基于HFSS的蓝宝石谐振器仿真设计

本文介绍了一种工作在回音壁模式下的蓝宝石谐振器的仿真方案.该方案基于Ansoft HFSS软件,首先通过本征模模式探究了蓝宝石柱体与腔体的尺寸改变对不同回音壁模式谐振频率与无载品质因数的影响;再向谐振腔中加入了耦合端口,通过驱动模式探究耦合端口位置与形状的改变对整个谐振腔传递函数的影响.最终设计出的蓝宝石谐振器有着良好...     

MOEMS陀螺的谐振腔设计

微光机电(MOEMS)陀螺代表着微型光学陀螺的重要发展方向,而MOEMS谐振腔的设计是谐振式MOEMS陀螺的核心技术.提出了一种新颖的基于微纳米加工技术的MOEMS空间谐振腔结构,介绍了其工作原理和系统构成.建立了谐振腔的数学模型,并利用MATLAB软件对其重要参数进行了仿真计算及分析.为提高谐振腔清晰度及系统测量精度,优化了谐振腔输入输出镜的技术指标,并在此基础上完成了谐振腔的微加工工艺设计.结果表明:所设计的谐振腔清晰度可以达到346,陀螺极限灵敏度为0.25(°)/h,同时可以有效克服克尔效应、背向散射、偏振等光路噪声的影响.      

电介质测量中的谐振腔Q因子特性

对同轴线-集中电容负载谐振腔, 采用传输测量使用的3dB 三频法决定有载Q_l, 计及谐振频率下的插入损耗后获得无载Q_u, 对同一腔体, 也用单端口反射测量技术的xdB 三频法, 并通过测量回程损耗在谐振点和xdB 点的输入反射系数振幅来获得无载Q_u. 在500MHz 下40 个不同的耦合状况下, 两种方法得到无载Q_u的算术平均值和标准差为2519±34. 这两种技术被用来调节和实现传输型谐振腔的输入、输出的等耦合和电介质测量, 本文从介质损耗测量的观点讨论了如何使用有载Q_l和无载Q_u.      

带状注分布作用速调管多间隙谐振腔高频特性

带状注分布作用速调管(SBEIK)的典型特征是平面多间隙谐振腔及其分布式注波互作用系统.对应用于W波段微型化SBEIK的一种强耦合式五间隙分布作用谐振腔进行了研究,并结合传统的弱耦合式谐振腔与输出腔对其高频特性进行了深入分析,结果表明强耦合式腔体具备谐振模式隔离、各间隙高频场(RF)的耦合及其能量输出的良好技术优势.此外,对五间隙谐振腔周期结构引入的轴向简并模式竞争问题进行了研究,得到其工作模式与竞争模式之间的频率间隔在600MHz以上,完全可以满足SBEIK整体方案设计中100MHz带宽的要求.最后,利用三维粒子模拟(PIC)软件对优化后的强耦合式五间隙输出腔注波互作用性能进行了初步的模拟仿真,验证了其在相应工作模式上具备了高功率产生与输出的技术特征.本研究工作对毫米波和太赫兹频段高功率SBEIK的物理设计与工程研究具有重要的价值.      

极小型氢频标磁控管微波腔的仿真设计

用Ansoft HFSS仿真软件建立了极小型氢频标磁控管微波腔的几种模型结构,在给定腔体尺寸下,仿真了不同电极间距的空型和磁控管型微波腔谐振频率和品质因数,得出极小型氢频标磁控管微波腔的设计参数,并对实际设计中影响磁控管微波腔谐振频率的因素给出了建议。     

考虑陀螺频率特性的角速率输入圆锥补偿算法

针对陀螺直接输出角速率且通带内增益不一致(频率特性),而传统角速率输入圆锥补偿算法要求输入理想的角速率,提出了一种考虑陀螺频率特性的角速率输入圆锥补偿算法.推导了圆锥运动情况下姿态更新周期内理想旋转矢量增量和实际姿态算法计算的旋转矢量增量,以最小化理想旋转矢量增量和计算旋转矢量增量之间非周期项的差异为计算圆锥误差补偿系数的准则,最优补偿系数可以看成是采用理想角速率输入的圆锥补偿算法系数与考虑频率特性时对理想圆锥补偿算法系数修正的和.得到了公式化求解考虑频率特性的各子样算法最优系数的方法.仿真结果表明,所提出的算法比传统角速率输入圆锥补偿算法在精度上有明显提高.     

PCB材料与电源/地层谐振阻抗关系

为降低多层高速PCB(Printed Circuit Board)电源/地谐振阻抗,根据平行平面腔体谐振模型理论推导出PCB电源/地谐振阻抗、谐振频率、谐振品质因数与构成PCB板的导体材料和绝缘材料的电磁参数的之间的函数关系式,并根据此关系式得出了从PCB材料选取角度减小电源/地谐振阻抗的两种途径,即采用高磁导率、低电导率的导体材料代替普通导体材料;采用高介电常数和损耗正切的平面间绝缘体材料.随后PCB电源/地平行平面结构的全波仿真结果证实了这两种途径的有效性.      

谐振腔法复介电常数测量系统的谐振频率标定

微波介质材料的复介电常数,或称相对介电常数和介质损耗角正切参数是表征其介电特性的最重要的物理参数。目前对于微波介质材料普遍采用谐振法进行测试,但仍然存在测试频率不够高、测量结果一致性不理想等诸多问题。本文以本单位自行研制的基于分离圆柱体谐振腔法的材料复介电常数测量夹具所建立的微波复介电常数测量系统为研究对象,通过实验的方法,对该测量系统的TE_(011)的谐振频率这一关键指标的最优测试条件、标定方法和结果、稳定性等进行了系统地研究,实验结果表明,该谐振腔法测量系统非常适合作为计量标准装置,用于微波介质材料标准样片的复介电常数的计量和校准。     

谐振式微光学陀螺标度因数及其非线性度分析

谐振式微光学陀螺(RMOG, Resonator Micro-Optic Gyro)输出标度因数非线性度在大角速度应用时变得明显,影响陀螺性能.理论分析了RMOG中频率调制偏置量对标度因数及其非线性度的影响;根据RMOG谐振腔的谐振输出特性,仿真计算了输入角速度范围内的理论标度因数及其非线性度.利用已知的温度性能测试结果建立了标度因数温度误差模型.搭建RMOG实验系统,实际测量输出标度因数~0.95.模拟和实际转动实验得到±500(°)/s范围内标度因数非线性度分别为6.88×10^-4和0.93%,表明通过有效消除环境因素影响,可以使RMOG的输出非线性度满足多数惯性应用的要求.     

太赫兹肖特基二极管混频性能分析

工作在太赫兹波段的肖特基混频二极管的混频性能会受到高频效应的影响而降低.将有限差分算法引入二极管内部电磁场的计算中,并从结电容并联效应、趋肤效应、等离子共振、速率饱和效应四个方面分析了高频效应对二极管混频性能的影响,并以截止频率作为品质因数,对二极管结构参数进行优化设计.仿真实验结果表明:随着频率的提高,减小阳极直径、减小外延层厚度和提高外延层掺杂浓度能减小高频效应的影响,提高太赫兹二极管的混频性能.     

Near infrared observations of comet Halley from Vega 2

Spatial distribution of the continuum radiation in the range of 0.95–1.9 μm presumes total dust production rate of the comet of 10ρ tonne s⁻¹ (ρ is the dust material density) and its angular distribution proportional cos . Observations of the water vapor band at 1.38 μ m reveal strong jets, their time shift from the dust jet measured in situ is consistent with gas velocity of 0.82±0.1 km s⁻¹ and dust velocity of 0.55±0.08 km s⁻¹. The OH vibrational-rotational bands observed are excided directly via photolysis of water vapor. Water vapor production rate deduced from the H₂O band and OH band intensities is 8×10²⁹ s⁻¹. Intensity of the CN(0,0) band result in the CN column density of 9×10¹² cm⁻², i.e. larger by a factor of 3 than given by the violet band.     

High-velocity impact experiments needed to improve our understanding of the asteroids

The lifetime of almost all the asteroids against catastrophic impact events is less than the age of the solar system, implying that the asteroids can be considered as outcomes of catastrophic collisions. Therefore to understand their physical properties (structure, shape, rotation, regolith development) and their family memberships (since families are generated by the escape of breakup fragments), a systematic knowledge of the outcomes of catastrophic impacts under a variety of conditions seems needed. In particular, interesting fields to be explored by laboratory experiments are: the dependence of the critical energy densities associated with various degrees of fragmentation on the target's size and composition; the velocity distribution of the fragments and the inelasticity of the process in different cases; the shape of the fragments and its possible correlation with other quantities; the way a dust- or regolith-covered target affects the collisional outcomes; the angular momentum partitioning and the rotation of the fragments. On this latter problem very few experimental results are presently available; on the other hand, the rotation of small asteroids presents several intriguing “anomalies”.

A significant progress of our understanding of asteroid collisional evolution and related phenomena can be provided by new laboratory experiments of collisional breakup. The targets should have spherical and/or irregular shape (up to axial ratios of the order of 2), and should be made of (possibly different) geological materials. The interesting projectile velocities are of the order of the relative velocities commonly found among asteroids, i.e., in the range 1 to 10 Kms⁻¹. In order to get catastrophic collisions, the ratio of the projectile kinetic energy to the target mass (≡E/M) has to be chosen within a “critical” range (for basalt targets, from 10⁶ to 10⁸ erg/g). In some particular cases, this kind of experiments has been already performed in past (Gault and Wedekind [10]; Fujiwara et al. [7]; Fujiwara and Tsukamoto [9]); however the generalization of the results to a wide range of experimental conditions is lacking, and many problems of outstanding importance to model asteroid evolution are still completely open.     

Geminga pulsar observations with gamma-telescope Gamma-1

The Geminga light curve obtained with the “Gamma-1” telescope features two peaks separated by 0.5 ± 0.03 period. The light curve is pronounced for γ-quanta energies higher than 400 MeV. The pulsed flux upper limit (1σ) in the energy interval 50 – 300 MeV is 6·10⁻⁷ cm⁻²sec⁻¹. For energies >300 MeV the pulsed component power law spectrum has an exponent 1.1 _−0.3^+1.1 and an integral flux (1.1±0.3)·10⁻⁶ cm⁻²sec⁻¹.     

Modelling the neutral gas environment of comets with special application to P/Halley

A technique has been developed which allows relatively accurate modelling of cometary gas production from nothing more than a visible light curve. Application to P/Halley suggests the production rate of parent molecules will be about 2.6 × 10²⁹ per second on March 10, 1986, for example. The uncertainties and intrinsic limitations in this approach are outlined. The theory is then extended to predictions of abundance of other gaseous species, and a photometric model of these gases provided. Combined with the dust model of N. Divine, preliminary predictions of the luminance of P/Halley as seen in any direction from inside the coma or outside can be provided for λλ3000–7000.     

Physical properties of cometary dust: Relation of DIDSY data to grain properties

The Dust Impact Detection System (DIDSY) for the Giotto Halley Mission consists of two types of sensors for the detection of cometary dust particles: two impact plasma sensors and five piezo-electric momentum sensors. One sensor of each type is covered by a penetration film. A 1 μm thick aluminum film covers an impact plasma sensor. One momentum sensor is mounted onto the rear shield behind the 1 mm front shield made from aluminum. The parameters measured are the total charge released upon impact and the amplitude of the acoustic signal generated by the impact. Both quantities depend on the mass and speed of the impacting particles. At the impact speed of 68 km/sec the mass of cometary dust particles can be determined in the mass range from 10⁻¹⁷ g to 10⁻³ g. From the difference in the countrates measured by the sensors with and without penetration film the average bulk density of dust particles of masses 10⁻¹⁴ g and 10⁻⁶ g can be determined. With appropriate calibration an accuracy of a factor of 2 for both the mass and density determination can be obtained.     

S3 and S4 absorption cross sections in the range of 340 to 600 nm and evaluation of the S3 abundance in the lower atmosphere of Venus

S₃ absorption cross section equals 6×10⁻¹⁷ cm² at 400 nm, 6 × 10⁻¹⁹ cm² at 500 nm (less by a factor of 4 than that given by Sanko), 4×10⁻²⁰ cm² at 600 nm. That of S₄ equals 1.5 × 10⁻¹⁷ cm² at 450 nm, 8 × 10⁻¹⁷ cm² at 500 nm, and 4.7 × 10⁻¹⁷ cm² at 600 nm. Preliminary evaluation of the S₃ mixing ratio in the lower atmosphere of Venus is (8±3)×10⁻¹¹ at 5 to 25km according to the Venera 14 measurements and several times lower at the locations of the Veneras-11 and -13.     

Investigation of the differential rotation of the large-scale magnetic elements for the solar activity cycles 20 and 21

The differential rotation of the patterns of the large-scale solar magnetic field during solar activity cycles 20 and 21 is investigated. Compact magnetic elements with the polarity of the general solar magnetic field have larger speed of rotation than the elements with the opposite polarity. The surface of the Sun was divided by 10°-zones. In all of them the average rotation rate of the magnetic elements with negative polarity is little higher than that of the magnetic elements with positive polarity, except for 50°-zone of the south hemisphere and at the 10° latitude of the north hemisphere.

The rates of differential rotation for large-scale magnetic elements with negative and positive polarities have similar behavior for both cycles of the solar activity.

The rotation rate varies at polarity reversal of the circumpolar magnetic fields. For the cycle No 20 in 1969–1970 the threefold reversal took place in the northern hemisphere and variations of rotation rate can be noticed for magnetic elements both with positive and negative polarity for each 10°-zone in the same hemisphere.     

High spectral resolution Fabry-Perot interferometer measurements of comet Halley at H-alpha and 6300 Å

A 40.6 cm Newtonian telescope has been interfaced to the Fabry-Perot interferometer at the Arecibo Observatory to make high spectral resolution measurements of Comet Halley emissions at 6562.72 Å (H-alpha) and 6300.3 Å (OI). In March 1986 the H-alpha surface brightness for a 5′.9 field of view centered on the comet nucleus decreased from 39±7.8 rayleighs on 12 March to 16±3.8 rayleighs on 23 March. The atomic hydrogen production rate on 12 March 1986 was 1.62±0.5 × 10³⁰ s⁻¹, and on 23 March 1986 it was 6.76±2.3 × 10²⁹ s⁻¹. Using spectral resolution of 0.196 Å, we found the atomic hydrogen outflow velocity to be approximately 7.9±1.0 km s⁻¹. In general, the H-alpha spectra are highly structured, and indicative of a multiple component atomic hydrogen velocity distribution. An isotropic outflow of atomic hydrogen at various velocities is not adequate to explain the spectra measured at H-alpha. The 6300.3 Å emission of O(1D) had a surface brightness of 81±16 rayleighs on 15 March 1986, and 95±11 rayleighs on 17 March 1986. After adjustment for atmospheric extinction, the implied O(1D) production rate on 15 March is 6.44±3.0 × 10²⁸ s⁻¹, and the production rate on 17 March is 5.66±2.7 × 10²⁸ s⁻¹. These spectra included a feature at 6300.8 Å that we attribute to NH₂. The brightness of this emission feature was 37±11 rayleighs on 15 March.     

HXMT satellite for space hard X-ray observation

In this paper, the Hard X-ray Modulation Telescope mission is introduced. Its primary objective is to perform the hard X-ray all sky survey of high resolution and high sensitivity. The expected angular resolution and position accuracy of the satellite are better than 10^′ and 2^′, respectively. The preliminary mission design is analyzed. And a new attitude subsystem scheme is presented to meet the high precision demand of attitude determination. A conclusion is drawn that the mission design is feasible. The possible launch of it will significantly advance the astrophysical study.