Spatial heterogeneity in the radiogenic activity of the lunar interior: Inferences from CHACE and LLRI on Chandrayaan-1

In the past, clues on the potential radiogenic activity of the lunar interior have been obtained from the isotopic composition of noble gases like Argon. Excess Argon (40) relative to Argon (36), as compared to the solar wind composition, is generally ascribed to the radiogenic activity of the lunar interior. Almost all the previous estimates were based on, ‘on-the-spot’ measurements from the landing sites. Relative concentration of the isotopes of ⁴⁰Ar and ³⁶Ar along a meridian by the Chandra’s Altitudinal Composition Explorer (CHACE) experiment, on the Moon Impact Probe (MIP) of India’s first mission to Moon, has independently yielded clues on the possible spatial heterogeneity in the radiogenic activity of the lunar interior in addition to providing indicative ‘antiquity’ of the lunar surface along the ground track over the near side of the moon. These results are shown to broadly corroborate the independent topography measurements by the Lunar Laser Ranging Instrument (LLRI) in the main orbiter Chandrayaan-1. The unique combination of these experiments provided high spatial resolution data while indicating the possible close linkages between the lunar interior and the lunar ambience.     

The ‘Standard’ Sun Modelling and Helioseismology

The ‘standard’ solar model is based on a number of simplifying assumptions and depends on knowledge of the physical properties of matter in the Sun. Given these assumptions, the constraint that the model have the observed surface luminosity provides an estimate of the initial solar helium abundance. From helioseismic analyses further information can be obtained about the present composition, including a fairly precise measure of the envelope helium abundance and an estimate of the hydrogen profile in the radiative interior. It must be emphasized, however, that these inferences may suffer from systematic error arising from incomplete knowledge about the equation of state and opacity of the solar interior. This revised version was published online in June 2006 with corrections to the Cover Date.     

"神舟三号"大气成分探测器探测结果--2002年4月磁暴期间大气成分的异常变化

"神州三号"(SZ-3)大气成分探测器搭载在SZ-3留轨舱上于2002年3月26日发射入轨,正遇2002年4月发生的连续两次地磁扰动事件,SZ-3大气成分探测器测得了轨道舱运行高度上(330-350 km附近)大气成分的响应变化和异常现象.探测数据表明,在地磁扰动期间,不仅发生了大气中主要成分O和N2的数密度值增变的响应变化,而且在进入地磁扰动峰期开始后6h左右在较高纬度处出现了N2的异常增变和O的异常降变.4-5h后,这种异常增变峰和降变谷由纬度42°N左右逐渐推移向纬度较低地区,直至消失.     

钛合金蜂窝三层结构的扩散焊接研究

介绍了俄罗斯钛合金蜂窝三层结构扩散焊接的研究成果.详细介绍了铝合金、焊接规范选择、接头应力变形状态的分析、模拟计算等,有助于国内钛合金的焊接研究.     

Micro powder injection molding of boron carbide components with SiC-Al2O3-Y2O3 sintering additives

Sintering additives and micro-powder injection molding offer an effective method to densify boron carbide（B₄C） and make B₄C components with complex shapes. By adjusting the proportion of three kinds of powders（SiC, Al₂O₃ and Y₂O₃）, four kinds of sintering additives were prepared. The feedstock uniformity, debinding behavior, phase composition and microstructure of micro injection molded B₄C components with different sin...     

航空术语的构词分析

以全国科学技术名词审定委员会公布的"航空科学技术名词"为览本,对航空术语的词性和构型进行分析,通过举例作出了某些详述,并推导出对外来术语的吸纳方法和原则。     

高硅条件下锰对奥贝球铁硬度的影响研究

奥贝球墨铸铁能够实现高硬度的同时具有较高的韧性,适合于一定冲击条件下的耐磨零件工作要求,本文针对奥贝球铁高硅成分中锰的作用研究,为该材料的应用提供了实验基础研究。     

在DD3单晶上进行FGH95粉末激光多层涂覆:单晶涂层组织形式规律研究

利用高温合金 FGH95粉末在 DD3单晶的不同晶面上进行激光多层涂覆实验 ,深入研究了涂覆层中凝固显微组织的生长规律。研究表明基材的晶体取向和局部凝固条件对涂层中的凝固显微组织有很大的影响。当单晶基材择优晶向与热流方向夹角小于 30°时 ,可以得到从基材上外延生长的单晶 ,涂层内二次臂退化 ,枝晶一次间距为 10～ 2 0 μm;当实验所在的单晶基材的择优晶向与热流的方向夹角大于 30°时 ,涂层中晶体取向偏离基材的取向 ,并出现多晶。即便当实验在同一个择优晶面上进行时 ,局部凝固条件不同 ,涂层内的凝固显微组织也有很大的差别。二次臂退化 ,一次臂间距大约为 10～ 2 0 μm。进一步的研究表明 ,涂层中主要组成相为枝晶干上分布的基体相 γ和沉淀硬化相 γ′以及枝晶间的 γ+γ′花状共晶和少量碳化物 ,γ′相主要为具有良好强化效果的细小立方体 ,尺度约为 0 .1μm     

The Coma of Comet 9P/Tempel 1

As comet 9P/Tempel 1 approaches the Sun in 2004–2005, a temporary atmosphere, or “coma,” will form, composed of molecules and dust expelled from the nucleus as its component icy volatiles sublimate. Driven mainly by water ice sublimation at surface temperatures T > 200 K, this coma is a gravitationally unbound atmosphere in free adiabatic expansion. Near the nucleus (≤ 10² km), it is in collisional equilibrium, at larger distances (≥10⁴ km) it is in free molecular flow. Ultimately the coma components are swept into the comet’s plasma and dust tails or simply dissipate into interplanetary space. Clues to the nature of the cometary nucleus are contained in the chemistry and physics of the coma, as well as with its variability with time, orbital position, and heliocentric distance. The DI instrument payload includes CCD cameras with broadband filters covering the optical spectrum, allowing for sensitive measurement of dust in the comet’s coma, and a number of narrowband filters for studying the spatial distribution of several gas species. DI also carries the first near-infrared spectrometer to a comet flyby since the VEGA mission to Halley in 1986. This spectrograph will allow detection of gas emission lines from the coma in unprecedented detail. Here we discuss the current state of understanding of the 9P/Tempel 1 coma, our expectations for the measurements DI will obtain, and the predicted hazards that the coma presents for the spacecraft. An erratum to this article is available at .     

Formation and Composition of Planetesimals

The composition of planetesimals depends upon the epoch and the location of their formation in the solar nebula. Meteorites produced in the hot inner nebula contain refractory compounds. Volatiles were present in icy planetesimals and cometesimals produced in the cold outer nebula. However, the mechanism responsible for their trapping is still controversial. We argue for a general scenario valid in all regions of the turbulent nebula where water condensed as a crystalline ice (Hersant et al., 2004). Volatiles were trapped in the form of clathrate hydrates in the continuously cooling nebula. The epoch of clathration of a given species depends upon the temperature and the pressure required for the stability of the clathrate hydrate. The efficiency of the mechanism depends upon the local amount of ice available. This scenario is the only one so far which proposes a quantitative interpretation of the non detection of N₂ in several comets of the Oort cloud (Iro et al., 2003). It may explain the large variation of the CO abundance observed in comets and predicts an Ar/O ratio much less than the upper limit of 0.1 times the solar ratio estimated on C/2001 A2 (Weaver et al., 2002). Under the assumption that the amount of water ice present at 5 AU was higher than the value corresponding to the solar O/H ratio by a factor 2.2 at least, the clathration scenario reproduces the quasi uniform enrichment with respect to solar of the Ar, Kr, Xe, C, N and S elements measured in Jupiter by the Galileo probe. The interpretation of the non-uniform enrichment in C, N and S in Saturn requires that ice was less abundant at 10 AU than at 5 AU so that CO and N₂ were not clathrated in the feeding zone of the planet while CH₄, NH₃ and H₂S were. As a result, the 14N/15N ratio in Saturn should be intermediate between that in Jupiter and the terrestrial ratio. Ar and Kr should be solar while Xe should be enriched by a factor 17. The enrichments in C, N and S in Uranus and Neptune suggest that available ice was able to form clathrates of CH₄, CO and the NH₃ hydrate, but not the clathrate of N₂. The enrichment of oxygen by a factor 440 in Neptune inferred by Lodders and Fegley (1994) from the detection of CO in the troposphere of the planet is higher by at least a factor 2.5 than the lower limit of O/H required for the clathration of CO and CH4 and for the hydration of NH₃. If CO detected by Encrenaz et al. (2004) in Uranus originates from the interior of the planet, the O/H ratio in the envelope must be around of order of 260 times the solar ratio, then also consistent with the trapping of detected volatiles by clathration. It is predicted that Ar and Kr are solar in the two planets while Xe would be enriched by a factor 30 to 70. Observational tests of the validity of the clathration scenario are proposed.