Morse理论支持下的建筑物点云特征提取

针对传统特征提取算法的结果存在交叉紊乱、不连续、缺少拓扑关系等问题,本文提出了基于Morse理论的建筑物点云特征提取算法。首先定义三维表面模型上顶点的Morse函数指标;然后采用邻点比较法自动提取特征点;最后针对Morse-Smale复形的对偶性在建筑物拓扑特征中已无实际意义的问题,提出了单复形拓扑模型的提取与简化算法。试验结果表明,该算法能够获得清晰、连续、完整的建筑物特征线,实现对建筑物模型表面的完全分割;简化算法在保证建筑物特征线拓扑一致性的前提下,可以获取不同层次的建筑物拓扑特征,为建筑物模型的重建与可视化提供了保障。     

Influence of molecular outflows from young stellar objects on molecular clouds

In this paper it is investigated whether molecular outflows can support the turbulence in molecular clouds against decay. In the momentum-driven regime of molecular flows the time scale of the replenishment of the fluctuations is longer than the dissipation time scale of pure hydrodynamical supersonic turbulence.     

Properties of the process of massive star formation

The dynamics of protostellar envelopes around forming massive stars is analysed and the main stages of the process of massive star formation are identified. It is shown that massive stars can be formed in the outer layers of giant molecular cloud cores. Special conditions are necessary for the formation of massive stars.     

A voxel-based fine-scale 3D landscape pattern analysis using laser scanner point clouds

The landscape pattern metrics can quantitatively describe the characteristics of landscape pattern and are widely used in various fields of landscape ecology. Due to the lack of vertical information, 2D landscape metrics cannot delineate the vertical characteristics of landscape pattern. Based on the point clouds, a high-resolution voxel model and several voxel-based 3D landscape metrics were constructed in this study and 3D metrics calculation results were compared with that of 2D metrics. The results showed that certain quantifying difference exists between 2D and 3D landscape metrics. For landscapes with different components and spatial configurations, significant difference was disclosed between 2D and 3D landscape metrics. 3D metrics can better reflect the real spatial structure characteristics of the landscape than 2D metrics.     

Nitrosyl and Nitryl Chloride Formation in H2SO4/HNO3/H2O/HCl Solutions at 200 K

Infrared spectroscopy has been used to measure the vapor pressure of chlorine containing species generated from H2SO4/HNO3/H2O/HCl solutions at 200 K. The vapor pressure was observed to be a function of solution composition. Two solution compositions were investigated. One solution remained a liquid whereas the second solution was a mixed liquid and solid phase (an ice slurry). The liquid solution had a composition of 64.6 wt.% H2SO4/4.8 wt.% HNO3/30.1 wt.% H2O/0.5 wt.% HCl and produced only vapor phase HCl. The ice slurry solution had a composition of 76.6 wt.% H2SO4/3.0 wt.% HNO3/20.1 wt.% H2O/0.3 wt.% HCl and produced HCl, ClNO, and ClNO2 vapor phase components. The sulfuric acid, nitric acid, and water content of these solutions are representative of those present in polar stratospheric clouds (PSCs), however the HCl concentrations are much higher than present within these clouds. The partitioning of chlorine between vapor phase HCl (50%) and ClNO/ClNO2 (50%) for the ice slurry solution suggests a possible mechanism of halogen activation within PSCs. A reaction mechanism to model the observed chemistry is proposed.     

Solar Wind Streams And Intense Geomagnetic Storms Observed During 1986–1991

We have analyze the set of 70 intense geomagnetic storms associatedwith D_st decrease of more than 100 nT, observed duringthe period (1986–1991). We have compile these selected intensegeomagnetic storm events and find out their association with twotypes of solar wind streams and different interplanetary parameters.We concluded that the maximum numbers of intense geomagneticstorms are associated with transient disturbances in solar wind streams,which causes strong interplanetary shocks in interplanetary medium.The association of supersonic shocks and magnetic clouds with intensegeomagnetic storms have also been discussed.     

Mn i hyperfine structure in the near-infrared

Hyperfine interaction constants and hyperfine components of Mn  i lines in the near-infrared J and H bands were obtained by fitting the solar spectrum. I identified the 17744-Å solar absorption line as resulting from Mn  i , and I discarded the identifications of the 13281.65-Å and 16929.85-Å solar features as a result of Fe  i and Mn  i , respectively.     

Supernova remnants and the spiral structure of the Galaxy

A set of unit clouds of 10⁴ M randomly distributed between 3 and 7 kpc radii, move under the general gravitation of the galactic disk and their mutual gravitation. When the clouds collide they form loose aggregates or giant molecular clouds (GMC). Star formation rate is assumed to be proportional to the mass of the GMC. The more massive stars formed soon turn into supernovae, which in turn break up the GMC back into the unit clouds. After some 350 Myr a steady state is reached, in which the GMCs have a mass spectrum of gradient −1.6, and has the mass-radius relation M ∞ R², both in agreement with the observations. From our simulation we find there should be 775 ± 12 supernova remnants in our galaxy. The existence of spiral arms does not increase the production rate of supernova remnants, but it does make the GMCs to concentrate around them.     

The Local Interstellar Medium

Summary. Substantial progress in the field of the Local Interstellar Medium has been largely due to recent launches of space missions, mostly in the UV and X–ray domains, but also to ground-based observations, mainly in high resolution spectroscopy. However, a clear gap seems to remain between the wealth of new data and the theoretical understanding. This paper gives an overview of some observational aspects, with no attempt of completeness or doing justice to all the people involved in the field. As progress rarely evolves in straight paths, we can expect that our present picture of the solar system surroundings is not definitive. Received 30 October 1998