Rapid disappearance of a warm, dusty circumstellar disk

Stars form with gaseous and dusty circumstellar envelopes, which rapidly settle into disks that eventually give rise to planetary systems. Understanding the process by which these disks evolve is paramount in developing an accurate theory of planet formation that can account for the variety of planetary systems discovered so far. The formation of Earth-like planets through collisional accumulation of rocky objects within a disk has mainly been explored in theoretical and computational work in which post-collision ejecta evolution typically is ignored, although recent work has considered the fate of such material. Here we report observations of a young, Sun-like star (TYC?8241?2652?1) where infrared flux from post-collisional ejecta has decreased drastically, by a factor of about 30, over a period of less than two years. The star seems to have gone from hosting substantial quantities of dusty ejecta, in a region analogous to where the rocky planets orbit in the Solar System, to retaining at most a meagre amount of cooler dust. Such a phase of rapid ejecta evolution has not been previously predicted or observed, and no currently available physical model satisfactorily explains the observations.     

Discovery of X-rays from the protostellar outflow object HH2

Herbig-Haro (HH) objects have been known for 50 years to be luminous condensations of gas in star-forming regions, but their underlying physical nature is still being elucidated. Previously suggested models encompass newborn stars, stellar winds clashing with nebular material, dense pockets of interstellar gas excited by shocks from outflows, and interstellar 'bullets' (ref. 6). Recent progress has been made with the jet-induced shock model, in which material streams out of young stellar objects and collides with the surrounding interstellar medium. A clear prediction of this model is that the most energetic Herbig-Haro objects will emit X-rays, although they have not hitherto been detected. Here we report the discovery of X-ray emission from one of the brightest and closest Herbig-Haro objects, HH2, at a level consistent with the model predictions. We conclude that this Herbig-Haro object contains shock-heated material located at or near its leading edge with a temperature of about 106 K.     

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.     

A 'dry' condensation origin for circumstellar carbonates

The signature of carbonate minerals has long been suspected in the mid-infrared spectra of various astrophysical environments such as protostars. Abiogenic carbonates are considered as indicators of aqueous mineral alteration in the presence of CO2-rich liquid water. The recent claimed detection of calcite associated with amorphous silicates in two planetary nebulae and protostars devoid of planetary bodies questions the relevance of this indicator; but in the absence of an alternative mode of formation under circumstellar conditions, this detection remains controversial. The main dust component observed in circumstellar envelopes is amorphous silicates, which are thought to have formed by non-equilibrium condensation. Here we report experiments demonstrating that carbonates can be formed with amorphous silicates during the non-equilibrium condensation of a silicate gas in a H2O-CO2-rich vapour. We propose that the observed astrophysical carbonates have condensed in H2O(g)-CO2(g)-rich, high-temperature and high-density regions such as evolved stellar winds, or those induced by grain sputtering upon shocks in protostellar outflows.     

A young massive planet in a star-disk system

There is a general consensus that planets form within disks of dust and gas around newly born stars. Details of their formation process, however, are still a matter of ongoing debate. The timescale of planet formation remains unclear, so the detection of planets around young stars with protoplanetary disks is potentially of great interest. Hitherto, no such planet has been found. Here we report the detection of a planet of mass (9.8+/-3.3)M(Jupiter) around TW Hydrae (TW Hya), a nearby young star with an age of only 8-10 Myr that is surrounded by a well-studied circumstellar disk. It orbits the star with a period of 3.56 days at 0.04 au, inside the inner rim of the disk. This demonstrates that planets can form within 10 Myr, before the disk has been dissipated by stellar winds and radiation.     

物体作圆锥曲线运动的时间计算

在比耐公式的基础上导出了物体在受到与距离平方成反比的有心力作用下的轨道方程.系统阐述了物体作圆锥曲线运动的时间计算问题,并给出了物体作圆、椭圆、抛物线、双曲线运动的时间计算公式.对于双曲线的情况,同时给出了引力和斥力作用下的时间计算公式.     

视频序列中运动目标跟踪新方法

提出了一种跟踪视频图像序列中运动目标的新方法.该方法利用一种基于动态信息窗口的自适应背景更新方法解决背景的复杂性问题,结合一种新的计算颜色模型解决运动阴影问题,从而得到具有精确边缘的特定运动目标.计算了运动目标灰度质心,在坐标系中记录其位置,并采用最小二乘法拟合实现了对运动目标的跟踪.实验结果表明这种方法能有效地跟踪并预测视频序列中的运动目标.     

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.     

A Disk Scheduling Algorithm： SPFF

We put forward an optimal disk schedule with n disk requests and prove its optimality mathematically.Generalizing the idea of an optimal disk schedule, we remove the limit of n requests and, at the same time, consider the dynamically arrival model of disk requests to obtain an algorithm, shortest path first-fit first （SPFF）. This algorithm is based on the shortest path of disk head motion constructed by all the pendent requests. From view of the head moving distance, it has the stronger glohality than SSTF. From view of the head-moving direction, it has the better flexibility than SCAN. Therefore, SPFF keeps the advantage of SCAN and, at the same time, absorbs the strength of SSTF. The algorithm SPFF not only shows the more superiority than other scheduling polices, but also have higher adjustability to meet the computer system＇s different demands.     

用Disk Manager2000管理和维护大容量硬盘

详细介绍了利用 Disk Manager2000对新硬盘进行安装及安装中盘符交错的问题。安装后如何对硬盘进行维护、分区等。其中介绍了重新分区、正确定位光驱盘符、不同盘之间的文件拷贝,以及怎样创建 For Dos 的启动盘。同时介绍了硬盘检测工具 Run SmartedFender 使用方法。     

面向表单的对象模型的研究

在企业软件的开发过程中，现有的各种建模方法均不能有效的与用户进行沟通，所以迫切需要一种能够顺利解决这一问题的建模方法。基于这种要求，提出并实现了面向表单的建模方法。该种建模方法简单明了，能够很好解决与用户的交流问题，同时其能够自动生成底层数据库及最终代码，可以大大的提高软件开发的效率和系统的稳定性、可扩展性、可维护性和安全性。     

利用LINDO求解目标规划

通过引入“优先乘子”概念 ,将目标规划按一定规则转化为线性规划 ,再利用LIN DO求解。从而使得目标规划的求解变得简单易行     

基于模板更新的深层孪生网络跟踪算法

针对跟踪过程中因尺度变化、遮挡及运动模糊等造成的目标定位不准确问题,在SiamFC(fully-convolutional siamese network)的跟踪框架基础上提出了一种具有高置信度模板更新机制的深层孪生网络目标跟踪算法.首先,主干网络采用ResNet-50残差网络进行特征提取,并融合多层特征图进行目标预测;其次,为避免模板频繁更新带来的模板漂移问题,构建了高置信度的模板更新模块.在OTB100数据集上的实验结果表明,相比基准算法,文中算法的跟踪成功率和精确度分别提高了3.4%和2.6%;在多种挑战因素下的对比实验表明,文中算法可以较好地抵抗目标遮挡、尺度变化、运动模糊等多种复杂因素带来的影响,有很好的鲁棒性.     

海量数据下线性混合效应模型的估计算法

基于以往文献提出线性混合效应模型参数的三步估计方法,避免了繁杂的极大似然估计迭代步骤。同时为进一步解决海量数据下计算估计量时存在的存储瓶颈及计算时间过长问题,在海量纵向数据的两种不同数据格式下,分别基于三步估计方法利用分治算法计算模型参数的估计量。数值模拟和实证分析结果表明,本文所提出的三步估计方法和估计量的分治算法可以减轻计算负担,减少占用内存,解决内存不足的问题,并提高计算速度。     

A giant outburst two years before the core-collapse of a massive star

The death of massive stars produces a variety of supernovae, which are linked to the structure of the exploding stars. The detection of several precursor stars of type II supernovae has been reported (see, for example, ref. 3), but we do not yet have direct information on the progenitors of the hydrogen-deficient type Ib and Ic supernovae. Here we report that the peculiar type Ib supernova SN 2006jc is spatially coincident with a bright optical transient that occurred in 2004. Spectroscopic and photometric monitoring of the supernova leads us to suggest that the progenitor was a carbon-oxygen Wolf-Rayet star embedded within a helium-rich circumstellar medium. There are different possible explanations for this pre-explosion transient. It appears similar to the giant outbursts of luminous blue variable stars (LBVs) of 60-100 solar masses, but the progenitor of SN 2006jc was helium- and hydrogen-deficient (unlike LBVs). An LBV-like outburst of a Wolf-Rayet star could be invoked, but this would be the first observational evidence of such a phenomenon. Alternatively, a massive binary system composed of an LBV that erupted in 2004, and a Wolf-Rayet star exploding as SN 2006jc, could explain the observations.     

圆盘反应器成膜性能的实验研究

在直径为0.48m圆盘反应器内研究了物料黏度、液位、圆盘转速等因素对反应器功率、最小成膜转速、持液量以及膜厚的影响规律。结果表明:最小成膜转速随黏度的增加而降低,随液位的降低而升高;持液量随黏度和转速增加而增大,黏度较低时增加的趋势低于黏度较高时;无因次混合时间随着线速度的增加先减小后增加;同时得到了功率准数以及膜厚的关联式。     

一种快速运动目标检测算法

运动目标检测是智能视觉监控系统的重要组成部分,其主要功能是检测监控场景中的运动目标,为高层运动分析提供必要的信息。文章提出一种快速运动目标检测算法,以帧差法和背景减法为基础,快速实现背景提取、背景更新、运动目标检测的功能。实验结果表明,该算法计算量小,检测目标完整,能够满足实时监控系统的要求。     

不规则类圆形团块目标图像识别的新方法

针对类圆形目标图像识别方法的不足,以轧钢厂成捆棒材图像为实例,提出了不规则类圆形团块目标模式识别新方法,设计了边缘检测、中心增强和重心聚合等一系列算法,以实现计算机对类圆形目标图像的自动识别与检测.研究结果表明:以新算法为核心技术的软件能够对直径为12～40 cm的棒材进行计数,点支准确的捆精度达到99%,且每捆计数时问少于3 s.     

大尺度结构物附近小尺度杆件上波浪力的时域分析

为准确计算复合结构中小尺度杆件上的波浪荷载,不仅需考虑入射波浪的作用,还应该考虑大尺度结构物对波浪的绕射以及辐射的影响.本文以波浪对固定圆柱作用产生的绕射场为例,用Morison公式计算绕射场作用下细小杆件的波浪荷载.用高阶边界元法建立波浪对结构物作用的时域计算程序,利用积分方程求解域内水质点由绕射势产生的速度和加速度.结果显示,在一定的波浪条件下,考虑绕射波浪力得到的总力可达到入射波浪力的2倍.因此,在工程中应充分考虑复合结构中由于大尺度结构物存在而产生的绕射和辐射作用于细小杆件的波浪力.