Optimal crater landmark selection based on optical navigation performance factors for planetary landing

Planetary craters are natural navigation landmarks that widely exist and are easily observed. Optical navigation based on crater landmarks has become an important autonomous navigation method for planetary landing. Due to the increase in observed crater landmarks and the limitation of onboard computation, the selection of good crater landmarks has gradually become a research hotspot in the field of landmark-based optical navigation. This paper designs a fast crater landmark selection method, which not only considers the configuration observability of crater subsets but also focuses on the influence on navigation performance arising from the measurement uncertainty and the matching confidence of craters, which is different from other landmark selection methods. The factor of measurement uncertainty, which is anisotropic, correlated and nonidentically distributed, is quantified and integrated into selection based on crater pairing detection and localization error evaluation. In addition, the concept of the crater matching confidence factor is introduced, which reflects the possibility of 2D projection measurements corresponding to 3D positions. Combined with the configuration observability factor, the crater landmark selection indicator is formed. Finally, the effectiveness of the proposed method is verified by Monte Carlo simulations.     

Landmark Navigation Rule, a New Navigation Device

Two new methods of landmark navigation were recently presented. The landmarks are assumed to be within sight of the navigator but with unknown positions. Both methods require computations which are time consuming when a computer is not available. This correspondence presents the concept of a new navigation device called ?landmark navigation rule? which eliminates all the computation effort required in both new methods. The device is simple in construction, lightweight, and consumes no power.     

基于路标观测角的星际着陆器自主位姿确定技术

针对利用导航路标进行六自由度状态估计这一非线性、模糊性问题,对星际着陆器自主位姿确定技术进行了研究。为了减小算法的复杂性,提高求解精度,基于欧式变换下角度不变性,提出以导航路标观测视线之间所形成的夹角作为观测量,对像素观测方程中位置、姿态状态进行解耦求解。通过对观测矩阵的讨论,分析了导航路标空间分布对位姿确定精度的影响,给出了导航路标选取的最优观测方案。最后利用蒙特卡罗仿真对所提导航算法进行了验证,并对影响导航精度的各相关因素进行了分析。     

Joint probabilistic data association for autonomous navigation

A new autonomous navigation scheme based on the joint probabilistic data association (JPDA) approach that processes landmark detections in the field of view (FOV) of an on-board sensor is developed. These detections-some true, some false-are associated to a set of stored landmarks and used to update the state of the vehicle. The results obtained from Monte Carlo simulations prove the ability of this navigation filter to perform in very high false alarm environments. In the different environmental conditions tested in the simulations, the performance of the JPDA navigation filter (JPDANF) is very close to that of the filter based on perfect data association. The very efficient cluster decomposition algorithm presented for the purpose of the navigation problem can also be used in many multitarget tracking applications     

基于特征点的颅面复原技术

介绍了用人工神经网络算法确定待复原颅面的软组织厚度及颅面特征点的方法。在计算机辅助颅面复原过程中,通常只能根据颅骨上少数特征点及其所在部位的法向软组织厚度的统计值进行运算。由于现有统计值指标涵盖的年龄较宽泛,导致复原结果缺乏个性。在测定待复原颅骨骨龄的基础上,通过神经网络训练,确定软组织厚度随年龄的变化规律,较精确地计算出与拟复原对象的骨龄相适应的特征点软组织厚度值,并用最小二乘法及曲面法线原理建立数学模型,计算出颅面特征点。最后用基于Delaunay三角剖分的wavelet插值法复原出面貌雏形。     

多源信息融合卫星组合导航系统的可观度分析

针对基于GNSS卫星、地标矢量和星光矢量的多源信息融合的高轨卫星组合导航系统,分别利用系统可观度分析方法和状态可观度分析方法对其进行分析。仿真结果表明:在GNSS导航卫星不可见时,地标矢量和星光矢量可以有效地提供测量信息,并保证滤波器的稳定。可观度分析结果表明:系统可观度主要受GNSS导航星的可见星数目影响较大,地标矢量和星光矢量的引入有助于提高可观度;基于状态的可观度可以大致反映出滤波器每个状态的误差大小。     

Star-configuration searching for satellite attitude computation

A star pattern recognition algorithm is described which recovers attitude information by processing data obtained from a modular star sensor (MOSS) mounted on a spacecraft information is obtained by matching the stars detected by the MOSS with those inside a stellar catalogue. The system performance has been evaluated both from the point of view of computation time and error probability. The effect of errors in the MOSS measurements and multiple matches cases are also discussed     

The extremely X-ray bright Wolf-Rayet star HD193793

The Einstein Observatory showed that Wolf-Rayet stars have a much larger range in the ratio of X-ray to bolometric luminosity than normal early-type stars. EXOSAT measurements of HD193T93 (WCT+abs) show it to be extremely X-ray bright. This result is probably not connected with the infra-red and radio outburst that the star underwent in 1977. Other Einstein X-ray sources which are probably identified with Wolf-Rayet stars are newly reported.     

Accuracy of Star Occultation Measurements for Satellite Navigation

To determine the orbital parameters of a satellite using star occultations, it is necessary to measure the intensity of stars as they occult. The accuracy of the intensity measurements is reduced by interfering sources of light and internal noise, and is expressed in terms of the magnitude of various sources of interference. Subsequently, a specific system is analyzed in detail. Moonlit cloud tops introduce the largest systematic error. Photon noise from the star radiation, airglow, and moonlit cloud tops are the largest sources of random errors.     

Mixing in Stars and the Evolution of the 3He Abundance

We first recall the observational and theoretical facts that constitute the so-called 3He problem. We then review the chemical anomalies that could be related to the destruction of 3He in red giants stars. We show how a simple consistent mechanism can lead to the destruction of 3He in low mass stars and simultaneously account for the low 12C/13C ratios and low lithium abundances observed in giant stars of different populations. This process should both naturally account for the recent measurements of 3He/H in galactic HII regions and allow for high values of 3He observed in some planetary nebulae. We propose a simple statistical estimation of the fraction of stars that may be affected by this process.     

Space Interferometry Mission instrument model and astrometric performance validation

The Space Interferometry Mission (SIM), performed very accurate astrometric measurements to measure the positions of stars using a 10 m baseline optical interferometer. The lack of signal from the science targets precludes using the star as a feedback signal to control the science interferometer delay line. In order to solve this problem SIM uses pathlength feed forward (PFF) control of the science interferometer. In the case of controlling the science interferometer optical path, the information to position the science delay line comes from a combination of internal metrology, external metrology, and guide interferometer measurements. The accuracy of the internal and external metrology measurements and the guide interferometer measurements are important for the quality of the feed forward signal and also for the ultimate astrometric performance of the instrument. An instrument model of SIM has been built to evaluate optical performance and to emulate various observational scenarios. The effect of averaging methods to reduce metrology cyclic error and the viability of on-orbit calibration maneuvers are studied. The model consists of a real-time dynamics formulation of the spacecraft and a real-time attitude control system. Simulation results investigate the sensitivity of the feed forward signal to the various error sources and time-varying terms.     

MEMS惯测技术在管道测绘系统中的应用

针对小口径管道的测绘问题,提出了一种MEMS惯测装置在小管道测绘系统中应用的方法,直接利用地标点信息为MEMS惯测装置装订初始方位,采用因子图理论对惯性/里程计组合导航信息进行处理,通过后续处理对装订误差进行修正,解决了MEMS惯测装置无法完成初始对准的问题。给出了惯性/里程计组合导航的因子图以及和积算法递推公式,并通过牵引试验对所提方法进行了验证。试验结果表明,提出的应用方法能够有效解决小口径管道的测绘问题,在100m间隔的路标点条件下,单边定位精度能够达到5cm。     

Magnetic Fields in Massive Stars, Their Winds, and Their Nebulae

Massive stars are crucial building blocks of galaxies and the universe, as production sites of heavy elements and as stirring agents and energy providers through stellar winds and supernovae. The field of magnetic massive stars has seen tremendous progress in recent years. Different perspectives—ranging from direct field measurements over dynamo theory and stellar evolution to colliding winds and the stellar environment—fruitfully combine into a most interesting and still evolving overall picture, which we attempt to review here. Zeeman signatures leave no doubt that at least some O- and early B-type stars have a surface magnetic field. Indirect evidence, especially non-thermal radio emission from colliding winds, suggests many more. The emerging picture for massive stars shows similarities with results from intermediate mass stars, for which much more data are available. Observations are often compatible with a dipole or low order multi-pole field of about 1 kG (O-stars) or 300 G to 30?kG (Ap/Bp stars). Weak and unordered fields have been detected in the O-star ζ Ori A and in Vega, the first normal A-type star with a magnetic field. Theory offers essentially two explanations for the origin of the observed surface fields: fossil fields, particularly for strong and ordered fields, or different dynamo mechanisms, preferentially for less ordered fields. Numerical simulations yield the first concrete stable (fossil) field configuration, but give contradictory results as to whether dynamo action in the radiative envelope of massive main sequence stars is possible. Internal magnetic fields, which may not even show up at the stellar surface, affect stellar evolution as they lead to a more uniform rotation, with more slowly rotating cores and faster surface rotation. Surface metallicities may become enhanced, thus affecting the mass-loss rates.     

Solar and stellar seismology

This article reviews solar and stellar seismology, with emphasis on the enormous progress which has been made recently in the observation and understanding of solar p-modes. Precision measurements of p-mode frequencies and frequency splittings allow a greater understanding of the structure of the solar interior, while p-mode amplitudes and linewidths shed light on the mode excitation mechanism, which is probably stochastic excitation by turbulent convection. The prospects for making similar measurements on other stars are also discussed.     

亮星辅助下基于坐标转换的快速星图识别方法

数字天顶仪作为一种地面使用的星敏感器，主要用于高精度定位。为提高仪器的工作效率需要对星图识别的快速性进行研究。通过对恒星像点理论坐标与图像坐标的分析，构建坐标转换模型。依据星表中恒星的分布及星等筛选出视场范围内的亮星，并构建导航星表。结合导航星表完成3颗亮星的准确识别，在识别亮星的基础上解算坐标转换模型的参数。通过构建的坐标转换模型对视场范围内的恒星进行坐标转换，将转换后的星点坐标与提取的星点图像坐标进行匹配完成星图的识别，这样能够提高星图识别的快速性。实验数据表明：在保证识别星点数量的基础上，采用亮星辅助下基于坐标转换的星图识别方法使时间缩短为改进三角形星图识别算法的五分之一。     

基于地标信息的车载惯导姿态修正技术

惯导与速率计构成的组合系统是机动作战车辆较常使用的自主定位定向系统,其惯导姿态精度将直接影响组合定位精度。文章利用车辆运动途中的地标信息,讨论了车载惯导姿态误差估计与修正技术,通过仿真分析了地标位置与车辆零速信息在惯导姿态修正过程中的作用。结果表明：利用地标信息是进行车载惯导姿态修正较为实用的途径,在此基础上可以有效提高车载惯导／速率计组合定位系统的精度。     

The Be stars

Classical Be stars are defined and their relationship to normal B-type stars stated. Spectral classification of the underlying stars suggests that, on the average, Be stars are located 0.5–1.0 magnitude above the main sequence. Struve's rotational model for Be stars, and several tests which support the model, are reviewed. The best evidence at this time suggests that Be stars may not rotate with the critical velocity at which centrifugal force just balances the equatorial gravitational force, but a number of mechanisms for getting material out into the shell have been proposed and are discussed.The physical characteristics of Be shells were first derived from optical observations of shell stars, supplemented more recently by ultraviolet, infrared, radio, and polarization measurements. These data suggest that Be shells are probably lenticular with radii 3 to 20 times the radius of the underlying star, excitation temperatures lower than those of the reversing layers, and electron densities in the range 10¹⁰-10¹³ cm^-3.Variability of Be stars, from spectroscopic, photometric, and polarimetric observations, seems well established over time scales of years and months, but the evidence for night-to-night and hourly changes is somewhat conflicting. Of special interest are recent X-ray observations of several Be stars.Models for the envelopes of Be stars are reviewed, including state-state stellar wind models, time-dependent stellar wind models, the elliptical ring model, disk models, and binary models. Finally, the evolutionary status of Be stars is discussed, and some recommendations for future work made.     

Astrometric search for unseen stellar and sub-stellar companions to nearby stars and the possibility of their detection

Unseen companions to nearby stars are found astrometrically through perturbations in the proper motion from photographs taken with long-focus telescopes. The number of known unseen astrometric companions to nearby stars with photocentric orbits has grown by thirty percent in the last few years. Individual cases are discussed and optimum epochs given for resolution of the components. Orbital analysis of the photocentric positions on the photographic plates provides all information for accurate mass determination of the components except for m and angular separation, , of the two components which must come from another technique. There are potentially thirty low luminosity stars including some likely sub-stellar objects whose masses could be instantly found with the observations of these additional two parameters.A list of the stars known within five parsecs as of 1978 July is given and the status of unseen companions to these stars is discussed on the basis of long interval astrometric coverage.     

Towards a Unified View of Inhomogeneous Stellar Winds in Isolated Supergiant Stars and Supergiant High Mass X-Ray Binaries

Massive stars, at least \(\sim10\) times more massive than the Sun, have two key properties that make them the main drivers of evolution of star clusters, galaxies, and the Universe as a whole. On the one hand, the outer layers of massive stars are so hot that they produce most of the ionizing ultraviolet radiation of galaxies; in fact, the first massive stars helped to re-ionize the Universe after its Dark Ages. Another important property of massive stars are the strong stellar winds and outflows they produce. This mass loss, and finally the explosion of a massive star as a supernova or a gamma-ray burst, provide a significant input of mechanical and radiative energy into the interstellar space. These two properties together make massive stars one of the most important cosmic engines: they trigger the star formation and enrich the interstellar medium with heavy elements, that ultimately leads to formation of Earth-like rocky planets and the development of complex life. The study of massive star winds is thus a truly multidisciplinary field and has a wide impact on different areas of astronomy.In recent years observational and theoretical evidences have been growing that these winds are not smooth and homogeneous as previously assumed, but rather populated by dense “clumps”. The presence of these structures dramatically affects the mass loss rates derived from the study of stellar winds. Clump properties in isolated stars are nowadays inferred mostly through indirect methods (i.e., spectroscopic observations of line profiles in various wavelength regimes, and their analysis based on tailored, inhomogeneous wind models). The limited characterization of the clump physical properties (mass, size) obtained so far have led to large uncertainties in the mass loss rates from massive stars. Such uncertainties limit our understanding of the role of massive star winds in galactic and cosmic evolution.Supergiant high mass X-ray binaries (SgXBs) are among the brightest X-ray sources in the sky. A large number of them consist of a neutron star accreting from the wind of a massive companion and producing a powerful X-ray source. The characteristics of the stellar wind together with the complex interactions between the compact object and the donor star determine the observed X-ray output from all these systems. Consequently, the use of SgXBs for studies of massive stars is only possible when the physics of the stellar winds, the compact objects, and accretion mechanisms are combined together and confronted with observations.This detailed review summarises the current knowledge on the theory and observations of winds from massive stars, as well as on observations and accretion processes in wind-fed high mass X-ray binaries. The aim is to combine in the near future all available theoretical diagnostics and observational measurements to achieve a unified picture of massive star winds in isolated objects and in binary systems.     

A reference catalogue and atlas of galactic novae

This catalogue and atlas contains information on 277 objects, mainly classical novae and related objects (recurrent novae, X-ray novae, dwarf novae with long cycle lengths, symbiotic stars and suspected new stars). For most objects, brightness ranges, accurate positions, finding charts and selected bibliographies are given.Based in part on observations collected at the European Southern Observatory, La Silla, Chile, the Centro Astronomico Hispano-Aleman Calar Alto, operated by the Max-Planck-Institut für Astronomie, Heidelberg, and on measurements made at the European Southern Observatory, Garching, F.R.G.