Energy input from quasars regulates the growth and activity of black holes and their host galaxies

In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars. Supermassive black holes are found at the centres of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy. This suggests a link between the growth of the black holes and their host galaxies, which has indeed been assumed for a number of years. But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies, have remained unclear. Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions. We find that, in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar. The energy released by the quasar expels enough gas to quench both star formation and further black hole growth. This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.     

河外星系恒星形成的物理规律探讨

冷气体(T<20 K)是星系中恒星形成(SF)的原料,冷气体随引力塌缩成致密分子云核并终将继续塌缩转变成SF到恒星,而SF反馈又推动着星系的形成和演化.详细了解气体的性质,描绘SF和星系的物理关联以及SF对星系的反馈等,是当今极为重要的关键研究.本文主要总结了河外星系中SF的物理规律,探讨了SF与冷气体的相关关系,特别是随着对SF的进一步物理认识,归纳了我们对SF与致密气体关系的系列相关研究,从河外星系整体的研究到对近邻星系空间分解以及与银河系内致密云核的跨度10个数量级的关系;甚至是对更高密度的致密气体,从星系整体到近邻星系空间分解以及河内致密云核的跨度10个数量级的线性相关关系,并指出在ALMA时代SF研究方向的未来发展前景.JCMT的大项目MALATANG提供了对极高密度致密分子气体在近邻星系中大规模分布和SF的认识,了解在星系的中心和更广阔的漩涡盘区各种不同气体状态与致密分子气体和SF之间的物理关联,以及SF和致密分子气体在不同物理尺度上的联系等.随着ALMA/NOEMA的观测推进以及下一代望远镜的投入,有望最终获得不论是遥远或近邻星系从分子云尺度到星系局部、整体各个不同物理尺度上对致密气体和SF的物理性质和规律、多谱线诊断和星系局部SF效率等前沿问题的突破性认识.     

星系中心大黑洞的宇宙学演化

在冷暗物质晕等级成团宇宙学模型中,伴随着暗物质晕并合,星系中心黑洞也断地并合和增长.于展Press-Schechter公式（EPS）我们编写了一自适应时间长Monte Carlo程序,重构了表征暗物质晕等级成团并合树.在成功地建立了黑洞和暗物质晕宇宙学演化模型后,我们通过引入直接吸积（包标准薄盘吸积和磁流体力学吸积）和随吸积两类黑洞吸积模式,论了黑洞自旋和质量宇宙学演化.通过与观测到AGN光度函数比较,我们发现黑洞通过磁流体力学吸积模式增长,与观测符合最好.于以上理论框架,我们还研究了双大质量黑洞演化,发现双黑洞通过共转气体吸积盘吸积对双黑洞质量比分存在显著影响.     

The formation of cluster elliptical galaxies as revealed by extensive star formation

The most massive galaxies in the present-day Universe are found to lie in the centres of rich clusters. They have old, coeval stellar populations suggesting that the bulk of their stars must have formed at early epochs in spectacular starbursts, which should be luminous phenomena when observed at submillimetre wavelengths. The most popular model of galaxy formation predicts that these galaxies form in proto-clusters at high-density peaks in the early Universe. Such peaks are indicated by massive high-redshift radio galaxies. Here we report deep submillimetre mapping of seven high-redshift radio galaxies and their environments. These data confirm not only the presence of spatially extended regions of massive star-formation activity in the radio galaxies themselves, but also in companion objects previously undetected at any wavelength. The prevalence, orientation, and inferred masses of these submillimetre companion galaxies suggest that we are witnessing the synchronous formation of the most luminous elliptical galaxies found today at the centres of rich clusters of galaxies.     

Rapid evolution of the most luminous galaxies during the first 900 million years

The first 900 million years (Myr) to redshift z approximately 6 (the first seven per cent of the age of the Universe) remains largely unexplored for the formation of galaxies. Large samples of galaxies have been found at z approximately 6 (refs 1-4) but detections at earlier times are uncertain and unreliable. It is not at all clear how galaxies built up from the first stars when the Universe was about 300 Myr old (z approximately 12-15) to z approximately 6, just 600 Myr later. Here we report the results of a search for galaxies at z approximately 7-8, about 700 Myr after the Big Bang, using the deepest near-infrared and optical images ever taken. Under conservative selection criteria we find only one candidate galaxy at z approximately 7-8, where ten would be expected if there were no evolution in the galaxy population between z approximately 7-8 and z approximately 6. Using less conservative criteria, there are four candidates, where 17 would be expected with no evolution. This demonstrates that very luminous galaxies are quite rare 700 Myr after the Big Bang. The simplest explanation is that the Universe is just too young to have built up many luminous galaxies at z approximately 7-8 by the hierarchical merging of small galaxies.     

The evolution of galaxies from primeval irregulars to present-day ellipticals

Galaxy formation is believed to proceed in a 'bottom up' manner, starting with the formation of small clumps of gas and stars that then merge hierarchically into giant systems. The baryonic gas loses thermal energy by radiative cooling and falls towards the centres of the new galaxies, while supernovae blow gas out. Any realistic model therefore requires a proper treatment of these processes, but hitherto this has been far from satisfactory. Here we report a simulation that follows evolution from the earliest stages of galaxy formation through the period of dynamical relaxation, at which point the resulting galaxy is in its final form. The bubble structures of gas revealed in our simulation (for times of less than 3 x 10(8) years) resemble closely high-redshift Lyman-alpha emitters. After 10(9) years, these bodies are dominated by stellar continuum radiation and then resemble the Lyman break galaxies, which are high-redshift star-forming galaxies. At this point, the abundance of elements heavier than helium ('metallicity') appears to be solar. After 1.3 x 10(10) years, these galaxies resemble present-day ellipticals.     

嵩山主峰的形成及演变

对河南嵩山主蜂的形成和演变过程进行了分析讨论.嵩山地区地层的分布、沉积岩的岩性特征、地层闻的接触关系等证据,表明从古生代直至中生代嵩山并不存在.通过对嵩山山前新生代沉积盆地沉积和作为嵩山断块山和山前断陷盆地分界的君召-太后庙断层构造岩带的研究,证明现今的嵩山应当是在印支-燕山运动中孕育,在喜马拉雅运动中出生并长高的山脉.嵩山的成长过程可分为孕育、幼年、童年和青年阶段.嵩山在形成后主蜂不断向北推移,推移距离达6.5 km,隆起的铅直高度在7 km以上.嵩山和中国大地其他山脉,如喜马拉雅山、天山、昆仑山、秦岭等,是同一辈份的年青山脉.     

渤南凹陷构造演化与超压形成及演化过程的关系分析

盆地的构造演化通过构造活动、沉积体系控制了异常压力的发育,同时异常压力的存在对后期形成的断层有影响.本文通过双元孔隙度演化函数建模对渤南凹陷的古压力进行了恢复,研究表明,渤南凹陷的异常压力主要在裂陷期末开始发育,在坳陷期达到最大.同时由于异常压力的存在引起了流体压裂,对南部缓坡带盆倾断层的形成具有诱导作用.     

High star formation rates as the origin of turbulence in early and modern disk galaxies

Observations of star formation and kinematics in early galaxies at high spatial and spectral resolution have shown that two-thirds are massive rotating disk galaxies, with the remainder being less massive non-rotating objects. The line-of-sight-averaged velocity dispersions are typically five times higher than in today's disk galaxies. This suggests that gravitationally unstable, gas-rich disks in the early Universe are fuelled by cold, dense accreting gas flowing along cosmic filaments and penetrating hot galactic gas halos. These accreting flows, however, have not been observed, and cosmic accretion cannot power the observed level of turbulence. Here we report observations of a sample of rare, high-velocity-dispersion disk galaxies in the nearby Universe where cold accretion is unlikely to drive their high star formation rates. We find that their velocity dispersions are correlated with their star formation rates, but not their masses or gas fractions, which suggests that star formation is the energetic driver of galaxy disk turbulence at all cosmic epochs.     

百色盆地古近系那读组和百岗组层序地层划分与沉积演化

野外剖面显示百色盆地古近系那读组内部、那读组与百岗组之间存在不整合面。综合分析地震、测井等资料,将盆地古近系那读组和百岗组划分为1个二级层序,3个三级层序。那读组那三段构成三级层序的层序Ⅰ,那读组那二和那一段构成三级层序的层序Ⅱ,百岗组构成三级层序的层序Ⅲ。层序Ⅰ和层序Ⅱ是盆地断陷期的沉积,具有相似的充填特征,层序Ⅲ是盆地坳陷期的沉积。层序Ⅱ既发育厚度大、分布范围广的深湖亚相泥岩,又发育河流相、三角洲相和扇三角洲相砂岩,是盆地内主要的生储盖组合发育层序。盆地北部层序Ⅱ,Ⅲ发育的扇三角洲是盆地有利储集岩。各层序低水位体系域发育长轴分布的河流相和三角洲相砂岩,这些砂岩是盆地隐蔽性圈闭勘探的有利储层。     

百色盆地古近系那读组和百岗组层序地层划分与沉积演化

野外剖面显示百色盆地古近系那读组内部、那读组与百岗组之间存在不整合面。综合分析地震、测井等资料,将盆地古近系那读组和百岗组划分为1个二级层序,3个三级层序。那读组那三段构成三级层序的层序Ⅰ,那渎组那二和那一段构成三级层序的层序Ⅱ,百岗组构成三级层序的层序Ⅲ。层序Ⅰ和层序Ⅱ是盆地断陷期的沉积,具有相似的充填特征,层序Ⅲ是盆地坳陷期的沉积。层序Ⅱ既发育厚度大、分布范围广的深湖亚相泥岩,又发育河流相、三角洲相和扇三角洲相砂岩,是盆地内主要的生储盖组合发育层序。盆地北部层序Ⅱ,Ⅲ发育的扇三角洲是盆地有利储集岩。各层序低水位体系域发育长轴分布的河流相和三角洲相砂岩,这些砂岩是盆地隐蔽性圈闭勘探的有利储层。     

可变的广义Chaplygin气体的演化及其结构形成

在Friedmann理论框架下,将可变的广义Chaplygin气体（VGCG）作为一种暗能量模型,研究了与其相关的宇宙学量的演化规律.在此基础上,通过导出相关的物理量（诸如：物质的密度反差,增长变量和增长因子）所满足的运动方程,并对其求数值解,我们不仅给出了它们的演化图,深入探讨了相应的演化规律,而且还与ΛCDM模型做比较,讨论了此暗能量模型对宇宙结构形成的影响.研究结果表明,当今宇宙是从过去的减速膨胀演化为现在乃至将来的加速膨胀,并且在近阶段可以模拟ΛCDM模型的演化,它与目前的天文观测符合得较好.     

Clustered star formation as a natural explanation for the Halpha cut-off in disk galaxies

The rate of star formation in a galaxy is often determined by the observation of emission in the Halpha line, which is related to the presence of short-lived massive stars. Disk galaxies show a strong cut-off in Halpha radiation at a certain galactocentric distance, which has led to the conclusion that star formation is suppressed in the outer regions of disk galaxies. This is seemingly in contradiction to recent observations in the ultraviolet which imply that disk galaxies have star formation beyond the Halpha cut-off, and that the star-formation-rate surface density is linearly related to the underlying gas surface density, which is a shallower relationship than that derived from Halpha luminosities. In a galaxy-wide formulation, the clustered nature of star formation has recently led to the insight that the total galactic Halpha luminosity is nonlinearly related to the galaxy-wide star formation rate. Here we show that a local formulation of the concept of clustered star formation naturally leads to a steeper radial decrease in the Halpha surface luminosity than in the star-formation-rate surface density, in quantitative agreement with the observations, and that the observed Halpha cut-off arises naturally.     

青藏高原盆地系统演化与高原形成时间

青藏高原在以时间为坐标的隆升过程中,高原的范围、高度都是呈阶段性递增的.随着青藏高原的构造隆升,在高原的内部和外围发育了众多的沉积盆地,在这些沉积盆地中详细地记录了青藏高原的隆升过程.高原北部盆地的演化显示出向北递进增长的特征,以南北挤压为动力背景的北部前陆盆地演化代表了盆地对高原周缘造山带的响应关系:金沙江缝合带、昆仑山、祁连山的新生代逆冲抬升的时间分别为53 Ma、46 Ma和29.5 Ma.对高原南北盆地-造山带的构造演化对比发现:祁连山和高喜马拉雅的逆冲时间相同,说明青藏高原在渐新世基本定型.     

1786年磨西地震触发的摩岗岭滑坡演化过程与成因机理

研究1786年磨西地震触发的摩岗岭滑坡特征及形成演化过程.采用资料收集、地面调查、三维实体模型、高精度遥感影像、理论分析、数值模拟等技术方法,对摩岗岭滑坡的形成进行全过程演化分析.摩岗岭地震滑坡演化过程分为6个阶段:河谷高边坡形成阶段以及斜坡浅表部岩体卸荷拉裂阶段、卸荷拉裂隙扩展阶段、潜在滑动面形成阶段、震动拉裂和高速启动阶段、抛射撞击溃散阶段、滑体堵江及溃决阶段.其成因机理为卸荷震动拉裂-剪断抛射堆积.     

Suppression of star formation in early-type galaxies by feedback from supermassive black holes

Detailed high-resolution observations of the innermost regions of nearby galaxies have revealed the presence of supermassive black holes. These black holes may interact with their host galaxies by means of 'feedback' in the form of energy and material jets; this feedback affects the evolution of the host and gives rise to observed relations between the black hole and the host. Here we report observations of the ultraviolet emissions of massive early-type galaxies. We derive an empirical relation for a critical black-hole mass (as a function of velocity dispersion) above which the outflows from these black holes suppress star formation in their hosts by heating and expelling all available cold gas. Supermassive black holes are negligible in mass compared to their hosts but nevertheless seem to play a critical role in the star formation history of galaxies.     

Rapid collisional evolution of comets during the formation of the Oort cloud

The Oort cloud of comets was formed by the ejection of icy planetesimals from the region of giant planets--Jupiter, Saturn, Uranus and Neptune--during their formation. Dynamical simulations have previously shown that comets reach the Oort cloud only after being perturbed into eccentric orbits that result in close encounters with the giant planets, which then eject them to distant orbits about 10(4) to 10(5) AU from the Sun (1 AU is the average Earth-Sun distance). All of the Oort cloud models constructed until now simulate its formation using only gravitational effects; these include the influence of the Sun, the planets and external perturbers such as passing stars and Galactic tides. Here we show that physical collisions between comets and small debris play a fundamental and hitherto unexplored role throughout most of the ejection process. For standard models of the protosolar nebula (starting with a minimum-mass nebula) we find that collisional evolution of comets is so severe that their erosional lifetimes are much shorter than the timescale for dynamical ejection. It therefore appears that collisions will prevent most comets escaping from most locations in the region of the giant planets until the disk mass there declines sufficiently that the dynamical ejection timescale is shorter than the collisional lifetime. One consequence is that the total mass of comets in the Oort cloud may be less than currently believed.     

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.     

莺歌海盆地压力封存箱的形成、演化及与成藏关系

根据莺歌海盆地钻井资料、压力测试资料等,开展盆地超压特征的分析,结合构造演化及沉积过程,对盆地压力封存箱进行划分,并分析其形成及演化过程,探讨压力封存箱的形成、演化与成藏的关系。研究表明盆地存在3个主要的压力封存箱,压力封存箱经历的3期主要的演化阶段与盆地经历的3期主要构造活动相对应,压力封存箱的形成和演化是动态的。在3个构造期因泥底辟活动造成的箱体破裂,箱内流体向外运聚,该时期是油气的重要运聚时期,也是油气的主要成藏期。从压力封存箱的演化历史看,盆地中油气属于箱外的降温、降压过程中的成藏,这些泥底辟区及周围的斜坡地区应为油气勘探的重要目标区。非泥底辟带,构造相对稳定,超压封存箱演化也平稳,油气运聚规模不大。     

Changing role of even-skipped during the evolution of insect pattern formation.

The development of Drosophila is typical of the so-called long germband mode of insect development, in which the pattern of segments is established by the end of the blastoderm stage. Short germband insects, such as the grasshopper Schistocerca americana, by contrast, generate all or most of their metameric pattern after the blastoderm stage by the sequential addition of segments during caudal elongation. This difference is discernible at the molecular level in the pattern of initiation of the segment polarity gene engrailed, and the homeotic gene abdominal-A (ref. 5). For example, in both types of insects, engrailed is expressed by the highly conserved germband stage in a pattern of regularly spaced stripes, one stripe per segment. In Drosophila, the complete pattern is visible by the end of the blastoderm stage, although engrailed appears initially in alternate segments in a pair-rule pattern that reflects its known control by pair-rule genes such as even-skipped. In contrast, in the grasshopper, the engrailed stripes appear one at a time after the blastoderm stage as the embryo elongates. To address the molecular basis for this difference, we have cloned the grasshopper homologue of the Drosophila pair-rule gene even-skipped and show that it does not serve a pair-rule function in early development, although it does have a similar function in both insects during neurogenesis later in development.