现代教育技术在高职高专教学中的应用

计算机网络是现代教育技术的基础 ;开发和应用教学资源是开展教育技术工作的中心 ;建立专门从事现代教育技术开发、管理、推广、应用的机构和师资队伍是开展现代教育技术工作的保障。现代教育技术在教学中的应用优势和高职高专教学培养目标要求之间的一致性 ,使我们可以应用现代教育技术来促进高职高专教学的改革     

高职高专院校现代教育技术中心的构建与管理--西安航专现代教育技术中心的构建与管理模式分析

做好高职高专院校现代教育技术中心的构建与管理 ,对于促进学校现代教育技术工作的健康发展具有重要的作用。以西安航专现代教育技术中心的构建与管理模式为例 ,从隶属关系、职能职责、组织结构、人员构成以及设备配置等方面进行了分析、探讨 ,提出了加快发展高职高专院校现代教育技术中心的建议和思路     

基于现代教育技术的虚拟实验系统构建模式的研究

虚拟实验系统是现代教育技术和实践教学理论相结合的产物。通过对网上虚拟实验系统构建技术的全面分析和总结 ,将适合于高职高专院校的虚拟实验教学系统的构建模式划分为模拟演示型、系统仿真型、虚拟操作训练型和真实测量型等四种类型 ,并给出了对于高职高专院校具有重要的意义的构建方案、实现思路、适用场合和应用案例     

我国高职教育改革发展现状的思考——以西安航空职业技术学院为例

高等职业教育在现代职业教育体系建设进程中具有引领作用,《教育纲要》给职业教育提出新课题,国家产业发展趋势给职业教育提出新思考,向中国创造转变给职业教育提出新期望。以西安航空职业技术学院为例分析高职教育改革的现状和发展方向。高职院校必须根据自身所处的区域社会经济环境来制定学校发展战略,明确定位,办出特色,这对高职高专院校的发展具有一定的借鉴和现实意义。     

陕西省高职高专院校“评建工作”经验交流会召开

2007年4月19日至21日，陕西省高职高专院校“评建工作”经验交流会在西安市阎良区润天宾馆举行。此次会议由陕西省高职高专教育学会主办，目的是为了进一步提高各迎评院校对评建工作的深入认识，给大家提供一个学习和经验交流的平台，促进我省高职高专院校评建工作的顺利开展。     

高职院校学生心理健康问题及解决途径

近年来,高职院校学生的心理问题比较突出,但最终解决问题的效果却不尽人意.旨在探讨新时期高职学生心理健康的现状和存在的问题,分析这些问题的成因,提出了设置健全的心理健康教育机构、加强心理教育师资建设、普及心理学知识、开展心理咨询活动、展开校际合作和进行社会实践活动的心理健康教育模式,以达到对高职学生心理健康教育的效果.     

论现代教育技术与教师的作用

分析、探讨、研究、解决应用现代教育技术中出现的问题 ,对于创新教学模式 ,促进教育教学改革 ,实现教育现代化具有十分重要的意义 ,教师在应用现代教育技术中应发挥主力军作用。     

高职高专院校多媒体语音室的构建

计算机和数字化网络技术的发展 ,对传统的教育体系带来了新的挑战 ,在分析高职高专院校培养应用性人才特点的基础上 ,提出高职高专院校实际的多媒体语音室构建比较方案 ,有利于高职高专院校的教学改革。     

陕西高职高专发展战略及政策问题的思考

陕西高等职业教育具有一定的优势，但在改革与发展中也存在诸多困难和问题，为此，建议省政府实施品牌战略、产业发展带动战略和集团化发展战略；加大政府统筹，创新职业教育管理体制，对高职高专院校实施与本科院校平等的国民待遇，实行校企合作，由学校发放职业资格证书，建立资源共享的实验实训基地，加强政府督导，促进陕西高等职业教育健康发展。     

2007年陕西省高职高专院校学报工作会议在宝鸡召开

根据陕西省高职高专教育学会学报工作委员会工作安排，2007年5月17日-21日在宝鸡市召开了2007年度陕西省高职高专院校学报工作会议，来自全省的14所高职高专院校学报的17名同志参加了会议。     

离子发动机羽流特性的数值模拟

离子发动机羽流中产生的交换电荷(CEX)离子返流会影响航天器的正常工作.建立离子发动机羽流模型,采用单元内粒子方法(PIC)对羽流场进行数值模拟计算.结合DS-1探测器飞行实验的测量结果,分析了卫星电势、电子温度、卫星几何尺寸、推力器工作特性等对相关因素对CEX离子返流特性的影响.结果表明:从推力器出口附近到卫星背面,CEX离子密度为108~1012m-3.当卫星电势从-15V变化到27V,测量点位置处CEX离子密度从0.65×1012m-3变化到1.5×1012m-3.羽流中CEX离子密度和电势结构随电子温度变化不大,但电势大小随电子温度成比例地变化.同一位置处不同工况下CEX离子的密度可根据CEX离子生成率与工作点参数间的关系式准确地估计.卫星安装推力器的表面起着对CEX离子返流屏蔽和降低的作用.      

高压内冷涡轮的气热耦合计算(英文)

本文目的在于验证所开发的适用于涡轮气热耦合模拟的计算程序,并研究转捩对气热耦合计算结果影响。首先在流场求解程序HIT-3D中加入考虑转捩影响的q-ω低雷诺数二方程模型以及AGS代数转捩模型模块,然后采用直接耦合方法关联HIT-3D与自主开发的温度场求解程序,使新程序具备气热耦合求解功能。选取MarkⅡ叶片的三个不同试验工况作为验证算例,在计算中考虑管内流动影响,并对流道内流动分别采用了B-L代数模型、q-ω二方程模型以及B-L&AGS模型,而对管内流动则分别采用了B-L模型与B-L&AGS模型。计算表明采用各模型预测的压力分布与试验吻合较好,而在层流转捩区域采用B-L&AGS模型预测的温度分布与实验吻合最好,而在湍流流动区域,各模型预测的温度分布接近。这一方面表明所开发程序具备较准确进行内冷涡轮气热耦合计算的能力,另一方面也证明了考虑转捩影响对提高气热耦合计算精度的重要性。     

Exploring The Saturn System In The Thermal Infrared: The Composite Infrared Spectrometer

The Composite Infrared Spectrometer (CIRS) is a remote-sensing Fourier Transform Spectrometer (FTS) on the Cassini orbiter that measures thermal radiation over two decades in wavenumber, from 10 to 1400 cm^{− 1} (1 mm to 7μ m), with a spectral resolution that can be set from 0.5 to 15.5 cm^{− 1}. The far infrared portion of the spectrum (10–600 cm^{− 1}) is measured with a polarizing interferometer having thermopile detectors with a common 4-mrad field of view (FOV). The middle infrared portion is measured with a traditional Michelson interferometer having two focal planes (600–1100 cm^{− 1}, 1100–1400 cm^{− 1}). Each focal plane is composed of a 1× 10 array of HgCdTe detectors, each detector having a 0.3-mrad FOV. CIRS observations will provide three-dimensional maps of temperature, gas composition, and aerosols/condensates of the atmospheres of Titan and Saturn with good vertical and horizontal resolution, from deep in their tropospheres to high in their mesospheres. CIRS’s ability to observe atmospheres in the limb-viewing mode (in addition to nadir) offers the opportunity to provide accurate and highly resolved vertical profiles of these atmospheric variables. The ability to observe with high-spectral resolution should facilitate the identification of new constituents. CIRS will also map the thermal and compositional properties of the surfaces of Saturn’s icy satellites. It will similarly map Saturn’s rings, characterizing their dynamical and spatial structure and constraining theories of their formation and evolution. The combination of broad spectral range, programmable spectral resolution, the small detector fields of view, and an orbiting spacecraft platform will allow CIRS to observe the Saturnian system in the thermal infrared at a level of detail not previously achieved.This revised version was published online in July 2005 with a corrected cover date.     

The Swift X-Ray Telescope

he Swift Gamma-Ray Explorer is designed to make prompt multiwavelength observations of gamma-ray bursts (GRBs) and GRB afterglows. The X-ray telescope (XRT) enables Swift to determine GRB positions with a few arcseconds accuracy within 100 s of the burst onset. The XRT utilizes a mirror set built for JET-X and an XMM-Newton/EPIC MOS CCD detector to provide a sensitive broad-band (0.2–10 keV) X-ray imager with effective area of > 120 cm² at 1.5 keV, field of view of 23.6 × 23.6 arcminutes, and angular resolution of 18 arcseconds (HPD). The detection sensitivity is 2×10⁻¹⁴ erg cm⁻² s⁻¹ in 10⁴ s. The instrument is designed to provide automated source detection and position reporting within 5 s of target acquisition. It can also measure the redshifts of GRBs with Fe line emission or other spectral features. The XRT operates in an auto-exposure mode, adjusting the CCD readout mode automatically to optimize the science return for each frame as the source intensity fades. The XRT will measure spectra and lightcurves of the GRB afterglow beginning about a minute after the burst and will follow each burst for days or weeks. Dedicated to David J. Watson, in memory of his valuable contributions to this instrument.     

Effect of boron doping on waterproof and dielectric properties of polyborosiloxane coating on SiO2f/SiO2 composites

A hydrophobic coating of the silica fiber reinforced silica composites (SiO_2f/SiO₂) was synthesized by sol-gel method using methyltriethoxy-silane (MTES) and boric acid (B(OH)₃) as raw materials. The relationship among boron doping, chemical structure of precursors and durability of hydrophobic coatings was discussed. The Si-O-B and methyl groups were successfully introduced in the gel precursors according to the FT-IR and XPS results. The resins were filled in the internal and surface holes of the SiO_2f/SiO₂ composites partially or completely, which is beneficial to reduce the physical adsorption of the moisture. In addition, hydroxyl groups of the SiO_2f/SiO₂ composites reacted with the resins and hydrophobic methyl groups were introduced, leading to the reduction of the chemical adsorption of water. Also, the boron doping was beneficial to enhancing the physical cross-linking between the coating and the SiO_2f/SiO₂ composites, and improved the adhesion of the coating to the substrate. The results show that the optimal hydrophobic coating with contact angle 130.33°, moisture absorption 0.33% and adhesion level 1 is obtained when the molar ratio of MTES to B(OH)₃ is 10:4. The real permittivity of M10B4 is constant in the range of 2.32–2.51 and the dielectric tangent loss is constant in the range of 5.5 × 10⁻⁴–8.7 × 10⁻³. The hydrophobic coating has excellent dielectric properties.     

UVCS/SOHO Observations of H I Lyman Alpha Line Profiles in Coronal Holes at Heliocentric Heights Above 3.0 R⊙

The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) has been used to measure spectral line profiles for H I Lyα in the south polar coronal hole at projected heliocentric heights from 3.5 to 6.0 R_⊙ during 1998 January 5–11. Observations from 1.5 to 2.5 R_⊙ were made for comparison. The H I Lyα profile is the only one observable with UVCS above 3.5 R_⊙ in coronal holes. Within this region the outflowing coronal plasma becomes nearly collisionless and the ionization balance is believed to become frozen. In this paper, the 1/e half widths of the coronal velocity distributions are provided for the observed heights. The velocity distributions include all motions contributing to the velocities along the line of sight (LOS). The observations have been corrected for instrumental effects and interplanetary H I Lyα. The half widths were found to increase with projected heliographic height from 1.5 to 2.5 R_⊙ and decrease with height from 3.5 to 5 R_⊙. This revised version was published online in June 2006 with corrections to the Cover Date.     

热真空环境对常用胶接材料性能的影响

空间的热真空环境是造成光电子器件胶接材料性能退化和放气污染的重要因素.为此,考察了几类典型胶接材料的热真空老化和热真空挥发特性,分析了热真空老化后的力学性能变化及真空挥发产物的主要来源,并对热真空挥发预处理方法进行了验证.结果表明软质的硅橡胶与硬质的环氧树脂胶和丙烯酸树脂胶相比有着更大的质量损失,且含有端羟基的缩聚型硅橡胶和环氧树脂胶真空老化后的模量变化较大.通过真空预处理可以作为降低固化胶真空挥发产物来源的一种有效手段.可为宇航用光电子器件胶接材料的设计选型提供参考依据.     

Variable slip window technology in transition detection on pitching airfoil

In the pitching motion, the unsteady transition and relaminarization position plays an important role in the dynamic characteristics of the airfoil. In order to facilitate the computer to automatically and accurately calculate the position of the transition and relaminarization, a Variable Slip Window Technology (VSWT) suitable for airfoil dynamic data processing was developed using the S809 airfoil experimental data in this paper and two calculation strategies, i.e., global strategy and single point strategy, were proposed: global strategy and single point strategy. The core of the VSWT is the selection of the window function h and the parameters setting in the h function. The effect of the VSWT was evaluated using the dimensionless pulse strength value (INB), which can be used to evaluate the signal characteristics, of the root mean square (RMS) value of the fluctuating pressure. It is found that: the h function characteristics have a significant influence on the VSWT. The suitable functions are H_n function constructed in this paper and step function. For the left boundary of the magnified area, the step function can obtain the largest INB value, but the robustness is not good. The H₁ function (Gaussian-like function, n = 1) can show higher robustness while ensuring a large INB value. The two computing strategies, which are single point strategy and global strategy, have their own advantages and disadvantages. The former strategy, that is the single point strategy, can achieve a higher INB value, but the RMS magnification at the feature position needs to be known in advance. Although the INB value obtained by the latter strategy, that is the global strategy, is slightly smaller than the calculation results of the former strategy, it is not necessary to know the RMS magnification at the feature position in advance. So the global strategy has better robustness. The experimental data of NACA0012 airfoil was used to further validate the developed VSWT in this paper, and the results show that the VSWT developed in this paper can still double the INB value of the transition/relaminarization position. The VSWT developed in this paper has certain practicability, which is convenient for the computer to automatically determine the transition/relaminarization characteristics.     

The Radio Frequency Subsystem and Radio Science on the MESSENGER Mission

The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) Radio Frequency (RF) Telecommunications Subsystem is used to send commands to the spacecraft, transmit information on the state of the spacecraft and science-related observations, and assist in navigating the spacecraft to and in orbit about Mercury by providing precise observations of the spacecraft’s Doppler velocity and range in the line of sight to Earth. The RF signal is transmitted and received at X-band frequencies (7.2 GHz uplink, 8.4 GHz downlink) by the NASA Deep Space Network. The tracking data from MESSENGER will contribute significantly to achieving the mission’s geophysics objectives. The RF subsystem, as the radio science instrument, will help determine Mercury’s gravitational field and, in conjunction with the Mercury Laser Altimeter instrument, help determine the topography of the planet. Further analysis of the data will improve the knowledge of the planet’s orbital ephemeris and rotation state. The rotational state determination includes refined measurements of the obliquity and forced physical libration, which are necessary to characterize Mercury’s core state.     

The James Webb Space Telescope

The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth–Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < ; < 5.0 μ m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < ; < 29 μ m.The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations.To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities.