全新运载火箭圆宇宙航行之梦

星际航行可分为行星际航行和恒星际航行。行星际航行是指,冲破地球引力的束缚在太阳系范围内进行航行,又称航天飞行;恒星际航行是指脱离太阳系到银河系和河外星系中进行航行,又称宇宙航行。目前,人类已经实现了环绕地球的飞行,登上了月球,“勇气”号、“机遇”号也相继成功登上了火星。但是,要实现宇宙航行,还有许多问题需要解决。     

事实的客观性蕴涵着主体性和客体性

事实的客观性就内在地蕴涵着事实的主体性和客体性。“事实是表征物质世界客观存在和运动的具体状态、现实环节的概念”这一界说就内涵着事实的主体性，因为人的主体性活动本身就是“物质的各种实在形式和运动形式”中的一种具体形式。《论事实的客观性》实际上区分了事实的本体论意义和认识论意义并着重分析了其认识论意义，指出认识论意义上的事实是具体的、历史的、进入主体现实的求是活动范围的事物及其情况。问题的实质在于如何理解事实的主体性。笔者的观点是：不能把事实的主体性归结为事实“是人对事物的一种意识和断定”、“是人所把握的一种知识形式”。     

幂拓扑分子格的积

引入形如（Ｌ＾Ｘ，η）的拓扑分子格（称为幂拓扑分子格）族的“Ｘ积”和“积”以及幂扑分子格的“核”（核是分明拓扑空间），证明了幂拓扑分子格的分明性、弱诱导必和弱层性积性和可积性，对弱诱导的幂拓年分子格式，积之核等于核之积。     

星际弥散吸收带

星际弥散带（diffuse interstellar bands;DIBs）是源自星际空间的数百条吸收谱线的总称．自20世纪20年代首次发现两条DIBs以来,对DIBs的观测和证认已有80多年的历史．迄今为止,共观测到了300多条DIBs,但没有一条DIB的载体（carrier）被完全证认．DIBs的证认被认为是困扰着天文学家80多年的天体物理学的经典难题之一．我们简要回顾了星际弥散带的观测历史,介绍了银河系和河外星系星际弥散带的一些观测特征、星际紫外消光2175A驼峰强度和星际弥散带的相关性、星际弥散带之间的相关性和星际弥散带的分类方法;对星周环境中是否存在弥散吸收带的观测结果也给予了简要的评述;讨论了星际弥散带的载体和起源．     

与HⅡ区成协的星际脉泽激发机制

从紫外光子与星际分子的相互作用出发,对与HⅡ区成协的星际脉泽提出了一种重要的激发机制.它能统一解释星际OH和水2种脉泽,并能满足各种天文条件,克服了以往某些模型的困难.     

高职英语教学中小组活动的有效性探究——以湖南工程职业技术学院英语教改专业为例

小组活动教学是“可理解性输入”理论和“可理解性输出”理论的实际运用。本文以湖南工程职业技术学院英语教改专业进行小组活动教学为例，分析了小组活动教学的开展方式以及效果。     

图式理论与英语阅读理解

介绍了图式和图式理论，论述了图式理论在英语阅读理解的作用，指出阅读理解过程不仅是认词释义的过程，而且是心理因素和背景知识相互作用的过程，读者应使用“自下而上”和“自上而下”两种阅读方法，才能获得有效的阅读。     

700光年外发现太空中迄今最复杂有机分子

<正>科学网6月25日消息,天文学家在银河系星际气体中发现了一种新的复杂分子。来自法国的一家天文学研究机构和德克萨斯大学的天文学家,在星际介质中发现了迄今为止最为复杂的有机分子:蒽(anthracene)。     

论现代西方结构主义语言学对客观性语义的辩护及后结构语言学对它的消解

现代结构主义语言学主张文本的意义并不完全是客观、僵化、静态地凝固于文本之中的东西,而是与理解活动密不可分的,是历史性与当代性两种视域双向互动、实践整合过程中所生成的一种交往互惠,是文本理解者对生活经验的未来发展做出的可能性筹划。但是在后结构语言学看来,唯有对客观性语义进行颠倒和延异,用语言的历时性演变和同时性扩张,才能完成语言创新,恢复语言的多义性、表达的隐喻性、意义的可增生性。因为,任何语言认知都具有非结构性、意义的不确定性,任何语言系统都存在内在差异性和离散性,这恰恰导致了语言认知的游戏性和理解的任意性。因而,语义并非客观性地存在着,并非来自外部实在,而是来自延异性、离散性的语言游戏及其流变中。     

星际空间中的碳尘埃

碳是宇宙中仅次于氢、氦、氧的第4丰富的元素.在恒星演化晚期形成的碳元素,进入星际空间以后,以离子、原子、分子以及固体尘埃微粒的多种形式存在.含碳有机复杂分子是生命起源的基本物质.碳质尘埃是星际尘埃的主要成分之一,其红外光谱是探测各种天体环境物理和化学条件的重要指针.碳质尘埃如石墨、纳米金刚石、多环芳香烃、富勒烯、氢化非结晶碳等尘埃微粒是星际尘埃的重要研究对象,在星际空间广泛存在,它们是星际消光2175?驼峰、星际红外辐射谱带、星际弥散吸收带等光谱特征的最可能载体.本文主要介绍星际碳质尘埃的天文观测及其物理化学特性.近年来,石墨烯、碳纳米管逐渐进入人们的视野,本文亦将讨论与此相关的天文观测和理论模型的最新进展.     

Sublimation from icy jets as a probe of the interstellar volatile content of comets

Comets are some of the most primitive bodies left over from the Solar System's early history. They may preserve both interstellar material and material from the proto-solar nebula, and so studies of their volatile components can provide clues about the evolution of gases and ices, as a collapsing molecular cloud transforms into a mature planetary system. Previous observations of emission from rotational transitions in molecules have averaged over large areas of the inner coma, and therefore include both molecules that sublimed from the nucleus and those that result from subsequent chemical processes in the coma Here we present high-resolution observations of emission from the molecules HNC, DCN and HDO associated with comet Hale-Bopp. Our data reveal arc-like structures-icy jets-offset from (but close to) the nucleus. The measured abundance ratios on 1-3" scales are substantially different from those on larger scales, and cannot be accounted for by models of chemical processes in the coma; they are, however, similar to the values observed in the cores of dense interstellar clouds and young stellar objects. We therefore propose that sublimation from millimetre-sized icy grains ejected from the nucleus provides access to relatively unaltered volatiles. The D/H ratios inferred from our data suggest that, by mass, Hale-Bopp (and by inference the outer regions of the early solar nebula) consists of > or =15-40% of largely unprocessed interstellar material.     

Mixed aromatic-aliphatic organic nanoparticles as carriers of unidentified infrared emission features

Unidentified infrared emission bands at wavelengths of 3-20 micrometres are widely observed in a range of environments in our Galaxy and in others. Some features have been identified as the stretching and bending modes of aromatic compounds, and are commonly attributed to polycyclic aromatic hydrocarbon molecules. The central argument supporting this attribution is that single-photon excitation of the molecule can account for the unidentified infrared emission features observed in 'cirrus' clouds in the diffuse interstellar medium. Of the more than 160 molecules identified in the circumstellar and interstellar environments, however, not one is a polycyclic aromatic hydrocarbon molecule. The detections of discrete and broad aliphatic spectral features suggest that the carrier of the unidentified infrared emission features cannot be a pure aromatic compound. Here we report an analysis of archival spectroscopic observations and demonstrate that the data are most consistent with the carriers being amorphous organic solids with a mixed aromatic-aliphatic structure. This structure is similar to that of the organic materials found in meteorites, as would be expected if the Solar System had inherited these organic materials from interstellar sources.     

Racemic amino acids from the ultraviolet photolysis of interstellar ice analogues

The delivery of extraterrestrial organic molecules to Earth by meteorites may have been important for the origin and early evolution of life. Indigenous amino acids have been found in meteorites-over 70 in the Murchison meteorite alone. Although it has been generally accepted that the meteoritic amino acids formed in liquid water on a parent body, the water in the Murchison meteorite is depleted in deuterium relative to the indigenous organic acids. Moreover, the meteoritical evidence for an excess of laevo-rotatory amino acids is hard to understand in the context of liquid-water reactions on meteorite parent bodies. Here we report a laboratory demonstration that glycine, alanine and serine naturally form from ultraviolet photolysis of the analogues of icy interstellar grains. Such amino acids would naturally have a deuterium excess similar to that seen in interstellar molecular clouds, and the formation process could also result in enantiomeric excesses if the incident radiation is circularly polarized. These results suggest that at least some meteoritic amino acids are the result of interstellar photochemistry, rather than formation in liquid water on an early Solar System body.     

A new interstellar molecule: tricarbon monoxide

The cold dark interstellar Taurus Molecular Cloud One (TMC-1) is a rich source of acetylenic and polyacetylenic molecular species. As well as linear closed-shell molecules (H(C triple bond C)nCN) and symmetric rotors (CH3C triple bond CH, CH3C triple bond CCN), several radicals (C triple bond CH, C triple bond CCN, (C triple bond C2H) have also been identified, many of which had not been studied previously in the laboratory. Whether the observed abundances can be understood in terms of purely gas-phase ion-molecule chemical schemes, which produce reasonable agreement for the simplest polyatomic species, is unclear; alternative models involving the particulate interstellar grains as catalysts or sources have also been suggested. We now report the detection in TMC-1 of a new molecule, tricarbon monoxide (C3O), whose pure rotational spectrum has only very recently been studied in the laboratory. As C3O is the first known interstellar carbon chain molecule to contain oxygen, its existence places an important new constraint on chemical schemes for cold interstellar clouds. In fact, the observed abundance of tricarbon monoxide fits quite well into our model of galactochemistry.     

Infrared diffuse interstellar bands in the Galactic Centre region

The spectrum of any star viewed through a sufficient quantity of diffuse interstellar material reveals a number of absorption features collectively called 'diffuse interstellar bands' (DIBs). The first DIBs were reported about 90 years ago, and currently well over 500 are known. None of them has been convincingly identified with any specific element or molecule, although recent studies suggest that the DIB carriers are polyatomic molecules containing carbon. Most of the DIBs currently known are at visible and very near-infrared wavelengths, with only two previously known at wavelengths beyond one micrometre (10,000 ?ngstr?ms), the longer of which is at 1.318?micrometres (ref. 6). Here we report 13 diffuse interstellar bands in the 1.5-1.8 micrometre interval on high-extinction sightlines towards stars in the Galactic Centre. We argue that they originate almost entirely in the Galactic Centre region, a considerably warmer and harsher environment than where DIBs have been observed previously. The relative strengths of these DIBs towards the Galactic Centre and the Cygnus OB2 diffuse cloud are consistent with their strengths scaling mainly with the extinction by diffuse material.     

Amino acids from ultraviolet irradiation of interstellar ice analogues

Amino acids are the essential molecular components of living organisms on Earth, but the proposed mechanisms for their spontaneous generation have been unable to account for their presence in Earth's early history. The delivery of extraterrestrial organic compounds has been proposed as an alternative to generation on Earth, and some amino acids have been found in several meteorites. Here we report the detection of amino acids in the room-temperature residue of an interstellar ice analogue that was ultraviolet-irradiated in a high vacuum at 12 K. We identified 16 amino acids; the chiral ones showed enantiomeric separation. Some of the identified amino acids are also found in meteorites. Our results demonstrate that the spontaneous generation of amino acids in the interstellar medium is possible, supporting the suggestion that prebiotic molecules could have been delivered to the early Earth by cometary dust, meteorites or interplanetary dust particles.     

Identification of molecular-cloud material in interplanetary dust particles

Interplanetary dust particles (IDPs) collected in the Earth's stratosphere and meteorites are fragments of comets and asteroids. These are 'primitive' meteorites in part because they have preserved materials which predate the formation of the Solar System. The most primitive (least altered) meteorites contain a few parts per million of micrometre-sized dust which formed in the atmospheres of giant stars. Some meteorites have elevated D/H and 15N/14N ratios that are attributed to surviving interstellar organic molecules which have probably been strongly diluted and altered by parent-body processes. Most IDPs are chemically, mineralogically, and texturally primitive in comparison to meteorites. Here I show that H and N isotopic anomalies among fragile 'cluster' IDPs are far larger, more common, and less equilibrated than those previously observed in other IDPs or meteorites. In some cases, the D/H ratios that we measure reach the values of interstellar molecules, suggesting that molecular-cloud material has survived intact. These observations indicate that cluster IDPs are the most primitive class of Solar System materials currently available for laboratory analysis.     

星际C60

C60的发现起源于人们对星际尘埃的探索,肇始于1985年由Kroto等人首次在实验室合成,25年后最终于2010年在星际空间被探测到．近几年天文工作者在多种星周、星际环境观测到C60．本文综述了与天文观测和理论密切相关的C60的有关物理性质;介绍了C60在星际空间中的观测特性;最后讨论了C60在星际空间的形成与激发机制．     

中药材人参鉴定技术方法的研究与评价

主要探讨现有的人参鉴定传统方法和分子生物学方法在鉴定过程中的准确性和客观性,综述了聚合酶链式反应(Polymerase Chain Reaction,PCR)、随机扩增多态性DNA标记(Randomly Amplified Polymorphic DNA,RAPD)、限制性片段长度多态性分析(Restriction Fragment Length Polymorphism,RFLP)、扩增片段长度多态性分析(Amplified Fragment Length Polymorphism,AFLP)、多位点探针DNA指纹图谱和微卫星标记技术(SSR)等在人参物种鉴定中的应用,并对每种技术进行了相应的评价.     

An enhanced cosmic-ray flux towards zeta Persei inferred from a laboratory study of the H3+-e- recombination rate

The H3+ molecular ion plays a fundamental role in interstellar chemistry, as it initiates a network of chemical reactions that produce many molecules. In dense interstellar clouds, the H3+ abundance is understood using a simple chemical model, from which observations of H3+ yield valuable estimates of cloud path length, density and temperature. But observations of diffuse clouds have suggested that H3+ is considerably more abundant than expected from the chemical models. Models of diffuse clouds have, however, been hampered by the uncertain values of three key parameters: the rate of H3+ destruction by electrons (e-), the electron fraction, and the cosmic-ray ionization rate. Here we report a direct experimental measurement of the H3+ destruction rate under nearly interstellar conditions. We also report the observation of H3+ in a diffuse cloud (towards Persei) where the electron fraction is already known. From these, we find that the cosmic-ray ionization rate along this line of sight is 40 times faster than previously assumed. If such a high cosmic-ray flux is ubiquitous in diffuse clouds, the discrepancy between chemical models and the previous observations of H3+ can be resolved.