Thermal Properties of Icy Surfaces in the Outer Solar System

The thermal properties of airless icy surfaces are providing a wealth of information on their regolith structure after eons of space weathering. Numerous observations of the thermal cycles of Jupiter and Saturn icy satellites or Centaurs and TNOs have been acquired in the latest decades thanks to the Galileo and Cassini missions and to the Spitzer and Herschel telescopes. These observations and the latest developments on thermophysical modeling which have been achieved to link the thermal inertia to the regolith structure are reviewed here. Measured thermal inertias of these surfaces covered with water ice are very low, roughly between about 1 and 100 J/m²/K/s^1/2. Often interpreted as due to unconsolidated or highly porous regoliths, these low values may result from a composition of amorphous ice or from the roughness of grains defacing contacts in a regolith of normal compaction. Taken together, thermal inertias appear to increase with probed depth and to decrease with heliocentric distance. This latter effect can be easily reproduced if heat transfer is dominated by radiation in pores, despite low temperatures, because the conduction through grains is limited, either due to the presence of amorphous ice or because of the roughness of grains.     

Spectroscopy of Icy Moon Surface Materials

Remote sensing of icy objects in the outer solar system relies upon availability of appropriate laboratory measurements. Surface deposits of specific substances often provide our most direct route to understanding interior composition, thereby informing theories of endogenic surface modification, exogenic surface processing and processes involving exchange of material with the interiors. Visible to near-infrared reflectance spectra of properly prepared compounds are required to enable retrieval of surface abundances through linear and nonlinear mixture analysis applied to spacecraft observations of icy bodies. This chapter describes the techniques, conditions and approaches necessary to provide reference spectra of use to theoretical models of icy satellite surface compositions, and summarizes the current state of knowledge represented in the published literature.     

SiO_2气凝胶材料的制备、性能及其低温保温隔热应用

由于SiO2气凝胶独特的纳米多孔结构,使其具有诸多其他材料所不能比拟的优异性能,比如极高的孔隙率和比表面积、极低的热导率及密度等特性。这些优异的性能使得SiO2气凝胶在高效保温隔热、隔声等领域具有极大的应用潜力。本文阐述了SiO2气凝胶的溶胶-凝胶制备过程及其机理,分别对SiO2气凝胶的热学、力学、光学和疏水性能的研究进展进行了概述,同时分析了气凝胶的微观结构与上述性能之间的关系,并介绍了SiO2气凝胶在低温保温隔热领域的应用现状和前景。     

Characteristics of Icy Surfaces

The surfaces of the Solar System’s icy satellites show an extraordinary variety of morphological features, which bear witness to exchange processes between the surface and subsurface. In this paper we review the characteristics of surface features on the moons of Jupiter, Saturn, Uranus and Neptune. Using data from spacecraft missions, we discuss the detailed morphology, size, and topography of cryovolcanic, tectonic, aeolian, fluvial, and impact features of both large moons and smaller satellites.     

Evolution of Icy Satellites

Evolutionary scenarios for the major satellites of Jupiter, Saturn, Neptune, and Pluto-Charon are discussed. In the Jovian system the challenge is to understand how the present Laplace resonance of Io, Europa, and Ganymede was established and to determine whether the heat being radiated by Io is in balance with the present tidal dissipation in the moon. In the Saturnian system, Enceladus and Titan are the centers of attention. Tidal heating is the likely source of activity at the south pole of Enceladus, although the details of how the heating occurs are not understood. An evolutionary scenario based on accretion and internal differentiation is presented for Titan, whose present substantial orbital eccentricity is not associated with any dynamical resonance. The source and maintenance of methane in Titan’s present atmosphere remain uncertain. Though most attention on the Saturnian moons focuses on Titan and Enceladus, the mid-size satellites Iapetus, Rhea, Tethys, and the irregular satellite Phoebe also draw our interest. An evolutionary scenario for Iapetus is presented in which spin down from an early rapidly rotating state is called upon to explain the satellite’s present oblate shape. The prominent equatorial ridge on Iapetus is unexplained by the spin down scenario. A buckling instability provides another possible explanation for the oblateness and equatorial ridge of Iapetus. Rhea is the only medium-size Saturnian satellite for which there are gravity data at present. The interpretation of these data are uncertain, however, since it is not known if Rhea is in hydrostatic equilibrium. Pluto and Charon are representative of the icy dwarf planets of the Kuiper belt. Did they differentiate as they evolved, and do either of them have a subsurface liquid water ocean? New Horizons might provide some answers when it arrives at these bodies.     

多层反射纳米隔热材料的制备及性能研究

制备了超薄纳米隔热材料和高反射金属箔,并组合成多层反射纳米隔热材料.结果表明:制备的超薄纳米隔热材料表面平整、厚度小于0.5 mm,材料的孔和粒径为纳米尺度;制备的金属膜结构紧密,厚度满足设计要求,在中心波长附近平均反射率高于95%.典型多层反射纳米隔热材料室温热导率为16 mW/(m·K).     

Chemical Composition of Icy Satellite Surfaces

Much of our knowledge of planetary surface composition is derived from remote sensing over the ultraviolet through infrared wavelength ranges. Telescopic observations and, in the past few decades, spacecraft mission observations have led to the discovery of many surface materials, from rock-forming minerals to water ice to exotic volatiles and organic compounds. Identifying surface materials and mapping their distributions allows us to constrain interior processes such as cryovolcanism and aqueous geochemistry. The recent progress in understanding of icy satellite surface composition has been aided by the evolving capabilities of spacecraft missions, advances in detector technology, and laboratory studies of candidate surface compounds. Pioneers 10 and 11, Voyagers I and II, Galileo, Cassini and the New Horizons mission have all made significant contributions. Dalton (Space Sci. Rev., 2010, this issue) summarizes the major constituents found or inferred to exist on the surfaces of the icy satellites (cf. Table 1 from Dalton, Space Sci. Rev., 2010, this issue), and the spectral coverage and resolution of many of the spacecraft instruments that have revolutionized our understanding (cf. Table 2 from Dalton, Space Sci. Rev., 2010, this issue). While much has been gained from these missions, telescopic observations also continue to provide important constraints on surface compositions, especially for those bodies that have not yet been visited by spacecraft, such as Kuiper Belt Objects (KBOs), trans-Neptunian Objects (TNOs), Centaurs, the classical planet Pluto and its moon, Charon. In this chapter, we will discuss the major satellites of the outer solar system, the materials believed to make up their surfaces, and the history of some of these discoveries. Formation scenarios and subsequent evolution will be described, with particular attention to the processes that drive surface chemistry and exchange with interiors. Major similarities and differences between the satellites are discussed, with an eye toward elucidating processes operating throughout the outer solar system. Finally we discuss the outermost satellites and other bodies, and summarize knowledge of their composition. Much of this review is likely to change in the near future with ongoing and planned outer planet missions, adding to the sense of excitement and discovery associated with our exploration of our planetary neighborhood.     

ZrO2陶瓷热障涂层显微结构及隔热性能研究

用电子束物理气相沉积法(EB-PVD)在DZ125高温合金上制备Y2O3部分稳定化的ZrO2(YSZ)陶瓷热障涂层,并用扫描电镜(SEM)观察涂层显微结构.采用激光脉冲法对EB-PVD热障涂层的热扩散系数进行测试.为防止热扩散系数测试时激光穿透ZrO2陶瓷层,在试样表面制备不同材料的遮挡层.结果表明,EB-PVD热障涂层呈明显的柱状晶结构,柱状晶垂直于涂层/基体界面.基体的热扩散系数随温度的升高而急剧增加,陶瓷热障涂层的热扩散系数随温度的升高呈下降趋势,但变化幅度不大.室温下陶瓷层的热扩散系数小于基体的1/3,1200℃时约为基体的1/67.试样的激光遮挡层很好解决了激光脉冲法测试涂层热扩散系数时的不稳定性和激光穿透问题.在满足遮挡要求的条件下,遮挡层材料种类对热扩散系数测试无明显影响.     

航天服隔热材料技术研究进展

为明确我国未来航天服被动热防护技术的应用发展方向,结合国内外在用近地轨道航天服隔热材料技术的发展现状和先进航天服隔热材料的设计需求,对先进航天服隔热材料的相关研究进行了评述.目前,多层隔热组件是在近地轨道和月面等高真空环境下隔热效果最理想的材料,但为提高服装的活动性能和对空间环境的适应能力,需作进一步改进.纤维类材料在航天服隔热应用方面具有传统优势,但在面向火星任务为代表的低真空环境的深空探测中,未能达到热导率和材料厚度相结合的隔热目标;气凝胶类材料具有较低的热导率,在火星大气环境下具有最好的隔热性能,但无法规避粉尘污染及机械耐久性等问题.研究具有更细纤维尺度和特殊空隙结构的纤维种类,制备具有柔韧耐久特质的有机气凝胶材料,探索具有不同技术优势的材料的组合应用,将成为解决未来先进航天服隔热问题的主要途径.     

一种隔热材料热导率的测试及误差分析

在分析固体材料热导率不同测定方法的基础上.提出了一种新的高温隔热材料热导率的测量方法.建立了数理模型对这一方法进行理论分析,设计了测量方案并对测量方案进行详细的误差分析计算.误差分析表明:对于标准样本参比法,边界漏热导致的误差已经不是误差的主要因素,标准样本试件材料热导率成为测量误差的主要因素.     

Atmospheric/Exospheric Characteristics of Icy Satellites

The atmospheres/exospheres of icy satellites greatly vary from one to the next in terms of density, composition, structure or steadiness. Titan is the only icy satellite with a dense atmosphere comparable in many ways to that of the Earth’s atmosphere. Titan’s atmosphere prevents the surface from direct interaction with the plasma environment, but gives rise to Earth-like exchanges of energy, matter and momentum. The atmospheres of other satellites are tenuous. Enceladus’ atmosphere manifests itself in a large water vapor plume emanating from surface cracks near the south pole. Io’s SO₂ atmosphere originates from volcanoes. Europa’s tenuous O₂ atmosphere is produced by intense radiation bombardment. This chapter reviews the characteristics of the atmospheres of Titan, Enceladus, Io and Europa based on observations.     

高熵热障涂层陶瓷材料研究进展

随着军事和科技的发展,热障涂层应用技术已成为现代国防尖端技术中最重要的技术之一。而高熵热障涂层陶瓷材料具有高温相稳定性、超低热导率、耐腐蚀性强、热膨胀系数和断裂韧性较高等优点,可为高温合金基底提供良好的热防护,在航空航天、航海和核能等领域有重要的应用前景。对国内外已报道的高熵热障涂层陶瓷候选材料进行系统性分类总结,重点介绍了新型高熵热障涂层陶瓷材料的设计方法、结构类型及其性能特征,为高熵陶瓷在热障涂层材料领域的发展和应用思路。     

Effects of the External Environment on Icy Satellites

In order to understand the evolution of planetary satellite surfaces and atmospheres it is important to understand their external environments. In this paper we look at the interactions between plasma in planetary magnetospheres and satellite atmospheres responsible for the production and loss of atmospheric mass. We focus on the processes which take place in the tenuous atmospheres of the Galilean satellites and in the Enceladus water plume. We also review the impact histories of satellites in the outer solar system, and compare the record of impacts in the inner and outer solar system.     

Water and the Interior Structure of Terrestrial Planets and Icy Bodies

Water content and the internal evolution of terrestrial planets and icy bodies are closely linked. The distribution of water in planetary systems is controlled by the temperature structure in the protoplanetary disk and dynamics and migration of planetesimals and planetary embryos. This results in the formation of planetesimals and planetary embryos with a great variety of compositions, water contents and degrees of oxidation. The internal evolution and especially the formation time of planetesimals relative to the timescale of radiogenic heating by short-lived ²⁶Al decay may govern the amount of hydrous silicates and leftover rock–ice mixtures available in the late stages of their evolution. In turn, water content may affect the early internal evolution of the planetesimals and in particular metal-silicate separation processes. Moreover, water content may contribute to an increase of oxygen fugacity and thus affect the concentrations of siderophile elements within the silicate reservoirs of Solar System objects. Finally, the water content strongly influences the differentiation rate of the icy moons, controls their internal evolution and governs the alteration processes occurring in their deep interiors.     

双层涂层复合材料的介电性能

在涤纶基布上分别进行铁氧体/碳化硅、碳化硅/石墨双层复合涂层整理,制备两种双层涂层柔性复合材料.分别研究吸波剂含量对复合材料介电常数实部、虚部、损耗角正切的影响.鉴于该材料多用于工程领域,测试了该复合材料的机械性能.结果表明,该复合材料在低频范围内具备良好的介电性能,且具备一定的力学性能.     

Radiolysis and Photolysis of Icy Satellite Surfaces: Experiments and Theory

The transport and exchange of material between bodies in the outer solar system is often facilitated by their exposure to ionizing radiation. With this in mind we review the effects of energetic ions, electrons and UV photons on materials present in the outer solar system. We consider radiolysis, photolysis, and sputtering of low temperature solids. Radiolysis and photolysis are the chemistry that follows the bond breaking and ionization produced by incident radiation, producing, e.g., O₂ and H₂ from irradiated H₂O ice. Sputtering is the ejection of molecules by incident radiation. Both processes are particularly effective on ices in the outer solar system. Materials reviewed include H₂O ice, sulfur-containing compounds (such as SO₂ and S₈), carbon-containing compounds (such as CH₄), nitrogen-containing compounds (such as NH₃ and N₂), and mixtures of those compounds. We also review the effects of ionizing radiation on a mixture of N₂ and CH₄ gases, as appropriate to Titan’s upper atmosphere, where radiolysis and photolysis produce complex organic compounds (tholins).     

基于柱状结构的热障涂层隔热性能数值研究

基于四参数随机生长方法和热阻网络方法开发了涂层微结构构建和隔热性能分析软件,构建了各向异性孔隙结构的柱状涂层微结构,着重研究了柱状孔隙大小、数量和细长化对柱状涂层有效导热系数和隔热性能的影响。结果表明:提高涂层的孔隙率是增强涂层隔热性能的有效途径;孔隙率一定时,随着柱状孔隙直径减小,其隔热性能增强,并且结构更加稳定;孔隙率一定时,随着柱状孔隙细长化,其隔热性能在一定程度上会有所减弱,但其稳态导热温度分布更加均匀,结构更加稳定。     

高速电主轴热态特性的有限元分析

分析了高速电主轴中内装式电机的损耗发热和轴承的摩擦发热 ,研究了油 -水热交换冷却系统和油 -气润滑系统的散热特性 ,在此基础上建立了高速电主轴温度场的有限元分析模型 ,并用ANSYS有限元软件进行温度场的计算。最后提出了改进高速电主轴温度场分布的主要措施     

纳米结构热障涂层的制备与性能研究

为充分发掘氧化锆(YSZ:ZrO2-6wt%Y2O3)基热障涂层的潜力,利用纳米级的YSZ粉末作为陶瓷涂层原材料,分别对采用等离子喷涂(APS)和电子束物理气相沉积(EB-PVD)沉积具有纳米结构陶瓷涂层的工艺过程进行全面研究.对比性试验结果表明,涂层中引入纳米结构使热障涂层具有更高的隔热效果,更高的硬度以及更高的抗剥落能力.并对纳米结构陶瓷涂层微观结构的高温稳定性进行研究分析.     

内置光纤对复合材料性能的影响

将光纤内置于纤维增强复合材料结构中,可以实现复合材料结构的实时健康监测,具有成本低、不受电磁干扰、能监测结构内部变化等特点。采用内置光纤实时监测复合材料结构的健康状态是复合材料结构无损检测技术的重要发展趋势。