行星际日冕物质抛射中的磁流体波动观测

日冕物质抛射（CME）是最大尺度的太阳活动现象,灾害性空间天气的主要驱动源．行星际日冕物质抛射（ICME）中的等离子体波动性质与ICME的演化密切相关．由于ICME中的平均磁场较大,其中的Alfven低频扰动研究较少．前人的研究只分析了0．3AU和0．68AU处的个别ICME中的Alfven波动．ICME在1AU处的Alfven波观测较少．本文对第23太阳周1995—2006年期间所有引起大磁暴（Dst≤－100nT）的单个ICME事件进行统计分析,结果表明：（1）大约30％的ICME中长时间存在Alfven波（超过ICME持续时间的30％）;（2）约一半的ICME的鞘层中存在快磁声波;（3）所有ICME中都存在短时间段的慢磁声波．这些观测结果为研究CME在行星际传播过程时其中的Alfven波演化机制及其动力学演化提供了观测基础．     

Coordinated observations of large scale coronal brightening and H_αsurge

During the post_flare phase of an eruptive two_ribbon flare on February 4, 1995, the Soft X_ray Telescope (SXT) on board Yohkoh observed the rapid brightening of a set of large scale coronal loops (150-200 Mm in length). Simultaneously, coordinated ground_based observations reveal a co_incident H α surge event. To our knowledge, no H α surge event coincident with the large scale coronal brightening observed by Yohkoh has been reported. The possible mechanisms for the concurrent cool plasma ejection and the filling of the hot coronal loops are discussed. It is found that magnetic reconnection between a magnetic arcade and an overlying large scale coronal structure may account for the coincident events. Big amount of magnetic energy was converted into both mechanic energy (about 10 22 J) in the mass ejection and thermal radiation (10 23 J) contained in the large SXR loops.     

煤层气分子成泡的微观过程研究

运用化学理论对煤层气分子(主要成分为甲烷)在地层水的溶解和成泡过程进行了描述,对成泡过程的受力与做功进行分析,并结合生产实际讨论了温度、生产压差、地层水矿化度、压力降和孔隙介质的大小对甲烷分子成泡规律的影响.研究表明:甲烷分子在水中成泡包括甲烷分子在水中的溶解、局部聚集成核、成泡与气泡的破裂和气泡的生长与稳定4个过程.上覆压力越小,开发的压力降越大越有利于甲烷分子脱附后形成稳定的气泡;在煤层气开发初期,甲烷以扩散方式运移,低温和低矿化度有利于气泡的生成.     

Spherical episodic ejection of material from a young star

The exact processes by which interstellar matter condenses to form young stars are of great interest, in part because they bear on the formation of planets like our own from the material that fails to become part of the star. Theoretical models suggest that ejection of gas during early phases of stellar evolution is a key mechanism for removing excess angular momentum, thereby allowing material to drift inwards towards the star through an accretion disk. Such ejections also limit the mass that can be accumulated by the stellar core. To date, these ejections have been observed to be bipolar and highly collimated, in agreement with theory. Here we report observations at very high angular resolution of the proper motions of an arc of water-vapour masers near a very young, massive star in Cepheus. We find that the arc of masers can be fitted to a circle with an accuracy of one part in a thousand, and that the structure is expanding. Only a sphere will always produce a circle in projection, so our observations strongly suggest that the perfectly spherical ejection of material from this star took place about 33 years earlier. The spherical symmetry of the ejecta and its episodic nature are very surprising in the light of present theories.     

Noggin and retinoic acid transform the identity of avian facial prominences.

The signals that determine body part identity in vertebrate embryos are largely unknown, with some exceptions such as those for teeth and digits. The vertebrate face is derived from small buds of tissue, facial prominences, that surround the embryonic oral cavity. In chicken embryos, the skeleton of the upper beak is derived from the frontonasal mass and maxillary prominences. Here we show that bone morphogenetic proteins (Bmps) and the vitamin A derivative, retinoic acid (RA), are used to specify the identity of the frontonasal mass and maxillary prominences. Implanting two beads adjacent to the stage-15 presumptive maxillary field, one soaked in the Bmp antagonist Noggin and one soaked in RA, induces a duplicate set of frontonasal mass skeletal elements in place of maxillary bones. We also show that the duplicated beak is due to transformation of the maxillary prominence into a second frontonasal mass and not due to ectopic migration of cells or splitting of the normal frontonasal mass. Thus the levels of Bmp and RA determine whether specific regions of the face form maxillary or frontonasal mass derivatives.     

2003年10月与11月两次主要日冕物质抛射事件的空间天气效应比较

研究了分别发生在2003年10月28日和2003年11月18日的两次相似的强烈日冕物质抛射(CME)事件.通过比较这两次CME事件以及它们的行星际响应,分析了其伴随的两种主要空间天气效应:太阳高能粒子事件和地磁暴.这两次CME事件均伴随有一个强耀斑和一次暗条爆发,并且之前都有一个较弱的CME从同一源区产生.第一个CME事件引起了一次极大的太阳高能粒子事件,而第二个则没有引起明显的太阳高能粒子事件.这两次CME事件均引起了大的地磁暴,且第二个CME所引起的地磁暴比第一个CME所引起的地磁暴更强.通过比较分析这两次CME事件,以及与之相关的活动现象和对应的行星际磁云(MC),讨论了这两次CME引起不同空间天气效应的原因:形成不同强度的太阳高能粒子事件在于CME爆发过程中的能量释放率在这两次事件中显著不同,而地磁暴强度的差异则是由行星际MC轴的方向以及MC经过地球时的相对位置不同造成的.     

固定汽泡周围的温度场分布

为估计M arangon i对流和自然对流对汽泡周围流场的影响,对加热面朝上和朝下的不同大小和过冷度的汽泡周围温度场进行了测量。通过比较测量所得温度场和带N av ier-S tokes方程的数值模拟结果可知,在完全没有浮升力时,M arangon i流会使得流场呈现一个向下的类似于射流的形状,但有了浮升力,向下的流动会立刻转向上,在加热表面附近形成涡流。即使加热面朝下,这种浮升力引起的自然对流依然影响整个流场,以至于这个系统不能很好地表现在微重力条件下的汽泡周围的流场。     

X-ray clusters of galaxies as tracers of structure in the Universe

Clusters of galaxies are visible tracers of the network of matter in the Universe, marking the high-density regions where filaments of dark matter join together. When observed at X-ray wavelengths these clusters shine like cosmic lighthouses, as a consequence of the hot gas trapped within their gravitational potential wells. The X-ray emission is linked directly to the total mass of a cluster, and so can be used to investigate the mass distribution for a sizeable fraction of the Universe. The picture that has emerged from recent studies is remarkably consistent with the predictions for a low-density Universe dominated by cold dark matter.     

Meteoritic dust from the atmospheric disintegration of a large meteoroid

Much of the mass of most meteoroids entering the Earth's atmosphere is consumed in the process of ablation. Larger meteoroids (> 10 cm), which in some cases reach the ground as meteorites, typically have survival fractions near 1-25 per cent of their initial mass. The fate of the remaining ablated material is unclear, but theory suggests that much of it should recondense through coagulation as nanometre-sized particles. No direct measurements of such meteoric 'smoke' have hitherto been made. Here we report the disintegration of one of the largest meteoroids to have entered the Earth's atmosphere during the past decade, and show that the dominant contribution to the mass of the residual atmospheric aerosol was in the form of micrometre-sized particles. This result is contrary to the usual view that most of the material in large meteoroids is efficiently converted to particles of much smaller size through ablation. Assuming that our observations are of a typical event, we suggest that large meteoroids provide the dominant source of micrometre-sized meteoritic dust at the Earth's surface over long timescales.     

A review of recent studies on coronal dynamics: Streamers, coronal mass ejections, and their interactions

In this article I present a review of recent studies on coronal dynamics, including research progresses on the physics of coronal streamers that are the largest structure in the corona, physics of coronal mass ejections (CMEs) that may cause a global disturbance to the corona, as well as physics of CME-streamer interactions. The following topics will be discussed in depth: (1) acceleration of the slow wind flowing around the streamer considering the effect of magnetic flux tube curvature; (2) physical mechanism accounting for persistent releases of streamer blobs and diagnostic results on the temporal variability of the slow wind speed with such events; (3) force balance analysis and energy release mechanism of CMEs with a flux rope magnetohydrodynamic model; (4) statistical studies on magnetic islands along the coronal-ray structure behind a CME and the first observation of magnetic island coalescence with associated electron acceleration; and (5) white light and radio manifestations of CME-streamer interactions. These studies shed new light on the physics of coronal streamers, the acceleration of the slow wind, the physics of solar eruptions, the physics of magnetic reconnection and associated electron acceleration, the large-scale coronal wave phenomenon, as well as the physics accounting for CME shock-induced type II radio bursts.     

7075铝合金锻件表面气泡分析

铝合金制品表面缺陷是造成制品报废的主要原因之一。采用光学显微镜（optical microscopy,OM）、扫描电子显微镜(scanning electron microscope, SEM)、能谱仪（energy disperse spectroscopy,EDS）等检测设备,对7075铝合金挤压棒材经锻造热处理形成的气泡缺陷进行研究。研究结果表明：7075铝合金锻件表面气泡是表皮分层气泡,而非表面夹杂气泡;由于基材加工过程中存在空腔、分层或裂缝,热处理后的冷却过程中空腔压力增大,导致结合薄弱的晶界形成破坏性裂纹,最终以气泡形式表现出来;轧制、挤压、热处理过程中应注意工艺参数的合理性,适当控制生产工艺与热处理温度,有利于减少或消除表皮分层气泡。     

基于单泡溃灭能量转化理论的空化实验研究进展

随着水力机械向大型化、高速化发展,船舶螺旋桨、水轮机及增压泵等相关设备设施的空化现象越来越严重,国内外学者对空泡溃灭能量转化进行了大量的实验研究,为降低空化侵蚀的损伤提供理论指导。本文首先概述了高速摄像技术、接触式水听器测量技术、非接触式光偏转法技术等方法在空泡相关实验研究中的应用,并分别讨论了其可实现的测试功能。其次综述了四类空泡能量耗散形式：一重建空泡能量;二不对称溃灭微射流能量;三压力波能量;四以热能和光能的形式耗散。最后总结了目前研究尚存在的不足,并在单泡溃灭能量转化理论模型、多空泡和复杂壁面场景下能量转化实验研究及深入探究材料空化侵蚀能量转化机制三个方面进行了展望,以期推动空泡溃灭能量转化理论及技术与方法的进展。     

Condensation-Induced Steam Bubble Collapse in a Pipeline

IntroductionInfluidflowpipelinesenormousdamagemaybecausedbywaterhammerduetocavitycollapsecausedbysuddencontactionoftheliquidcolumnorbysteambubblecollapsewhenthesteambubblecontactscoolwaterandcondenses.Steambubblecollapseandthesubsequentwaterhammerreportedinanuclearpowerplantdestroyedthefeedwaterpipingintheplant.50mlongpipesweredeformedandpulledfromtheiranchorsbytheaccident.Thewaterhammerforcewasestimatedtobe0.7MN.Thiskindofaccidenthasalsooccurredinothernuclearpowerplantswhereoperatorsreported…     

加压下气泡在液体中的行为

通过物理实验,研究了容器压力、喷嘴孔径和吹气流量对气泡形貌、直径和上升速度的影响.结果表明,在常压下,大孔径喷嘴形成的气泡呈扁平状,其上升过程形状变化大;而在大的压力下,其形成的气泡呈椭球状,上升过程形状稳定.常压下吹气流量对大孔径产生的气泡等效直径影响较小,在小的喷嘴孔径下,吹气流量能明显增加气泡的等效直径,而压力对改变小气泡等效直径的作用不明显.在低的吹气流量和高的容器压力下,较大孔径的喷嘴也能产生较小的气泡.在大孔径下吹气,压力在0.1~0.2 MPa时,不同的吹气流量下的气泡等效直径相差小;而当压力增加到0.3~0.4 MPa时,不同吹气流量的气泡等效直径差别变大.压力增加,气泡的上升速度降低,且在大的吹气流量下,压力对气泡运动速度的影响更为明显;大孔径喷嘴产生的气泡一般有更大的上升速度.在常压下,气体流量对气泡上升速度起着决定性影响,而加压到0.4 MPa,喷嘴孔径对气泡上升速度起着决定性作用.     

Charon's size and an upper limit on its atmosphere from a stellar occultation

Pluto and its satellite, Charon (discovered in 1978; ref. 1), appear to form a double planet, rather than a hierarchical planet/satellite couple. Charon is about half Pluto's size and about one-eighth its mass. The precise radii of Pluto and Charon have remained uncertain, leading to large uncertainties on their densities. Although stellar occultations by Charon are in principle a powerful way of measuring its size, they are rare, as the satellite subtends less than 0.3 microradians (0.06 arcsec) on the sky. One occultation (in 1980) yielded a lower limit of 600 km for the satellite's radius, which was later refined to 601.5 km (ref. 4). Here we report observations from a multi-station stellar occultation by Charon, which we use to derive a radius, R(C) = 603.6 +/- 1.4 km (1sigma), and a density of rho = 1.71 +/- 0.08 g cm(-3). This occultation also provides upper limits of 110 and 15 (3sigma) nanobar for an atmosphere around Charon, assuming respectively a pure nitrogen or pure methane atmosphere.     

CO气氛下CaO对铁晶须生长影响的原位观察和机理研究

利用光学体视显微镜和高温热台对CO气体还原Fe2O3过程进行原位观察,并结合扫描电镜、能谱和红外光谱分析,研究掺入CaO对还原过程中铁晶须生成和生长机理的影响.实验结果表明:铁晶须是在实现FeO→Fe转变时形成和不断生长的;CaO对氧化铁的还原有抑制作用,当掺入CaO质量分数≥8%时,没有铁晶须生成和生长.因此,可以通过控制CaO掺入量的方式抑制铁晶须的生成和生长,进而减少矿粉颗粒团聚的发生.     

A star in a 15.2-year orbit around the supermassive black hole at the centre of the Milky Way

Many galaxies are thought to have supermassive black holes at their centres-more than a million times the mass of the Sun. Measurements of stellar velocities and the discovery of variable X-ray emission have provided strong evidence in favour of such a black hole at the centre of the Milky Way, but have hitherto been unable to rule out conclusively the presence of alternative concentrations of mass. Here we report ten years of high-resolution astrometric imaging that allows us to trace two-thirds of the orbit of the star currently closest to the compact radio source (and massive black-hole candidate) Sagittarius A*. The observations, which include both pericentre and apocentre passages, show that the star is on a bound, highly elliptical keplerian orbit around Sgr A*, with an orbital period of 15.2 years and a pericentre distance of only 17 light hours. The orbit with the best fit to the observations requires a central point mass of (3.7 +/- 1.5) x 10(6) solar masses (M(*)). The data no longer allow for a central mass composed of a dense cluster of dark stellar objects or a ball of massive, degenerate fermions.     

Cavity solitons as pixels in semiconductor microcavities

Cavity solitons are localized intensity peaks that can form in a homogeneous background of radiation. They are generated by shining laser pulses into optical cavities that contain a nonlinear medium driven by a coherent field (holding beam). The ability to switch cavity solitons on and off and to control their location and motion by applying laser pulses makes them interesting as potential 'pixels' for reconfigurable arrays or all-optical processing units. Theoretical work on cavity solitons has stimulated a variety of experiments in macroscopic cavities and in systems with optical feedback. But for practical devices, it is desirable to generate cavity solitons in semiconductor structures, which would allow fast response and miniaturization. The existence of cavity solitons in semiconductor microcavities has been predicted theoretically, and precursors of cavity solitons have been observed, but clear experimental realization has been hindered by boundary-dependence of the resulting optical patterns-cavity solitons should be self-confined. Here we demonstrate the generation of cavity solitons in vertical cavity semiconductor microresonators that are electrically pumped above transparency but slightly below lasing threshold. We show that the generated optical spots can be written, erased and manipulated as objects independent of each other and of the boundary. Numerical simulations allow for a clearer interpretation of experimental results.     

Vertical extension of the subglacial drainage system into basal crevasses

Water plays a first-order role in basal sliding of glaciers and ice sheets and is often a key constituent of accelerated glacier motion. Subglacial water is known to occupy systems of cavities and conduits at the interface between ice and the underlying bed surface, depending upon the history of water input and the characteristics of the substrate. Full understanding of the extent and configuration of basal water is lacking, however, because direct observation is difficult. This limits our ability to simulate ice dynamics and the subsequent impacts on sea-level rise realistically. Here we show that the subglacial hydrological system can have a large volume of water occupying basal crevasses that extend upward from the bed into the overlying ice. Radar and seismic imaging combined with in situ borehole measurements collected on Bench Glacier, Alaska, reveal numerous water-filled basal crevasses with highly transmissive connections to the bed. Some crevasses extend many tens of metres above the bed and together they hold a volume of water equivalent to at least a decimetre layer covering the bed. Our results demonstrate that the basal hydrologic system can extend high into the overlying ice mass, where basal crevasses increase water-storage capacity and could potentially modulate basal water pressure. Because basal crevasses can form under commonly observed glaciological conditions, our findings have implications for interpreting and modelling subglacial hydrologic processes and related sliding accelerations of glaciers and ice sheets.     

Filamentary structure on the Sun from the magnetic Rayleigh-Taylor instability

Magnetic flux emerges from the solar surface as dark filaments connecting small sunspots with opposite polarities. The regions around the dark filaments are often bright in X-rays and are associated with jets. This implies plasma heating and acceleration, which are important for coronal heating. Previous two-dimensional simulations of such regions showed that magnetic reconnection between the coronal magnetic field and the emerging flux produced X-ray jets and flares, but left unresolved the origin of filamentary structure and the intermittent nature of the heating. Here we report three-dimensional simulations of emerging flux showing that the filamentary structure arises spontaneously from the magnetic Rayleigh-Taylor instability, contrary to the previous view that the dark filaments are isolated bundles of magnetic field that rise from the photosphere carrying the dense gas. As a result of the magnetic Rayleigh-Taylor instability, thin current sheets are formed in the emerging flux, and magnetic reconnection occurs between emerging flux and the pre-existing coronal field in a spatially intermittent way. This explains naturally the intermittent nature of coronal heating and the patchy brightenings in solar flares.