Chaplygin气体与精细结构常数的宇宙学演化(英文)

Chaplygin气体作为暗能量的候选者,可以由标量场来实现.该标量场又同时使得精细结构常数α随着宇宙的演化而演化.在十多年之前,人们对类星体的观测中发现了这一现象,并引起了国内外学者的广泛关注.本文作者考虑了各种Chaplygin气体模型,并与试验进行比较,发现只要暗能量的状态方程参数不是严格等于-1,这些模型都能很好地解释Δα/α的变化.此外,等效原理依然是成立的.     

Deuterium in the Galactic Centre as a result of recent infall of low-metallicity gas

The Galactic Centre is the most active and heavily processed region of the Milky Way, so it can be used as a stringent test for the abundance of deuterium (a sensitive indicator of conditions in the first 1,000 seconds in the life of the Universe). As deuterium is destroyed in stellar interiors, chemical evolution models predict that its Galactic Centre abundance relative to hydrogen is D/H = 5 x 10(-12), unless there is a continuous source of deuterium from relatively primordial (low-metallicity) gas. Here we report the detection of deuterium (in the molecule DCN) in a molecular cloud only 10 parsecs from the Galactic Centre. Our data, when combined with a model of molecular abundances, indicate that D/H = (1.7 +/- 0.3) x 10(-6), five orders of magnitude larger than the predictions of evolutionary models with no continuous source of deuterium. The most probable explanation is recent infall of relatively unprocessed metal-poor gas into the Galactic Centre (at the rate inferred by Wakker). Our measured D/H is nine times less than the local interstellar value, and the lowest D/H observed in the Galaxy. We conclude that the observed Galactic Centre deuterium is cosmological, with an abundance reduced by stellar processing and mixing, and that there is no significant Galactic source of deuterium.     

The signature of the first stars in atomic hydrogen at redshift 20

Dark and baryonic matter moved at different velocities in the early Universe, which strongly suppressed star formation in some regions. This was estimated to imprint a large-scale fluctuation signal of about two millikelvin in the 21-centimetre spectral line of atomic hydrogen associated with stars at a redshift of 20, although this estimate ignored the critical contribution of gas heating due to X-rays and major enhancements of the suppression. A large velocity difference reduces the abundance of haloes and requires the first stars to form in haloes of about a million solar masses, substantially greater than previously expected. Here we report a simulation of the distribution of the first stars at redshift 20 (cosmic age of around 180 million years), incorporating all these ingredients within a 400-megaparsec box. We find that the 21-centimetre hydrogen signature of these stars is an enhanced (ten millikelvin) fluctuation signal on the hundred-megaparsec scale, characterized by a flat power spectrum with prominent baryon acoustic oscillations. The required sensitivity to see this signal is achievable with an integration time of a thousand hours with an instrument like the Murchison Wide-field Array or the Low Frequency Array but designed to operate in the range of 50-100 megahertz.     

建筑环境中有害气体扩散及分布的分析

利用温差射流原理分析了有害气体泄漏时在大气中扩散的特点;在与实验结果对比的基础上,对某建筑小区环境下有害气体连续泄出的扩散迁移过程进行了初步数值计算．结果表明,泄出气体的主运动方向沿大气流动方向发生偏转,气体浓度分布区的范围和形状主要与大气主流风速的大小、建筑物阻挡作用和气体泄出速度等因素相关．     

Stabilization of the disk around beta Pictoris by extremely carbon-rich gas

The edge-on disk surrounding the nearby young star beta Pictoris is the archetype of 'debris disks', which are composed of dust and gas produced by collisions between--and evaporation of--planetesimals, analogues of Solar System comets and asteroids. These disks may provide insight into the formation and early evolution of terrestrial planets. Previous work on beta Pic concluded that the disk gas has roughly solar abundances of elements, but this poses a problem because such gas should rapidly be blown away from the star, contrary to observations showing a stable gas disk in keplerian rotation. Here we report the detection of singly and doubly ionized carbon (C II, C III) and neutral atomic oxygen (O I) gas in the beta Pic disk. Carbon is extremely overabundant relative to every other measured element. This appears to solve the problem of the stable gas disk, because the carbon overabundance should keep the gas disk in keplerian rotation. The overabundance may indicate that the gas is produced from material more carbon-rich than expected of Solar System analogues.     

A disk of dust and molecular gas around a high-mass protostar

The processes leading to the birth of low-mass stars such as our Sun have been well studied, but the formation of high-mass (over eight times the Sun's mass, M(o)) stars remains poorly understood. Recent studies suggest that high-mass stars may form through accretion of material from a circumstellar disk, in essentially the same way as low-mass stars form, rather than through the merging of several low-mass stars. There is as yet, however, no conclusive evidence. Here we report the presence of a flattened disk-like structure around a massive 15M(o) protostar in the Cepheus A region, based on observations of continuum emission from the dust and line emission from the molecular gas. The disk has a radius of about 330 astronomical units (Au) and a mass of 1 to 8 M(o). It is oriented perpendicular to, and spatially coincident with, the central embedded powerful bipolar radio jet, just as is the case with low-mass stars, from which we conclude that high-mass stars can form through accretion.     

Near-infrared flares from accreting gas around the supermassive black hole at the Galactic Centre

Recent measurements of stellar orbits provide compelling evidence that the compact radio source Sagittarius A* (refs 4, 5) at the Galactic Centre is a 3.6-million-solar-mass black hole. Sgr A* is remarkably faint in all wavebands other than the radio region, however, which challenges current theories of matter accretion and radiation surrounding black holes. The black hole's rotation rate is not known, and therefore neither is the structure of space-time around it. Here we report high-resolution infrared observations of Sgr A* that reveal 'quiescent' emission and several flares. The infrared emission originates from within a few milliarcseconds of the black hole, and traces very energetic electrons or moderately hot gas within the innermost accretion region. Two flares exhibit a 17-minute quasi-periodic variability. If the periodicity arises from relativistic modulation of orbiting gas, the emission must come from just outside the event horizon, and the black hole must be rotating at about half of the maximum possible rate.     

非局域引力的宇宙动力学

研究了非局域修改引力的宇宙动力学.发现幂律解是稳定的,而作为幂律解的极限情况德西特(de Sitter)解也是稳定的.在平坦空间中,对于一般的非局域项f,宇宙动力学系统中总存在一个临界点,当态参数w>1/3时,它是吸引子,而w<1/3时,它是鞍点.在非平坦空间中,当物质满足强能量条件时,宇宙动力学系统还存在另一个稳定吸引子,它对应着稳定膨胀的宇宙.数值计算结果证实了上述定性分析的结论.     

原始谱型对黑洞发光环双峰轮廓的影响

黑洞发光环的谱线轮廓具有双峰结构．运用光子输运方程方法将双峰轮廓的数值积分推广到原始谱型为多普勒线型，并讨论原始谱型对轮廓的影响．     

基于非吸附平衡的钻孔周围瓦斯压力分布规律

传统钻孔周围瓦斯压力分布规律研究均以煤体对瓦斯的吸附处于平衡状态为基础,但是,瓦斯流动本身就会使得这种平衡被打破。本研究首先对瓦斯流动条件下的吸附平衡性实验方案进行了设计,并开展了相应的实验研究;在此基础上,对处于非吸附平衡条件下的钻孔周围瓦斯压力分布规律进行了研究,得出了钻孔周围煤层瓦斯压力计算表达式。研究结果表明,在瓦斯流动条件下,煤体对瓦斯的吸附作用处于非平衡状态,钻孔周围煤层瓦斯压力随时间基本呈线性规律下降。采用瓦斯压力指标对预抽煤层瓦斯消突效果进行检验,可能出现低指标突出现象,建议改用瓦斯含量指标。     

类星体吸收线等值宽度的统计分析

对相关文献的1806个MgII（279．6,280．3nm）吸收系统的样本进行了统计分析．发现MgI（285．2nm）,Fell（238．2nm）,FeII（258．7nm）NFell（260．0nm）吸收线也常出现在MgII（279．6,280．3nm）吸收系统中,并且,与MgII（279．6nm）的吸收强度相比,它们的吸收也较强,但是MnlI（257．6nm）NTill（324．2nm）吸收线比较少出现在MglI（279．6,280．3nm）吸收系统中,并且很弱．     

Simulations of the formation, evolution and clustering of galaxies and quasars

The cold dark matter model has become the leading theoretical picture for the formation of structure in the Universe. This model, together with the theory of cosmic inflation, makes a clear prediction for the initial conditions for structure formation and predicts that structures grow hierarchically through gravitational instability. Testing this model requires that the precise measurements delivered by galaxy surveys can be compared to robust and equally precise theoretical calculations. Here we present a simulation of the growth of dark matter structure using 2,160(3) particles, following them from redshift z = 127 to the present in a cube-shaped region 2.230 billion lightyears on a side. In postprocessing, we also follow the formation and evolution of the galaxies and quasars. We show that baryon-induced features in the initial conditions of the Universe are reflected in distorted form in the low-redshift galaxy distribution, an effect that can be used to constrain the nature of dark energy with future generations of observational surveys of galaxies.     

稀薄气体中高超速圆柱绕流仿真研究

高速尤其是高超音速飞行是航空航天发展的主流方向.目前,70 km以上高超音速飞行器的需求越来越大.当飞行高度达到或超过70 km时,稀薄效应明显,此时连续介质假设失效,传统的连续流体运动方程(NS方程)和相应的CFD方法已经失效.利用连续流体运动方程(NS方程)和直接模拟蒙特卡洛方法(DSMC),对四个典型Kn(Kn分别为0.001、0.01、0.1和1)下的圆柱绕流进行了计算.分析比较发现,随着Kn的增大,流场中的激波间断结构变弱变粗,甚至消失,圆柱后方的分离区也逐渐变小直到消失.     

基于一次谐波的光谱吸收式甲烷气体传感器设计

甲烷气体检测是工业生产、环境监测和科学研究领域中的一个重要研究课题.该文在基于波长调制技术的光谱吸收式光纤气体检测方法的基础上,分析了一次谐波信号的数学模型,提出了一种基于一次谐波设计的光纤甲烷气体传感器的实施方案,设计精确的电流和温度电路控制垂直腔面发射激光器,利用锁相放大器AD630提取一次谐波信号幅度,实现对不同浓度的甲烷气体进行测量.实验结果表明,一次谐波信号幅度与浓度存在着很好的线性关系,分辨率达到20ppm.该系统消除了光源波动的影响,工作稳定,简化了结构,调试简便.     

梨树断陷营一段页岩气资源评价

由于我国页岩气勘探开发仍处于不成熟阶段,页岩气资源评价需用多种方法。通过对目的层段的钻井取心及对取心资料的地球化学分析、X衍射资料、扫描电镜等资料分析,结合研究区页岩气成藏条件,基于有机质丰度、有机质成熟度、泥页岩厚度、埋深和地表条件等5方面,建立了页岩气远景区、有利区和目标区优选参数体系,并采用概率体积法计算出了其地质资源量。研究发现梨树断陷页岩气丰富,具有巨大的勘探潜力。     

沈阳周边矿区开发煤层气的研究

沈阳周边的铁法、抚顺和沈南矿区，煤层气含量高、煤层气储量大、储量可靠，具有形成规模开发的资源条件；各矿区煤层气井下抽放及利用工作开展得较早，发展速度快，地面钻井开发通过在各矿区的试验，取得了一定的开发经验，采用进下抽放与地面钻井相结合的开发方式，煤层气资源的开发具有较好的经济效益。沈阳市有巨大的需求。     

用蒸发气充填液化天然气球形储罐隔热层的传热计算

针对大型液化天然气储罐在隔热层填充N2(氮气)成本高、工艺复杂的问题,现改为用BOG(蒸发气体)代替N2填充隔热层.阐述BOG代替N2的不同及其用球形储罐储存LNG的优点.通过分析传热过程、建立传热模型,计算总漏热量和蒸发率,验证BOG代替N2在理论上的可行性.