W33B的羟基脉泽辐射

使用两个跃迁频率,观测W33B的OH分子左右圆偏振的脉泽辐射.从左右圆偏振谱的Zeeman速度分裂,导得脉泽活动区的磁场大约为5mG.采用均匀抽运,完全饱和辐射的球模型,估计脉泽活动区的原恒星物质的氢分子数密度为3×107cm-3.      

Bi_(1.9)Pb_(0.3)Sr_(2.0)Ca_(1.7)Mg_(0.3)Cu_(3.1)O_x 超导块材弱连接区的低磁场性

通过对在不同外磁场下Ｂｉ１．９Ｐｂ０．３Ｓｒ２．０Ｃａ１．７Ｍｇ０．３Ｃｕ３．１Ｏｘ超导块材的交流磁化率的测量，获得了样品内晶粒间和晶粒内对外场的不问响应范围．通过与粉状样品实验结果的比较和Ｘ光分析，认为块状样品在温度为１００Ｋ左右出现的抗磁台阶是样品内晶粒间超导弱连接的一种抗磁效应．对弱连接区有效钉扎力Ｆｐ和临界电流密度Ｊｃ与外场Ｈ的关系进行了讨论．     

欧空局发射SOHO卫星

ＳＯＨＯ（ＳｏｌａｒＨｅｌｉｏｓｐｈｅｒｉｃＯｂｓｅｒｖａｔｏ－ｒｙ）意为太阳日光层观测台。这颗卫星计划于１９９５年１２月在美国佛罗里达洲的肯尼迪航天中心发射，进入地球上方１５０万ｋｍ的轨道，它将停留在“日晕”轨道上，连续工作两年。“日晕”轨道位于地...     

“阿里安”火箭1995年月均一发

阿里安空间公司最近公布“阿里安”运载火箭１９９５年的发射计划如下：１．１月，发射欧空局的第二颗地球资源卫星ＥＲＳ－２。２．２月，发射国际通信卫星－７０６。３．３月，发射美国休斯公司的第三颗直接广播卫星ＤＢＳ－３。４．３月，发射法国第一颗军事侦察卫星太阳神－１。５．４月，发射日本电报电话公司（ＮＴＴ）的“Ｎ－星”卫星。６．５月，发射泛美卫星公司的ＰＡＳ－４卫星和以色列Ｓｐａｃｅｃｏｍ卫星通信公司的Ａｍｏｓ卫星。７．６月，发射卢森堡ＳＥＳ公司的Ａｓｔｒａ－１Ｅ卫星。８．８月，发射法国电信公司（Ｔｅｌ…     

航天简讯

韩国建立移动卫星通信与跟踪系统韩国三星公司（Ｓａｍｓｕｎｇ）与美国魁尔康姆公司（Ｏｕａｌｃｏｎ。ｍ）签订了在韩国建立ＯｍｎｉＴｒａｃｓ双向移动卫星通信与跟踪系统的协议，合同价值为１００万美元。根据协议将在韩国汉城郊区建立一个ＯｍｎｉＴｒａｃｓ中心，它由韩国电信部（ＫｏｒｅａＴｅｌｃｏｍ）操作运营。该中心将利用韩国电信部的“高丽卫星”上的Ｋｕ频段转发器。美国魁尔康姆公司所开发的ＯｍｎｉＴｒａｃｓ系统是使用静止轨道卫星实现双向通信与跟踪为目的的系统。三星公司将利用此系统开通卡车、渔船和火车的跟踪业务…     

J-Ⅰ火箭及近期发射计划

一、Ｊ－Ⅰ火箭概要和发射能力１．概要　Ｊ－Ⅰ火箭的第一级利用Ｈ－２火箭的固体助推器（ＳＲＢ），第二级使用文部省宇宙科学研究所发射科学卫星（ＩＳＡＳ）的Ｍ－３ＳⅡ型火箭，上面级由第三级和整流罩这几部分共同组成的三级式火箭。主要技术参数列于表１。表１　Ｊ－Ⅰ火箭主要技术参数项目技术参数总　长／ｍ３３．１外　径／ｍ１．８全部装备重量／ｔ８７．５（不含卫星）制导方式无线电制导方式各级第一级第二级第三级长度／ｍ１９．３６．２２．７外径／ｍ１．８１．４１．５各级重量／ｔ７０．９１３．２３．６推进剂重量／ｔ５…     

AXAF：探测宇宙X射线的新天王

“先进Ｘ射线空间望远镜”（ＡｄｖａｎｃｅｄＸ－ＲａｙＡｓｔｒｏｐｈｙｓｉｃｓＦａｃｉｌｉｔｙ——ＡＸＡＦ）是继“开普顿γ射线空间望远镜”（ＧＲＯ）和“哈勃空间望远镜”（ＨＳＴ）之后，ＮＡＳＡ的第三个大型空间望远镜，耗资１４亿美元，可提供关于黑洞和银河...     

两种信道编码记录方式在光盘应用中的对比

依据数字编码理论对几种光盘编码调制的结构参数性能进行了比较，着重分析了光盘的两种信道编码记录方式：用于磁光（ＭａｇｎｅｔｏＯｐｔｉｃａｌｄｉｓｋ－ＭＯ）光盘的游程长度受限（ＲｕｎＬｅｎｇｔｈＬｉｍｉｍｔｅｄ）脉宽调制（ＰｕｌｓｅＷｉｄｔｈＭｏｄｕｌａｔｉｏｎ）［ＲＬＬ（１，７）－ＰＷＭ］记录方式，及用于相变（ＰｈａｓｅＣｈａｎｇｅ－ＰＣ）光盘的游程长度受限（ＲｕｎＬｅｎｇｔｈＬｉｍｉｍｔｅｄ）脉位调制（ＰｕｌｓｅＰｏｓｉｔｉｏｎＭｏｄｕｌａｔｉｏｎ）［ＲＬＬ（２，７）－ＰＰＭ］记录方式，并结合记录介质的特点，阐明了两者并存的原因．     

Orbcomm星座遇到频率纠纷

自１９９５年４月３日头２颗Ｏｒｂｃｏｍｍ卫星发射成功以来，截至１９９８年９月２３日，共有２８颗Ｏｒｂｃｏｍｍ卫星进入了轨道。这个由２８颗卫星组成的低轨道星座目前正在为全球的大多数地区提供数据和电文传送业务。卫星的发射情况见表１。表１Ｏｒｂｃｏｍｍ卫星...     

极区中层惯性重力波的VHF雷达观测

本文采用ＳＯＵＳＹＶＨＦ雷达１９８７年６月在挪威Ａｎｄｏｐｖａ（６９°Ｎ，１０°Ｅ）的观测数据，研究中层惯性重力波的传播特征．几个周期为数小时的准单色波例子，在垂直方向上有确定的相位移动，表明它们是惯性内重力波．通过分析波相关的流体速度东向和北向分量的变化，获得水平传播矢量的大小和方向，它们与中层高度上典型的观测值一致．同时还观察到三个等相面上行的惯性重力波，其速度偏振椭圆是逆时针旋转的．波相关的扰动速度为１５－４０ｍ／ｓ，说明在中层存在强烈的向下的能量传输．估算出它的运动学参量，周期为数小时，垂直相速度在０．ｌ—０．６ｍ／ｓ之间，垂直波长约为６．０ｋｍ．     

Evidence for a 2200 km extended wave system at the mesopause level

A panoramic view of the nightglow atmospheric emission in the 780–1000 nm spectral range is constructed using CCD images taken at the Pic de Châteaurenard (Altitude 2989 m, Hautes-Alpes) on July 14–15, 1999. A set of 28 images each having a 36° × 36° field of view is assembled to form a panorama covering 360° in azimuth and extending from the horizon to the zenith. Each photograph is processed in order to invert the perpective effect assuming that the emission comes from a thin layer located at the altitude of 85 km. The effect of refraction is calculated and taken into account. The stars are removed using a numerical filter. The inverted panorama appears as a disk having a radius equal to 1100 km. It is comparable to a satellite view of the emissive layer. A wave system extends in the W-NW to E-SE direction over more than 2200 km. A second set of 30 successive images of the same field of view taken on May 18–19, 1998 is used to determine the wave parameters. The main horizontal wavelength is equal to 42 km and the horizontal phase velocity has a value of 40 ± 2 m.s⁻¹. The images show that the atmospheric OH emission is a tracer of the dynamics of the atmosphere at the level where the excited OH radicals are produced. The OH* radical population depends upon its quenching by O, O₂ and N₂. As a result, the emission intensity is a function of the air temperature and density which are subject to variations due to gravity and windshear waves and other dynamic processes such as tides and turbulence.     

Gravity wave mixing effects on the OH*-layer

Based on an advanced numerical model for excited hydroxyl (OH*) we simulate the effects of gravity waves (GWs) on the OH*-layer in the upper mesosphere. The OH* model takes into account (1) production by the reaction of atomic hydrogen (H) with ozone (O₃), (2) deactivation by atomic oxygen (O), molecular oxygen (O₂), and molecular nitrogen (N₂), (3) spontaneous emission, and (4) loss due to chemical reaction with O. This OH* model is part of a chemistry-transport model (CTM) which is driven by the high-resolution dynamics from the KMCM (Kühlungsborn Mechanistic general Circulation Model) which simulates mid-frequency GWs and their effects on the mean flow in the MLT explicitly. We find that the maximum number density and the height of the OH*-layer peak are strongly determined by the distribution of atomic oxygen and by the temperature. As a results, there are two ways how GWs influence the OH*-layer: (1) through the instantaneous modulation by O and T on short time scales (a few hours), and (2) through vertical mixing of O (days to weeks). The instantaneous variations of the OH*-layer peak altitude due to GWs amount to 5–10 km. Such variations would introduce significant biases in the GW parameters derived from airglow when assuming a constant pressure level of the emission height. Performing a sensitivity experiment we find that on average, the vertical mixing by GWs moves the OH*-layer down by ~2 to 7 km and increases its number density by more than 50%. This effect is strongest at middle and high latitudes during winter where secondary GWs generated in the stratopause region account for large GW amplitudes.     

Use of coated silicon field emitters as neutralisers for fundamental physics space missions

Spacecraft neutralisers are required as part of the ion propulsion system for accurate station keeping in fundamental physics missions. This paper describes the use of thin layers of insulating materials as coatings for the gated silicon field emitter array structure used in a spacecraft neutraliser. These thin coatings are postulated to reduce power consumption and reduce overheating. The power consumption and lifetime of aluminium nitride and amorphous hydrogenated diamond-like carbon coatings have been tested by current–voltage and endurance tests. Diamond-like carbon coatings were promising, performing better in endurance tests than uncoated samples, but further work is required to characterise the coating’s physical properties and its effects on field emission. The thermal conductivity of the coating material had little effect on measured sample lifetimes. Aluminium nitride had reduced power consumption compared to diamond-like carbon coated and uncoated samples. A thin (∼5 nm) layer of aluminium nitride was found to be optimal, meeting European Space Agency specifications for the neutraliser engineering model.     

场发射电推力器的参数选择与调控方法

场发射电推力器具有几种不同的发射模式,分别产生荷质比不同的带电液滴或带电离子,使得不同模式下推力性能差别显著。针对不同的空间应用,需要设计不同种类的场发射电推力器,使其达到相应的推力参数。为此对场发射电推力器的发射过程展开分析,确定了推力参数的调控方法。首先对场发射电推力器的基本工作原理进行了阐述,并对不同发射模式的基础物理机制进行了分析。在此基础上通过理论计算得出采用不同推进剂可达到不同发射模式这一结论,并最终得出推力器性能参数的调控方法,论证了推力性能受到推进剂种类和发射模式的影响,在离子发射模式下处于高比冲、低推力工况,而液滴发射模式下处于低比冲、高推力工况。此外推力参数还受到供给流量、外加电压等多种因素的影响。在得到推力器参数的调控方法后,设计了一种主动供给型离子液体电推力器,以离子液体EMI BF4作为推进剂,进行了相应的试验研究。通过改变外加电压,实现了对推力器推力性能的调控,证实了此调控方法的可行性。推力器达到的推力范围为1.6~10μN,比冲范围为154~978s。     

利用OH夜气辉反演原子氧数密度时输入参数的不确定度对反演结果的影响

借助OH夜气辉辐射的光化学模式,由OH夜气辉辐射反演中间层-低热层区域的原子氧数密度时,输入参数的不确定性将导致反演得到的原子氧数密度具有不确定性.以在sudden death猝灭模式下通过OH(8-3)振动带体辐射率反演原子氧数密度为例,分别研究了大气参数和OH气辉辐射率的不确定度引起的反演不确定度、化学反应速率常数的不确定度引起的反演不确定度,以及所有输入参数的不确定度共同引起的反演不确定度,找出其不确定度对反演结果影响最大的参数.结果表明,三种反演不确定度均随着高度的升高而增大,温度和体辐射率的不确定度对第一种反演不确定度的贡献最大,反应速率常数b(8)和A(8-3)、的不确定度对第二种反演不确定度的贡献最大.     

An investigation of the solar cycle impact on the lower thermosphere O(S) nightglow emission as observed by WINDII/UARS

The yearly variation of the integrated emission rate of the O(¹S) nightglow in the lower thermosphere is studied and the solar cycle impact is examined from the observations of the Wind Imaging Interferometer (WINDII) operated on the Upper Atmosphere Research Satellite (UARS). More than 300,000 volume emission rate profiles of the O(¹S) nightglow observed by WINDII for 40°S–40°N latitudes during November 1991–August 1997 over half of a solar cycle are utilized. These profiles are vertically integrated for the altitude range of 80–100 km and the equivalent column integrated emission rates are then zonally averaged for bins with 10° latitude and 3 month intervals. It is found that for each latitude the O(¹S) nightglow emission rate appears to increase with increasing solar F10.7 cm flux, following a linear relationship. This characterizes the solar cycle impact on the O(¹S) nightglow, while the solar influence is modulated by a seasonal variation. Based on these variations, an empirical formula is derived for predicting the three-month averages of the O(¹S) nightglow integrated emission rate. The standard error of the estimated values from the formula is smaller than 30 Rayleigh.     

H-450 X射线参考辐射质的研建及验证

根据PTB和ISO 4037-1:2019要求,关于高空气比释动能系列（H系列）X射线参考辐射质的推荐数据,外推得出H-450的附加过滤为6.24 mm Cu,第一半值层（HVL_1st）为(5.39~5.52)mm Cu,平均光子能量为(214.25~214.78)keV,剂量率为11.51 Gy/h（距离焦斑为1 m处,管电流为10 mA）。随后,使用PTW32005电离室作为测量器具,采用半值层法建立H-450 X射线参考辐射质,得出HVL_1st为5.37 mm Cu,第二半值层（HVL_2nd）为5.97 mm Cu,同质系数为0.9。最后,使用PTW30013次级标准电离室测量得出H-450 X射线参考辐射质下距离焦斑1 m,管电流为10 mA时的剂量率值为11.98 Gy/h,与理论值的相对误差为4.07 %。采用MCNP 5软件对H-450 X射线参考辐射质进行能谱模拟并计算得出其平均光子能量为200.4 keV。     

Simultaneous dual wavelength observations of an impulsive microwave burst using the V.L.A.

Simultaneous observations of a microwave burst at 2 and 6 cm wavelengths were carried out with the Very Large Array (VLA). The 6 cm burst source is located close to a magnetic neutral line, presumably near the top of a flaring loop, while the 2 cm emission originates from the footpoints of the loop. It is concluded that the 6 cm emission is dominated by gyrosynchrotron radiation of the thermal electrons in the bulk heated plasma at a temperature of ～ 4 × 10⁷ K, while the 2 cm emission is due to nonthermal particles released and accelerated during the flare process. From the observed low degree of polarization and the lack of the 2 cm source cospatiality with the 6 cm source a magnetic field of 200–350 G and δ ? 4 are estimated in the flare energy release site. A DC electric field flare model is invoked to explain the long delay between the peaks at the two wavelengths. From the delay, the strength of the electric field is estimated to be 0.2–4 μ statvolt cm^?1 in the flaring region.     

Multiple wavelength observations of flaring active regions

We present observations of flaring active regions with the Very Large Array (V.L.A. at 6 cm and 20 cm wavelengths) and the Westerbork Synthesis Radio Telescope (W.S.R.T. at 6 cm wavelength). These are compared with photospheric magnetograms (Meudon) and with Hα and offband Hα photographs (Big Bear and Ottawa River Solar Observatories). The 6 cm radiation of these active regions marks the legs of dipolar loops which have their footpoints in lower-lying sunspots. The intense, million degree radiation at 6 cm lies above sunspot umbrae in coronal regions where the longitudinal magnetic field strength H_? = 600 Gauss and the height above the sunspot umbrae h = 3.5±0.5 × 10⁹ cm. Circularly polarized horseshoe structures at 6 cm ring the sunspot umbrae. The high degree of circular polarization (?_c = 95%) of the horseshoes is attributed to gyroresonant emission above sunspot^? penumbrae. The 20 cm radiation of these active regions exhibits looplike coronal structures which extend across regions of opposite magnetic polarity in the underlying photosphere. The 20 cm loops are the radio wavelength counterparts of the X-ray coronal loops. We infer semilengths L = 5 × 10⁹ cm, maximum electron temperatures T_e(max) = 3 × 10⁶ K, emission measures ∫N_e²d$\text{l}$ = 10²⁸ cm^?5, and electron densities N_e = 10⁹ cm^?3 (or pressures p = 1 dyn cm^?2) for the 20 cm bremsstrahlung. A total of eight solar bursts were observed at 6 cm or 20 cm wavelength with second-of-arc angular resolution. The regions of burst energy were all resolved with angular sizes between 5″ and 30″, brightness temperatures between 2 × 10⁷ K and 2 × 10⁸ K, and degrees of circular polarization between 10% and 90%. The impulsive phase of the radio bursts are located near the magnetic neutral lines of the active regions, and between the flaring Hα kernels which mark the footpoints of magnetic loops. In one case there was preburst heating in the coronal loop in which a burst occurred. Snapshot maps at 10 s intervals reveal interesting burst evolution including rapid changes of circular polarization and an impulsive burst which was physically separated from both the preburst radio emission and the gradual decay phase of the burst.     

复合式离心泵汽蚀特性的数值模拟与试验分析

为研究某型航天离心泵汽蚀特性,基于Mixture多相流模型与汽蚀模型相结合对长短复合叶轮离心泵内乙二醇水溶液进行不同的进口负压下汽液两相定常数值模拟并进行不同进口压力下的汽蚀性能特性试验,结果表明汽化区域随进口负压的增大而扩大。当进口负压在-50kPa,泵进出口压差在155kPa,已经接近额定压差的3%限制范围,此时离心泵的出口压力105kPa为临界汽蚀出口压力;进口负压到-60kPa时,出口流量突变为300L/h,该泵产生临界汽蚀状态,小于技术要求的最小进口压力10kPa,因此该泵在其工作范围内不会发生汽蚀现象,并证得本文数值模拟的可靠性。