Spartan 201 coronal spectroscopy during the polar passes of ulysses

Spartan 201 is a shuttle deployed spacecraft that is scheduled to perform ultraviolet spectroscopy and white light polarimetry of the extended solar corona during two 40 hour missions to occur in September 1994 and August 1995. The spectroscopy is done with an ultraviolet coronal spectrometer which measures the intensity and spectral line profile of HI Ly up to heliocentric heights of 3.5 solar radii. It also measures the intensities of the OVI doublet at 1032 and 1037 Å and of Fe XII at 1242 Å. The HI Ly line profile measurements are used to determine the random velocity distribution of coronal protons along the line-of-sight. The absolute HI Ly intensities can be used together with electron densities from the white light coronagraph to estimate electron temperatures from hydrogen ionization balance calculations, and bulk outflow velocities from models of Doppler dimmed resonant scattering. Intensities of minor ion lines are used to determine coronal abundances and outflow velocities of O⁵⁺. Ultraviolet spectroscopy of extended coronal regions from the 11 April 1993 mission of Spartan 201 are discussed.     

The spacelab Lyman alpha and white light coronagraphs program

The Harvard-Smithsonian Center for Astrophysics and the High Altitude Observatory have defined a joint coronagraphs experiment for a future Spacelab mission. The instrumentation package would include an ultraviolet light coronagraph to measure the intensity and profiles of spectral lines formed between 1.2 and 8 solar radii from Sun center and a white light coronagraph to measure the intensity and polarization of visible light. The overall goals of the joint program are to use new coronal plasma diagnostic techniques to understand the physical processes and mechanisms operating in the solar corona, to understand the acceleration of high-speed and low-speed solar wind streams and to extrapolate this knowledge to other stars in order to help understand the physics of stellar coronae and stellar mass loss.Proceedings of the Conference Solar Physics from Space, held at the Swiss Federal Institute of Technology Zurich (ETHZ), 11–14 November 1980.     

Source Region of High and Low Speed Wind during the Spartan 201-05 Flight

The large-scale coronal magnetic fields of the Sun are believed to play an important role in organizing the coronal plasma and channeling the high and low speed solar wind along the open magnetic field lines of the polar coronal holes and the rapidly diverging field lines close to the current sheet regions, as has been observed by the instruments aboard the Ulysses spacecraft from March 1992 to March 1997. We have performed a study of this phenomena within the framework of a semi-empirical model of the coronal expansion and solar wind using Spartan, SOHO, and Ulysses observations during the quiescent phase of the solar cycle. Key to this understanding is the demonstration that the white light coronagraph data can be used to trace out the topology of the coronal magnetic field and then using the Ulysses data to fix the strength of the surface magnetic field of the Sun. As a consequence, it is possible to utilize this semi-empirical model with remote sensing observation of the shape and density of the solar corona and in situ data of magnetic field and mass flux to predict values of the solar wind at all latitudes through out the solar system. We have applied this technique to the observations of Spartan 201-05 on 1–2 November, 1998, SOHO and Ulysses during the rising phase of this solar cycle and speculate on what solar wind velocities Ulysses will observe during its polar passes over the south and the north poles during September of 2000 and 2001. In order to do this the model has been generalized to include multiple streamer belts and co-located current sheets. The model shows some interesting new results. This revised version was published online in August 2006 with corrections to the Cover Date.     

Interstellar grains in the solar system: Requirements for an analysis

We discuss present knowledge about interstellar dust grains in the heliosphere in order to give goals for future investigations. As far as the identification of the interstellar flux from brightness observations is concerned we calculate the influence of interstellar dust entering the solar system on the Zodiacal light and Zodiacal emission brightness. In case of the Zodiacal light produced by the scattering of solar radiation, the brightness from interstellar dust within the solar system is not detectable within the limits of present observations. In the case of the thermal emission a distinction of the brightness from the interstellar dust component may be possible. This would be especially interesting for an analysis of the overall spatial distribution of the interstellar flux in the solar system. As far as the identification of the interstellar flux from impact experiments is concerned, parameters like the impact direction are essential. Since the interstellar dust flux is modified in the outer solar system already, it is helpful to probe its variation with increasing distance from the Sun in interstellar upstream direction.     

Space-borne coronagraphy

We consider the main aspects of a rather delicate discipline, space-borne coronagraphy, which is essentially performed with white-light, externally-occulted coronagraphs. Methods of observation and recent results are presented in a scientific section; a short account of historical rocket-borne and balloon-borne experiments is also given. The review concentrates on both the NRL-type coronagraphs and the HAO-type coronagraphs, stressing the essential features and merits of numerous experiments which were flown. A small section is devoted to other designs. A large number of figures, including many drawings, are used to illustrate the growing complexity of experiments.Dedicated to: B. Lyot, who built the first ground-based coronagraph; G. Newkirk, who built the first flying coronagraph; G. Nikolsky, who built the largest, each of whom prematurely passed away.On leave from Paris Institut d'Astrophysique CNRS, 98 Bis Bd Arago, F-75014, Paris, France.     

机载显示器亮度自适应调节算法研究

合适的亮度能够帮助驾驶员更加准确有效地获取机载显示器上的信息。为了使显示器亮度能够适应各种环境光照度，提出了基于韦伯-费希纳定律的步进式亮度调节算法，将显示器亮度与环境光照度的对数成正比，同时根据人眼能识别的最小相对亮度变化量将显示器亮度进行分级，以人眼明暗适应的不同要求调整步进大小，使显示器亮度能够在环境光照度变化时自动而柔和的调节。为了满足不同驾驶员的个性化要求，还考虑了手动调节介入的影响，使自动亮度调节曲线能够实时更新，达到自适应的调节效果。     

适合航天飞机应用的星体跟踪器

本文推导了航天飞机采用新型探测器件——电荷耦合器件CCD（ChargeCoupled DeVices）组成的星体跟踪器进行姿态稳定的公式。并提供一种适合航天飞机应用的星体跟踪器原理样机。     

双通道微波辐射计大气折射率剖面反演的神经网络算法

基于地基双通道微波辐射计（23．8GHz和31．65GHz）所测天顶方向的亮温测量数据和地面气象参数,给出了一种利用微波辐射测量反演大气折射率剖面的神经网络算法。利用青岛地区历史探空数据仿真的大气辐射亮温对神经网络进行了训练,回归得到了三段折射率剖面模型,并对利用实测亮温反演的大气折射率剖面与探空实测折射率剖面和模式剖面进行了比较分析,分析结果表明利用微波辐射计反演的折射率剖面与实测剖面间有很好的一致性,较三段折射率剖面模式具有更好的反演精度。     

Dynamic Modeling of Brushless dc Motors for Aerospace Actuation

A discrete time model for simulation of the dynamics of samarium cobalt-type permanent magnet brushless dc machines is presented. The similation model includes modeling of the interaction between these machines and their attached power conditioners. These are transistorized conditioner units. This model is part of an overall discrete-time analysis of the dynamic performance of electromechanical actuators, which was conducted as part of prototype development of such actuators studied and built for NASA-Johnson Space Center as a prospective alternative to hydraulic actuators presently used in shuttle orbiter applications. The resulting numerical simulations of the various machine and power conditioner current and voltage waveforms gave excellent correlation to the actual waveforms collected from actual hardware experimental testing. These results, numerical and experimental, are presented here for machine motoring, regeneration and dynamic braking modes. Application of the resulting model to the determination of machine current and torque profiles during closed-loop actuator operation were also analyzed and the results are given here. These results are given in light of an overall view of the actuator system components. The applicability of this method of analysis to design optimization and trouble-shooting in such prototype development is also discussed in light of the results at hand.     

The Rotation of the Fe XIV Solar Corona During the Recent Solar Activity Minimum

We analyze data observed by the LASCO C1 coronagraph on board the SOHO spacecraft during the solar minimum activity from April 1996 to March 1997. Using the phase dispersion technique, we investigate the periodicity and recurrence of Fe XIV emission structures with heliospheric latitude and distance above the Sun's surface with high spatial resolution. We find no significant deviation from a rigidly rotating Fe XIV corona with latitude or with distance from the Sun even on these small scales. In agreement with earlier work, the coronal rotation period at solar minimum is about 27.5 ± 1 days. This revised version was published online in June 2006 with corrections to the Cover Date.     

Electronic device for the blind

Electronic devices are a help for the blind. Some electronic devices push video signals directly to the brain but the device presented in this paper uses a sensitive and ready sensorial system: the auditory system. This article presents a low cost electronic device that enables the blind to distinguish the color and distance of objects. The project was first published in the UK and that system with the intensity of musical notes proportional to the brightness has proven to be annoying as the musical notes sound uninterrupted. In order to solve this problem, a new system for brightness perception was designed so a brief musical note is sounded when the sensor detects an increase of brightness and another brief musical note, one octave below, is sounded when the sensor detects a decrease in brightness     

EUV and Radio Observations of an Equatorial Coronal Hole

An equatorial coronal hole has been observed on 18 and 19 October 1996 with SOHO-CDS and with the Nancąy Radioheliograph (RH). The CDS EUV line intensities are used to determine the coronal hole Differential Emission Measure (DEM); in turn this is used to compute the radio brightness temperature T_b at the observed frequencies, leaving the coronal electron temperature and density as free parameters. EUV line intensities, calculated from the derived models, show a good agreement with EUV observations. This revised version was published online in June 2006 with corrections to the Cover Date.     

Yohkoh results in the context of the high-latitude heliosphere

Designed primarily to study solar activity, Yohkoh includes an X-ray telescope that obtains full-sun coronal images which show a range of features. Coronal X-ray emission-exclusive of flares, is notable for its variability even in the largest structures. A mass ejection event is related to magnetic field reconnection. Such events exhibit both accelerated and decelerated behaviour. Coronal hole temperatures are estimated from the filter ratio method. A plasma component at around 2.10⁶ K is identified. X-ray emission is detected from the South polar coronal hole. A preliminary comparison of Spartan coronagraph images with Yohkoh data suggests that polar plumes or rays are not connected to bright points.     

航天飞机头部无粘绕流的无波动,无自由参数格式的数值计算

本文采用气动中心张涵信教授提出的无波动、无自由参数耗散格式(NND)进行了如下的计算:航天飞机头部段对称剖面内的二维无粘绕流;航天飞机头部段三维无粘绕流;轴对称凹陷外形的三维无粘绕流。在物面坐标系下,用代数方程生成计算网格,利用特征相容关系式处理激波和物面边界。为了比较,还用SCM格式进行了计算。结果表明,本文所采用的NND格式,在捕捉流场内激波时不会出现非物理振荡,其收敛速度和所获得的计算结果都是令人满意的。     

Leasecraft: An Innovative Space Vehicle

The Leasecraft system is an innovative means to provide a permanent mobile platform in low Earth orbit and the related launch, integration, test, operation, and in-orbit servicing for payloads of industrial and government users. The Leasecraft system is being funded and developed by Fairchild Industries and furthers the industrialization of space with its significant business potential. The technology and techniques underlying this venture are derived from the shuttle compatible multimission modular spacecraft (presently used for the NASA solar maximum mission and Landsat-D/D' mission) and the upcoming demonstration of shuttle repair to be performed on the solar maximum satellite in the first quarter of 1984. Leasecraft can be identified as a system, comprising a low orbit space platform, an operations control center, user accommodations, and services such as payload interfaces, documentation, and ground support equipment and procedures. The combination of these elements facilitates the use of the space environment by both the space and nonspace oriented user. Early potential applications of Leasecraft include the processing of pharmaceuticals and materials, satellite-aided search and rescue, data collection, and support of NASA's astrophysics programs. Initial assessments made concerning the benefits to users and the cost of providing these benefits indicates that Leasecraft can provide needed services at very competitive rates. The leasing arrangement is cost effective as compared with present spacecraft platform development and cost assessment techniques.     

TiAl金属间化合物研究

TiAl金属间化合物是新一代发动机热端和航天飞机外部零件可采用的材料，比钛合金更耐高温且密度更低，本文分析了γ－TiAl基合金室温脆性的原因以及改善方法。     

The STEREO Mission: An Introduction

The twin STEREO spacecraft were launched on October 26, 2006, at 00:52 UT from Kennedy Space Center aboard a Delta 7925 launch vehicle. After a series of highly eccentric Earth orbits with apogees beyond the moon, each spacecraft used close flybys of the moon to escape into orbits about the Sun near 1 AU. Once in heliospheric orbit, one spacecraft trails Earth while the other leads. As viewed from the Sun, the two spacecraft separate at approximately 44 to 45 degrees per year. The purposes of the STEREO Mission are to understand the causes and mechanisms of coronal mass ejection (CME) initiation and to follow the propagation of CMEs through the inner heliosphere to Earth. Researchers will use STEREO measurements to study the mechanisms and sites of energetic particle acceleration and to develop three-dimensional (3-D) time-dependent models of the magnetic topology, temperature, density and velocity of the solar wind between the Sun and Earth. To accomplish these goals, each STEREO spacecraft is equipped with an almost identical set of optical, radio and in situ particles and fields instruments provided by U.S. and European investigators. The SECCHI suite of instruments includes two white light coronagraphs, an extreme ultraviolet imager and two heliospheric white light imagers which track CMEs out to 1 AU. The IMPACT suite of instruments measures in situ solar wind electrons, energetic electrons, protons and heavier ions. IMPACT also includes a magnetometer to measure the in situ magnetic field strength and direction. The PLASTIC instrument measures the composition of heavy ions in the ambient plasma as well as protons and alpha particles. The S/WAVES instrument uses radio waves to track the location of CME-driven shocks and the 3-D topology of open field lines along which flow particles produced by solar flares. Each of the four instrument packages produce a small real-time stream of selected data for purposes of predicting space weather events at Earth. NOAA forecasters at the Space Environment Center and others will use these data in their space weather forecasting and their resultant products will be widely used throughout the world. In addition to the four instrument teams, there is substantial participation by modeling and theory oriented teams. All STEREO data are freely available through individual Web sites at the four Principal Investigator institutions as well as at the STEREO Science Center located at NASA Goddard Space Flight Center.     

Study of Dynamical Properties of Coronal Structures in the Polar Regions

We present the results from a study of the dynamical properties of polar jets in the Sun's polar regions using LASCO C2 coronagraph and EIT observations. In the simplest impulsive acceleration scenarios for jets, gravity is expected to be the dominant force on the jet following the initial acceleration, especially in the Sun's polar regions where the open magnetic fields should not significantly impede the jet's motion. Our analysis shows that although at low heights the kinematics of the jets could be consistent with a gravitational deceleration of the ejected plasma, at higher heights their motions may simply follow the ambient solar wind outflow. If so, the polar jets can be used as tracers of the solar wind in coronal holes. This revised version was published online in June 2006 with corrections to the Cover Date.     

Spatial distribution and orbital properties of interplanetary dust at high latitudes

Although the interplanetary dust cloud is assumed to be mainly concentrated in the ecliptic plane, there is a component of dust particles on highly inclined orbits that forms the out-of-ecliptic distribution. The ULYSSES mission for the first time makes this component accessible to in-situ, detection. Evidence for this dust component is also provided from the analysis of the Zodiacal light brightness and especially from the spherical shape of the solar F — corona. An obvious source for an out-of-ecliptic dust population is the activity of comets on high eccentric, highly inclined orbits. We discuss the dynamical conditions of particles under the influence of the radiation pressure when released from the comet and discuss their input to the dust cloud based on brightness analysis and in-situ results.