非晶态(Fe_(0.5)Ni_(0.5))_(80-x)Cr_xP_(14)B_6合金薄带的磁场敏感特性的研究

本文对非晶态(Fe_(0.5)Ni_(0.5))_(80-x)Cr_xP_(14)B_6(x=0,1,2,3,4,6,10)合金薄带样品的室温直流磁场敏感特性进行了测量。结果表明,在几十个A/m范围的外磁场内,样品具有开关型磁场敏感特性。对影响开关特性的三个因素进行了一些讨论。     

非晶态(Fe_(0.5)Ni_(0.5))_(80-x)Cr_xP_(14)B_6合金的内禀磁性和热稳定性的研究

对Cr含量变化对非晶态(Fe_(0.5)Ni_(0.5))_(80-x)Cr_xP_(14)B_6(x=0,1,2,3,4,6,10)合金薄带样品的内禀磁性和热稳定性进行了研究。对所得的随着Cr含量增加,样品的磁性原子的平均磁矩(?)和居里温度T_c的减少,热稳定性的提高等结果进行了讨论。当Cr含量x=4at％时,样品表现出一些特殊性质;而当x>4at％和<4at％时,样品的磁性和热稳定性的变化不尽相同。     

非晶态铁镍铬磷硼合金磁致伸缩的研究

本文分别以张力冲击法和应变电阻法对非晶态(Fe_(50)Ni_(50))_(80-z)Cr_xP_(14)B_6合金(x=0,1,2,3,4,6,10)薄带的室温饱和磁致伸缩系数进行了测量;测量结果表明,Cr元素的加入,使样品的λ_(?)有所减少;并对结果进行了讨论。     

SmCox-0.4Ti0.4合金薄带的相结构和磁性能

SmCo_x-0.4Ti_0.4(x=5.0, 5.5, 6.5, 7.0)合金经42m/s速度甩带快速凝固制成薄带,在真空热处理炉中,进行750℃两小时热处理.对制得的甩带状态和热处理状态合金薄带分别测试其相结构和磁性能.结果表明:SmCo_x-0.4Ti_0.4合金甩带状态样品相结构随Co含量的不同而变化,其中x=5.0,5.5和6.5的合金样品由2∶ 17和1∶ 5两相结构组成;x=7.0成分样品由1∶ 7单相结构组成.甩带状态样品的比饱和磁化强度和比剩余磁化强度基本上线性增加,内禀矫顽力在合金成分为x=5.0时出现最大值,为1.01T.薄带样品热处理前后均具有纳米晶结构,表现出剩磁增强效应.样品矫顽力机制主要为形核型,反磁化形核场主要来源于SmCo硬磁相大的磁晶各向异性及其纳米晶结构.热处理后,除x=7.0样品外,其余样品矫顽力均有所下降.     

磁扰和磁静期间海南扩展F起始时间出现率研究

利用2002年2月至2007年12月(第23太阳活动周的下降段)近6年的海南DPS-4型电离层测高仪探测数据, 对磁扰和磁静夜晚期间扩展F起始时间出现率进行统计研究. 结合海南电离层观测站所观测到的扩展F类型, 将扩展F区分为频率型、区域型、混合型和强区域型, 分别进行统计分析. 结果表明, 无论磁扰还是磁静夜晚, 混合型扩展F起始时间总出现率最高, 最为活跃, 其次为频率型和强区域型扩展F, 最不活跃的是区域型扩展F; 无论在磁扰还是在磁静夜晚条件下, 混合扩展F起始时间主要围绕在午夜前后, 且磁静时更多地起始于午夜前, 而磁扰时则倾向于延至午夜后, 频率型扩展F在午夜后较高, 而强区域型扩展F则在午夜前较高. 在本次太阳活动下降阶段, 强区域型与区域型扩展F的起始时间出现率逐年与太阳活动呈现一定的相关性. 所得结果有助于分析不同类型扩展F在形态和机制方面的差异.      

具有不同等离子体β值的Hall MHD重联中的低频波研究

数值研究具有不同等离子体β值(等离子体热压与磁压之比)的Hall MHD重联过程.对于β值在0.5≤β≤6.5的算例,稳态重联率(6)A/(6)t|st为0.15≥(6)A/(6)t|st≥0.095.本文研究β值在上述范围内的Hall MHD重联中的波动.通过快速傅里叶变换(FFT),将平面外磁场By分量和xz平面内的速度分量vx,vz位于给定点的时间序列转换为功率谱.结果表明,By,vx,vz功率谱的频率范围为Ωci＜ω＜8Ωci,其中Ωci为离子回旋频率.随着β值增大,功率谱峰值能量降低,并且朝着低频端移动.对于电场E采用最小方差分析法(MVA)可以确定波的传播方向k,波矢k与局地磁场B之间的夹角α随β值增大而增大.对于β值最大的算例3(β=6.5),α＜28°.上述结果表明,k准平行于B.为了研究波的偏振特征,在垂直于k的平面内画出E的矢端图.三个算例的矢端图均表明,波动具有右旋偏振特征,在算例1(β=0.5)中矢端图为右旋椭圆偏振,而在算例2(β=2.5)和算例3(β=6.5)中矢端图变成复杂的右旋偏振图形,这些均为哨声波的典型特征.本文的研究为快速磁重联与哨声波之间提供了一种可能的联系.      

叶尖间隙对失速颤振影响的实验研究

本文介绍了在跨音压气机试验台上,对BF-1系列转子在两种不同的叶尖间隙(δ_1=1.6,δ_2=0.5mm)下进行颤振实验的情况。文中对实验结果进行了初步分析。实验结果表明,对δ=0.5mm的叶尖间隙,由于二次流损失减少,气流激振能量增加,使叶片失速颤振区的范围扩大,颤振边界前移。     

谱约束之下的矩阵逼近问题

在对一个线性系统进行观测或复原时,出于资料不全或对照资料进行核检等理由,曾提出过如下的数学问题: 根据对未知矩阵A的n~2个元素(?)_(ij)的观测(?)_(ij)以及理论或设计上对A的谱要求:A具有k个特征值λ_1,λ_2,……,λ_k及相应的特征向量X_1,X_2,……,X_k,如何对A作出某种意义下的最佳估计? 显然,据观测数据(?)_(ij)和先验的概率统计信息,可对A进行估计。设所得到的初步估计为(?)。但(?)未必能满足对A的谱要求,所以(?)未必是问题的解。因而我们考虑这样的一个问题:在所有满足谱约束的n阶方阵中,选取与(?)最“接近”的矩阵,以作为A的最佳估计。本文给出了A的最佳估计的存在性与唯一性,以及最佳估计的具体求法,最后用一个简单的算例来说明之。这里假定(?)已据现有的概率统计方法求得。     

地球磁鞘中磁场起伏特性的分布

本文利用行星际起伏通过激波后的变化的MHD模型, 具体讨论了地球磁鞘中磁场起伏特性在黄道面内的分布.主要结果是:(1)行星际磁场起伏的强度和各向异性在磁鞘中被显著放大;(2)行星际磁场基本位于黄道面内时, 磁鞘中磁场起伏特性(强度、相对起伏和各向异性等)呈现明显的晨一昏不对称性, 早晨侧(准平行激波)显著地高于黄昏侧(准垂直激波);(3)行星际磁场方向对磁场起伏特性在磁鞘中的分布有强烈的控制作用, 早晨侧响应灵敏, 黄昏侧反响不大.相对地讲, 黄昏侧的磁活动较之早晨侧稳定;(4)行星际磁场转南的增强将导致磁鞘中磁场起伏的最大区域自黄道面低纬向北极高纬移动, 南-北不对称性磁活动随之加强, 最强大致出现在磁场与黄道面相交成大约45°时, 而晨-昏不对称性的强弱程度则发生相反变化;(5)行星际磁场的相对起伏增加, 晨-昏不对称性反随之减弱.磁鞘中磁场起伏分布的特性与卫星观测大体符合, 是磁顶、边界层某些晨-管不对称性出现的可能起因之一.      

高T_cBi－Pb－Sr－Cu－Ca－O系氧化物超导材料的Meissner效应和磁屏蔽效应

对高ＴｃＢｉ－Ｐｂ－ｓｒ－Ｃｕ－Ｃａ－Ｏ系氧化物超导材料的多晶块状、多晶粉末状和单晶等三种样品的Ｍｅｉｓｓｎｅｒ效应和磁屏蔽效应进行了仔细测量和分析．块状样品具有较强的磁屏蔽能力，在ＺＦＣ（Ｚｅｒｏ－ＦｉｅｌｄＣｏｏｌｅｄ）和ＦＣ（ＦｉｅｉｄＣｏｏｌｅｄ）两种过程中，超导体的体积比之差最大约１０％左右（μ０Ｈ≈２００Ｘ１０－４Ｔ）；粉末样品和单晶样品的磁屏蔽能力很小（７７Ｋ）．     

Monte Carlo calibration of the response of the University of Chicago’s Cosmic Ray Nuclei Experiment (CRNE) on IMP-8 to electrons above 0.5 MeV

Modern instrument-simulation techniques offer the possibility of increasing the scientific yield from archival space datasets. In this paper, we report on a simulation of the electron response of the University of Chicago’s Cosmic Ray Nuclei Experiment (CRNE) instrument on the IMP-8 satellite. IMP-8/CRNE returned data from 1973 to 2006. The CRNE particle telescope was designed to measure the isotopic composition of Galactic cosmic-ray (GCR) nuclei and has also been used in many studies of protons and ions above 10 MeV/nucleon from solar energetic particle (SEP) events. But CRNE also functions as a highly-capable detector for solar electrons above 0.5 MeV, an energy range that has not been extensively studied. Utilization of the CRNE electron data has heretofore been limited by the fact that CRNE was never calibrated for electrons. We have therefore used the GEANT4 Monte Carlo simulation package to model the CRNE response to electrons and (separately) protons for multiple energies and incident angles. The results were used to compute the energy- and angle-dependence of the effective area and the energy-dependence of the geometric factor. The response to protons, which was already well understood, was used to verify the mass model, the simulation settings, and the post-processing software. Our simulation of the IMP-8/CRNE electron response now allows analysis of hundreds of relativistic solar electron events observed by CRNE over the years, including studies of evolution of electron energy spectra with high time resolution. We show examples of these results and briefly discuss potential applications to future scientific investigations.     

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．     

Multiwavelength spectral models for SNR G347.3-0.5 from non-linear shock acceleration

The remnant G347.3-0.5 exhibits strong shell emission in the radio and X-ray bands, and has a purported detection in the TeV gamma-ray band by the CANGAROO-II telescope. The CANGAROO results were touted as evidence for the production of cosmic ray ions, a claim that has proven controversial due to constraining fluxes associated with a proximate unidentified EGRET source 3EG J1714-3857. HESS has now seen this source in the TeV band. The complex environment of the remnant renders modeling of its broadband spectrum sensitive to assumptions concerning the nature and parameters of the circumremnant medium. This paper explores a sampling of reasonable possibilities for multiwavelength spectral predictions from this source, using a non-linear model of diffusive particle acceleration at the shocked shell. The magnetic field strength, shell size and degree of particle cross-field diffusion act as variables to which the radio to X-ray to gamma-ray signal is sensitive. The modeling of the extant data constrains these variables, and the potential impact of the recent HESS detection on such parameters is addressed. Putative pion decay signals in hard gamma-rays resulting from hadronic interactions in dense molecular clouds are briefly discussed; the requisite suppression of the GeV component needed to accommodate the 3EG J1714-3857 EGRET data provides potential bounds on the diffusive distance from the shell to the proximate clouds.     

我国首批0.5米级商业高分辨率遥感卫星高景－1年底发射

2016年,中国航天发射进入了高峰期,完成了不少重大航天任务。时至年末收官之际,中国航天的热度仍未消退,又相继发射多颗影响力较大的卫星。12月下旬,我国即将以“一箭双星”方式发射首批具有全球竞争力的商业遥感卫星高景－1;另外,我国还将发射“全球二氧化碳监测科学试验卫星”,进一步发展我国温室气体监测能力。此前的11月22日,我国中继卫星系统又添一颗天链－1的04星,该星堪与世界一流卫星比肩;12月11日,我国成功发射了具有国际先进水平的首颗第二代静止气象卫星风云－4;还有,9月发射的天宫－2空间实验室上的14项科学与应用任务已取得初步成果。借此契机,本刊特推出中国航天专题,以飨读者。     

非晶态铁硼薄膜的平面霍耳效应

对于用射频溅射法制得的Fe_(83)B_(17)薄膜进行了平面霍耳效应的研究。实验表明:厚度大于800(?)的薄膜测量结果与导出的公式符合良好,且平面霍耳电压V_H的磁滞回线有轴对称性,但对较薄的膜则出现对公式的偏离并失去对称性。V_H的幅值可达500μV,开关临界磁场为22×10~(-4)T,晶化以后薄膜的V_H减小约一个数量级。利用平面霍耳效应测量了薄膜的静态磁特性。     

A Far Infrared Photometer (FIRP) for the Infrared Telescope in Space (IRTS)

We describe the design and calibration of the Far-Infrared Photometer (FIRP), one of four focal plane instruments on the Infrared Telescope in Space (IRTS). The FIRP will provide absolute photometry in four bands centered at 150, 250, 400, and 700 μm with spectral resolution λ/Δλ ≈ 3 and spatial resolution ΔΘ = 0.5 degrees. High sensitivity is achieved by using bolometric detectors operated at 300 mK in an AC bridge circuit. The closed-cycle ³He refrigerator can be recycled in orbit. A 2 K shutter provides a zero reference for each field of view. More than 10% of the sky will be surveyed during the ≈3 week mission lifetime with a sensitivity of <10⁻¹³ W·cm⁻²·sr⁻¹ per 0.5 degree pixel.     

Global Environmental Alert Service (GEAS)

Early warning systems represent an innovative and effective approach to mitigate the risk associated with natural hazards. Early warning technologies are now available for almost all natural hazards and systems are already in operation in all parts of the world. Nevertheless, recent disasters such as the Indian Ocean tsunami in 2004 and Katrina hurricane in 2005, highlighted inadequacies in early warning technologies.

Efforts towards the development of a global warning system are necessary for turning the tide in early warning processes and technologies. There is a pressing need for a globally comprehensive early warning system based on existing systems. The global system should be a mechanism which can consolidate scientific information and evidences, package this knowledge in a form usable to international and national decision makers and actively disseminate this information to those users.

The proposed Global Environmental Alert Service (GEAS) will provide information emanating from monitoring, Earth observing and early warning systems to users in a near-real-time mode and bridge the gap between the scientific community and policy makers. Characteristics and operational aspects of such a service, GEAS, are discussed.