Widespread magma oceans on asteroidal bodies in the early Solar System

Immediately following the formation of the Solar System, small planetary bodies accreted, some of which melted to produce igneous rocks. Over a longer timescale (15-33 Myr), the inner planets grew by incorporation of these smaller objects through collisions. Processes operating on such asteroids strongly influenced the final composition of these planets, including Earth. Currently there is little agreement about the nature of asteroidal igneous activity: proposals range from small-scale melting, to near total fusion and the formation of deep magma oceans. Here we report a study of oxygen isotopes in two basaltic meteorite suites, the HEDs (howardites, eucrites and diogenites, which are thought to sample the asteroid 4 Vesta) and the angrites (from an unidentified asteroidal source). Our results demonstrate that these meteorite suites formed during early, global-scale melting (> or = 50 per cent) events. We show that magma oceans were present on all the differentiated Solar System bodies so far sampled. Magma oceans produced compositionally layered planetesimals; the modification of such bodies before incorporation into larger objects can explain some anomalous planetary features, such as Earth's high Mg/Si ratio.     

Phyllosilicates on Mars and implications for early martian climate

The recent identification of large deposits of sulphates by remote sensing and in situ observations has been considered evidence of the past presence of liquid water on Mars. Here we report the unambiguous detection of diverse phyllosilicates, a family of aqueous alteration products, on the basis of observations by the OMEGA imaging spectrometer on board the Mars Express spacecraft. These minerals are mainly associated with Noachian outcrops, which is consistent with an early active hydrological system, sustaining the long-term contact of igneous minerals with liquid water. We infer that the two main families of hydrated alteration products detected-phyllosilicates and sulphates--result from different formation processes. These occurred during two distinct climatic episodes: an early Noachian Mars, resulting in the formation of hydrated silicates, followed by a more acidic environment, in which sulphates formed.     

合成碳酸二甲酯的现状及展望

碳酸二甲酯是重要的有机化工原料,是新的燃油添加剂,是21世纪具有广阔应用前景的绿色化工产品。综述了碳酸二甲酯的各种合成路线,分析了不同工艺路线的优劣,介绍了国内外最新的生产情况、应用研究以及未来的发展趋势。     

活体水仙模板调控合成碳酸钙晶体

探讨利用一种新的天然活体植物——水仙作为模板,在室温下调控合成碳酸钙晶体,并对产物进行了SEM、XRD的分析和表征.碳酸钙的形貌随水仙的叶子、鳞茎、花部位不同而变化,分别是纺锤形、立方体、类球形,晶体大小为纳微米级,均为方解石和球霰石的混合物,但球霰石的含量随以上晶体形貌的改变而递增.这一结果充分说明水仙不同部位生物分子组成不同,因此导致对碳酸钙的调控作用不同.     

PbO均相催化反应精馏合成碳酸二苯酯的研究

通过对碳酸二甲酯(DMC)与苯酚(PhOH)酯交换法反应精馏合成碳酸二苯酯(DPC)的研究,筛选合适的催化剂和寻找最佳的工艺条件,为将来DPC的工业化打下基础。实验结果表明：在常压下,温度110～195℃范围内,当原料配比n(PhOH)：n(DMC)=2：1,n(PhOH)：n(催化剂)=1：0．016,反应时间10h,碳酸二甲酯转化率为32．63％(mol),DPC产率为25．01％(mol),碳酸苯甲酯(MPC)产率为7．62％(mol),DPC的选择性为76．65％,且无苯甲醚生成。所选催化剂PbO的催化性能明显优于路易斯酸和二丁基二月桂酸锡。     

酸性吗啉离子液体催化合成阿司匹林的研究

以N-甲基吗啉,氯磺酸为原料合成N-甲基-N-磺酸基吗啉盐酸盐的酸性离子液体,将其代替浓硫酸用于催化乙酸酐和水杨酸的酯化反应,合成阿司匹林。考察了原料配比、离子液体用量、反应温度、反应时间等因素对阿司匹林产率的影响,并通过正交实验确定最佳合成条件。结果表明该离子液体对阿司匹林的合成具有良好的催化效果,在水杨酸20mmol、乙酸酐40mmol、N-甲基-N-磺酸基吗啉盐酸盐离子液体3mL、反应温度70℃、反应时间30min的条件下,阿司匹林产率可达77.12%。     

有机锡均相催化反应蒸馏合成碳酸二苯酯

通过对碳酸二甲酯(DMC)与苯酚酯交换法反应蒸馏合成碳酸二苯酯(DPC)的研究,筛选合适的催化剂和寻找最佳的工艺条件,为DPC的工业化打下基础。实验结果表明,在常压下,温度145℃,原料配比n(PhOH)∶n(DMC)=3∶1,n(PhOH)∶n(催化剂)=1∶0.012,反应时间10h,碳酸二甲酯总转化率为32.04%,DPC产率为18.00%,碳酸苯甲酯(MPC)产率为14.04%,DPC的选择性为56.18%,而且无苯甲醚和CO2生成,所选催化剂二丁基二月桂酸锡的催化性能明显优于路易斯酸。     

Pb-Zn-O催化酯交换合成碳酸二苯酯

本研究采用正交试验考察了铅锌复合氧化物的制备条件,如铅锌比、老化时间、煅烧温度、煅烧时间和氨水浓度对催化剂的影响,实验结果表明煅烧温度显著影响催化剂的活性.以铅锌复合氧化物为催化剂,在常压,温度为160-190℃,n(苯酚):n(碳酸二甲酯):n(催化剂)为4:1:0.04,反应时间约为6 h的条件下,碳酸二苯酯的转化率为77.95%.XRD谱结果表明,PbO为主催化剂,ZnO为助催化剂.     

NKC-9酸性树脂非均相催化合成查耳酮

NKC-9酸性树脂催化芳醛与苯乙酮的Claisen-Schmidt缩合合成了五种查耳酮,收率81％～92％．考察了催化剂的用量和溶剂对收率的影响．该方法产率高、操作简便．产物结构经IR、NMR数据确认．     

Subsurface water and clay mineral formation during the early history of Mars

Clay minerals, recently discovered to be widespread in Mars's Noachian terrains, indicate long-duration interaction between water and rock over 3.7 billion years ago. Analysis of how they formed should indicate what environmental conditions prevailed on early Mars. If clays formed near the surface by weathering, as is common on Earth, their presence would indicate past surface conditions warmer and wetter than at present. However, available data instead indicate substantial Martian clay formation by hydrothermal groundwater circulation and a Noachian rock record dominated by evidence of subsurface waters. Cold, arid conditions with only transient surface water may have characterized Mars's surface for over 4 billion years, since the early-Noachian period, and the longest-duration aqueous, potentially habitable environments may have been in the subsurface.     

花状碳酸钙的仿生合成及其载药性能

生理温度下,以无水氯化钙和碳酸钠为原料,硫酸软骨素为靶向试剂,癌细胞分泌物为形貌调控剂,制得花状碳酸钙.运用场发射扫描电子显微镜(FESEM)、X射线粉末衍射仪(XRD)、傅里叶红外光谱仪(FT-IR)对碳酸钙的形貌和结构成分进行了表征测定.激光共聚焦实验和负载实验证明该碳酸钙可以高效负载抗肿瘤药物盐酸阿霉素(DOX),不同pH值下的释放实验表明,该负载体系的DOX更易在弱酸性条件下释放,并且释放较为缓慢,有较好的缓释性能.细胞活性(MTT)实验表明,该负载体系对肿瘤细胞有特异性抑制效果.     

酯交换法合成碳酸二甲酯过程产物的气相色谱分析

采用HP-FFAP毛细柱,建立了一种同时定量测定一步酯交换法合成碳酸二甲酯过程产物的色谱分析方法.考察了柱温对分离效果的影响,确定了适宜的操作条件.结果表明,在所确定的操作条件下,反应混合物中的环氧乙烷、甲醇、碳酸二甲酯、乙二醇单甲醚、乙二醇和碳酸乙烯酯等组分峰都可以较好地分开,且峰形好;定量测定各组分含量的重现性相对标准偏差(RSD)均小于5%,准确性相对误差均小于3%,表明所建立的分析方法可以较好地满足工业生产过程控制分析的要求.     

环氧乙烷吸收溶液合成碳酸乙烯酯管式反应工艺条件

在自行建立的管式反应器上,采用实验室开发的NY-2催化剂,以环氧乙烷(EO)吸收溶液和CO2为原料,进行合成碳酸乙烯酯(EC)连续过程研究.考察液空速、吸收溶液中EC与乙二醇(EG)摩尔比、EC与EO摩尔比、水含量、催化剂用量、反应压力和温度对反应的影响.通过实验研究,确定了较佳的连续反应条件:反应温度为(125±5)℃、反应压力为(3.5±0.5)MPa、催化剂质量分数不小于2%、吸收溶液中水的质量分数少于1.2%、EC与EO摩尔比为5、EG质量分数小于30%、空速小于0.67 h-1.在此条件下,EO的转化率大于98%,EC的选择性大于80%.     

Dynamics of ice ages on Mars

Unlike Earth, where astronomical climate forcing is comparatively small, Mars experiences dramatic changes in incident sunlight that are capable of redistributing ice on a global scale. The geographic extent of the subsurface ice found poleward of approximately +/-60 degrees latitude on both hemispheres of Mars coincides with the areas where ice is stable. However, the tilt of Mars' rotation axis (obliquity) changed considerably in the past several million years. Earlier work has shown that regions of ice stability, which are defined by temperature and atmospheric humidity, differed in the recent past from today's, and subsurface ice is expected to retreat quickly when unstable. Here I explain how the subsurface ice sheets could have evolved to the state in which we see them today. Simulations of the retreat and growth of ground ice as a result of sublimation loss and recharge reveal forty major ice ages over the past five million years. Today, this gives rise to pore ice at mid-latitudes and a three-layered depth distribution in the high latitudes of, from top to bottom, a dry layer, pore ice, and a massive ice sheet. Combined, these layers provide enough ice to be compatible with existing neutron and gamma-ray measurements.     

Discovery of an aurora on Mars

In the high-latitude regions of Earth, aurorae are the often-spectacular visual manifestation of the interaction between electrically charged particles (electrons, protons or ions) with the neutral upper atmosphere, as they precipitate along magnetic field lines. More generally, auroral emissions in planetary atmospheres "are those that result from the impact of particles other than photoelectrons" (ref. 1). Auroral activity has been found on all four giant planets possessing a magnetic field (Jupiter, Saturn, Uranus and Neptune), as well as on Venus, which has no magnetic field. On the nightside of Venus, atomic O emissions at 130.4 nm and 135.6 nm appear in bright patches of varying sizes and intensities, which are believed to be produced by electrons with energy <300 eV (ref. 7). Here we report the discovery of an aurora in the martian atmosphere, using the ultraviolet spectrometer SPICAM on board Mars Express. It corresponds to a distinct type of aurora not seen before in the Solar System: it is unlike aurorae at Earth and the giant planets, which lie at the foot of the intrinsic magnetic field lines near the magnetic poles, and unlike venusian auroras, which are diffuse, sometimes spreading over the entire disk. Instead, the martian aurora is a highly concentrated and localized emission controlled by magnetic field anomalies in the martian crust.