The formation of stars by gravitational collapse rather than competitive accretion

There are two dominant models of how stars form. Under gravitational collapse, star-forming molecular clumps, of typically hundreds to thousands of solar masses (M(o)), fragment into gaseous cores that subsequently collapse to make individual stars or small multiple systems. In contrast, competitive accretion theory suggests that at birth all stars are much smaller than the typical stellar mass (approximately 0.5M(o)), and that final stellar masses are determined by the subsequent accretion of unbound gas from the clump. Competitive accretion models interpret brown dwarfs and free-floating planets as protostars ejected from star-forming clumps before they have accreted much mass; key predictions of this model are that such objects should lack disks, have high velocity dispersions, form more frequently in denser clumps, and that the mean stellar mass should vary within the Galaxy. Here we derive the rate of competitive accretion as a function of the star-forming environment, based partly on simulation, and determine in what types of environments competitive accretion can occur. We show that no observed star-forming region can undergo significant competitive accretion, and that the simulations that show competitive accretion do so because the assumed properties differ from those determined by observation. Our result shows that stars form by gravitational collapse, and explains why observations have failed to confirm predictions of the competitive accretion model.     

The formation of a massive protostar through the disk accretion of gas

The formation of low-mass stars like our Sun can be explained by the gravitational collapse of a molecular cloud fragment into a protostellar core and the subsequent accretion of gas and dust from the surrounding interstellar medium. Theoretical considerations suggest that the radiation pressure from the protostar on the in-falling material may prevent the formation of stars above ten solar masses through this mechanism, although some calculations have claimed that stars up to 40 solar masses can in principle be formed via accretion through a disk. Given this uncertainty and the fact that most massive stars are born in dense clusters, it was suggested that high-mass stars are the result of the runaway merging of intermediate-mass stars. Here we report observations that clearly show a massive star being born from a large rotating accretion disk. The protostar has already assembled about 20 solar masses, and the accretion process is still going on. The gas reservoir of the circumstellar disk contains at least 100 solar masses of additional gas, providing sufficient fuel for substantial further growth of the forming star.     

Imprints of fast-rotating massive stars in the Galactic Bulge

The first stars that formed after the Big Bang were probably massive, and they provided the Universe with the first elements heavier than helium ('metals'), which were incorporated into low-mass stars that have survived to the present. Eight stars in the oldest globular cluster in the Galaxy, NGC?6522, were found to have surface abundances consistent with the gas from which they formed being enriched by massive stars (that is, with higher α-element/Fe and Eu/Fe ratios than those of the Sun). However, the same stars have anomalously high abundances of Ba and La with respect to Fe, which usually arises through nucleosynthesis in low-mass stars (via the slow-neutron-capture process, or s-process). Recent theory suggests that metal-poor fast-rotating massive stars are able to boost the s-process yields by up to four orders of magnitude, which might provide a solution to this contradiction. Here we report a reanalysis of the earlier spectra, which reveals that Y and Sr are also overabundant with respect to Fe, showing a large scatter similar to that observed in extremely metal-poor stars, whereas C abundances are not enhanced. This pattern is best explained as originating in metal-poor fast-rotating massive stars, which might point to a common property of the first stellar generations and even of the 'first stars'.     

The formation of the first low-mass stars from gas with low carbon and oxygen abundances

The first stars in the Universe are predicted to have been much more massive than the Sun. Gravitational condensation, accompanied by cooling of the primordial gas via molecular hydrogen, yields a minimum fragmentation scale of a few hundred solar masses. Numerical simulations indicate that once a gas clump acquires this mass it undergoes a slow, quasi-hydrostatic contraction without further fragmentation; lower-mass stars cannot form. Here we show that as soon as the primordial gas--left over from the Big Bang--is enriched by elements ejected from supernovae to a carbon or oxygen abundance as small as approximately 0.01-0.1 per cent of that found in the Sun, cooling by singly ionized carbon or neutral oxygen can lead to the formation of low-mass stars by allowing cloud fragmentation to smaller clumps. This mechanism naturally accommodates the recent discovery of solar-mass stars with unusually low iron abundances (10(-5.3) solar) but with relatively high (10(-1.3) solar) carbon abundance. The critical abundances that we derive can be used to identify those metal-poor stars in our Galaxy with elemental patterns imprinted by the first supernovae. We also find that the minimum stellar mass at early epochs is partially regulated by the temperature of the cosmic microwave background.     

大康留日月星辰汉画像石考

山东滕州大康留日月星辰汉画像石为东汉中晚期画像石鼎盛时期之佳作,其上标绘日月星辰等天文图像,反映了汉代劳动人民对天文知识的了解及记录,其雕刻技法娴熟多样,画面舒展流畅,形象逼真.     

英吉苏凹陷天然气藏成岩演化模式及成藏机理

在对英吉苏凹陷基本地质条件、次生孔隙的形成、成岩序列分析及成岩演化阶段划分的基础上,建立了英吉苏凹陷天然气藏的成岩演化模式,研究了英吉苏凹陷天然气的成藏机理,建立了成藏模式.结果表明:英吉苏凹陷具备了形成大中型气藏的地质条件和成藏要素.研究结论对塔里木盆地气藏分布规律的研究以及寻找新的油气资源提供必要的依据.     

页岩气层钻井压力穿透效应研究

页岩段井壁稳定问题是钻井工程中的难点之一,国内外许多学者在研究钻井液与页岩之间的化学势差和水化膨胀作用方面作了大量工作,但对于压力穿透方面的研究工作则相对较少。为此,通过在压力容器中充满钻井液,模拟近井壁过平衡钻井所导致的压力穿透环境,测量压力对垂直于页岩层理和平行于页岩层理方向应变的影响。结果表明,垂直于层理方向的应变随压力增大呈现出显著的阶梯式变化,同一压力作用时页岩压力穿透效应具有时间延迟效应和各向异性。通过理论分析发现,在页岩有效孔隙度一定的条件下,页岩压力穿透效应主要受滤饼渗透率、钻井液液柱压力与地层孔隙流体压力之间的压差、页岩与钻井液接触时间以及钻井液黏度的综合作用。页岩压力穿透效应对研究页岩段钻井过程中井壁稳定与控制具有重要意义。     

非煤系地层隧道围岩有害气体形成机制

大量在建和拟建隧道面临非煤系地层有害气体的挑战,厘清非煤系地层隧道围岩有害气体形成机制是解决该问题的基础。基于此,综述了我国非煤系地层隧道围岩有害气体形成机制研究的最新进展,总结了非煤系地层有害气体主要类型,探讨了地质条件对于有害气体形成的影响机理,分析了有害气体的孕育机制,展望了非煤系地层隧道有害气体问题的研究方向。研究表明：非煤系地层隧道有害气体大体可按照成因分为构造连通型、围岩变质型和综合成因型;大型断裂、褶皱及深部循环的水热型高温导热带等地质构造对非煤系地层隧道围岩有害气体的形成、赋存和溢出起到关键作用;CH4、H2S和CO2等的来源相似,但物理化学性质的差异导致其形成机制不同;复杂地质构造、复合组分隧道围岩有害气体的孕育及运移模式、固-液-热-力多场耦合机制等方面值得进一步研究。研究对于非煤系地层隧道围岩有害气体防治的实践和研究具有积极意义。     

建国以来孙中山经济思想研究综述

经济思想是孙中山思想最具特色的部分。建国以来，研究研究的主要内容包括：“平均地权”与“耕有田”、国民经济建设思想、与近现代重要人物经济思想的比较等方面。     

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.     

The critical role of disks in the formation of high-mass stars

Although massive stars (commonly defined as those in excess of about eight solar masses, or with initial luminosities of a thousand times the solar luminosity or more) have an enormous impact on the galactic environment, how they form has been a mystery. The solution probably involves the existence of accretion disks. Rotational motions have been found in the gas surrounding young high-mass stars, which suggests that non-spherical accretion could be the fundamental ingredient of the massive-star formation recipe.     

"人少任务多"最小分派问题的一种解法

通过对“人少任务多”最小分派问题的解法探析，指出了“加边补零法”的局限性，并得到了一种新的解法——“加边补最小值”法，算例显示此法在n-m=1时优于其它算法。     

应用激光研究瓦斯爆炸的机理

依据气态反应的自由基机制和多原子分子光谱理论,提出用激光研究瓦斯爆炸的机理。利用自行设计的实验装置,在4种激光波长和8种瓦斯浓度下进行实验。初步实验表明,这种方法是可行的,可望获得矿井下激光安全应用的条件。     

准噶尔盆地车排子凸起隐蔽油气藏成藏机理

综合运用地质、地球物理、油气藏地球化学及盆地模拟领域中先进的技术与研究方法,以盆地演化和流体输导格架为成藏背景,从有效烃源岩及其生排烃历史出发,以能量场演化及其控制的化学动力学、流体动力学和运动学过程为核心,探讨了准噶尔盆地车排子凸起隐蔽油气藏的成藏机理.研究表明,油气藏主要以昌吉凹陷二叠系和四棵树凹陷侏罗系油气2期充注混源而成,油气分别以早期净浮力、晚期强超压为驱动机制,以不整合/区域性砂体、构造断裂为优势运移通道构成2源2期充注、阶梯式输导、地层/岩性型聚集的成藏模式.     

大牛地奥陶系马五段硫化氢腐蚀机理与影响因素

为了解决大牛地气田硫化氢腐蚀严重问题,分析了硫化氢腐蚀机理以及影响腐蚀程度的因素。结合大牛地奥陶系马家沟组马五段地质条件以及硫化氢赋存条件确定该区域硫化氢形成的机理,为硫酸盐热化学还原反应;且该区域存在的大量石膏层为含硫化氢气体提供了良好的圈闭条件。硫化氢腐蚀模拟试验模拟了马五段地层水环境对N80钢和P110钢的腐蚀程度,P110钢的腐蚀程度较N80钢轻微,两者均属于极严重腐蚀。结合腐蚀表面微观形貌观测与腐蚀产物能谱分析得出:大牛地奥陶系马家沟组马五段硫化氢腐蚀机理为高温高压下CO2/H2S电化学腐蚀为主;并伴随有高Cl-破坏腐蚀产物膜加速腐蚀。硫化氢腐蚀影响因素分析得出温度和CO2含量增加会加速硫化氢腐蚀。     

异常高压气藏储层应力敏感性研究

异常高压气藏开采过程中,由于流体的产出,使储层岩石受力发生改变并使储层岩石发生弹塑性变形;而弹塑性变形反过来又影响到储层的孔隙度和渗透率,因此,研究储层孔隙度和渗透率应力敏感性具有极其重要的意义.本文基于岩石力学的基本理论,推导出异常高压气藏岩石变形规律及变形方程,以此理论推导指导试验,将理论研究与实验规律相结合,在模拟地层条件下,对实际岩心样品进行了储层应力敏感性实验研究.实验研究表明,该方法能精确的描述储层孔隙度和渗透率应力敏感性,实验结果与理论推导结果完全吻合,进一步证明了理论推导的正确.进而探讨了异常高压气藏储层应力敏感性对气藏开发的影响.     

清洁发展机制对温室气体减排的贡献

为判断碳市场的规模和作用,应用一个全球碳排放贸易局部均衡模型研究清洁发展机制(CDM)的市场潜力和结构,讨论它对全球温室气体减排的贡献.计算显示,京都议定书第一承诺期中国CDM的市场规模(CO2当量)为2.2亿t, 占CDM市场总量的40%.如果只有联合履行和排放贸易机制而没有CDM, 附件1国家的总履约成本将比目前高67%;中国CDM市场使附件1国家在第一承诺期的履约成本降低23%.热空气比例和CDM交易成本是影响CDM市场结构的2个主要敏感参数.