with observations from other space-based and ground-based astronomical facilities.

The Chang’E-7 orbiter is expected to carry the Wide-band InfraRed Imaging Spectrometer (WIRIS), which will acquire high spectral resolution images and thermal emission data of the lunar surface across a broad spectral range from the visible to longwave infrared (0.45～10 µm). These data will support scientific investigations into lunar surface mineral composition, thermal environment, and water/hydroxyl detection. Compared to previous lunar orbital hyperspectral instruments, WIRIS enhances quantitative retrieval capabilities for key spectral features such as the Christiansen Feature (CF) of silicate minerals and molecular water. Building upon the design of the Tianwen-1 Mars Mineralogical Spectrometer, WIRIS extends its spectral coverage into the mid- to long-wave infrared range (3.3～10 μm), and incorporates simultaneous temperature measurements to reduce thermal correction uncertainties in the 3 μm water/hydroxyl absorption region. This study addresses the quantitative calibration requirements of the newly extended spectral range by proposing spectral, radiometric, and geometric calibration methods tailored for the mid- to long-wave infrared bands. Based on calibration experiments, the sources of error and associated uncertainties are analyzed. The results provide essential methodological and technical support for accurate physical parameter retrieval and scientific application of WIRIS mid- to long-wave infrared data.