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（Fe0.5Ni0.5）80—xCrxP14B6合金薄带的磁谱的研究

以阻抗电桥法对非晶态(Fe_(0.5)Ni_(0.5))_(80-z)Cr_zP_(14)B_6(x=0,1,2,3,4,6,10)合金薄带的淬态和等温退火后样品的磁谱进行了测量。结果表明:退火后相对起始磁导宰μ_(?)提高了3.6～6倍,截止频率f_c下降,磁损耗μ_2的磁谱出现了共振峰。同时,等温退火处理对各样品相对起始磁导率的影响比改变Cr元素含量x要大得多。     

D_(st)指数和AE指数的相关关系

本文对1972年7月至1974年12月的D~(st)指数和AE指数(时均值)作了初步的统计分析。每半年的资料所得到的相关系数在0.5到0.6之间。当地磁场扰动程度增大时,即D~(st)指数的值减小时,相关系数的值减小。因为D~(st)指数主要反映赤道环电流的强度,AE指数主要反映极光带电急流的强度,因此这两个指数间的关系有可能反映这两个电流体系之间的关系。行星际磁场的南北分量Bz对这种关系没有明显的影响。     

非晶态Co-T-Zr(T=Cr,Mo,V,W)合金作为磁强计磁芯材料的研究

以快淬法制备了非晶态Co_(90～x)T_xZr_(10)(T=Cr,Mo,V,W;x=0,4,6,8,10,12)合金系列样品,并对其一些热和磁性能进行了测试研究,探讨了它们在磁强计上应用的可能性。结果表明,随着样品中T元素含量的增加,样品的晶化温度和晶化激活能升高,饱和磁化强度和居里温度下降,交流磁导率变化不大。退火处理对交流磁导率和损耗有较大影响。以现有理论对实验结果进行了分析。非晶态Co_(78)Cr_(12)Zr_(10)合金适于用作磁强计探头的磁芯材料,尤其是它良好的高频性能使磁强计测量的交流磁场的截止频率大干20kHz。     

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．     

电阻磁流体力学模拟的CESE方法

利用时空守恒元解元方法(CESE)和两种改进方法, 即库朗数不敏感(CNIS)方法与高阶CESE方法求解2.5维电阻磁流体力学(resistive MHD)方程组, 模拟了两个单电流片重联问题. 并考察了上述三种方法所得结果的磁场散度. 分析表明, 三种方法所得到的磁场位形基本没有差别, 但在磁场散度上存在一定差异, 相比另外两种方法, CNIS方法在控制磁场散度方面表现得更好.      

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。     

太阳活动高年期间(1978—1981)耀斑-行星际激波传播的三维平均特性——日本行星际闪烁(IPS)观测的初步分析

文中通过对行星际激波传播的动力学效应的考虑,根据日本的IPS观测资料,对太阳活动高年期间85个耀斑-IPS激波事件进行了统计研究.结果表明:(1)激波的传播相对耀斑法线方向是非对称传播.传播最快的方向,就经度而言趋向行星际螺旋形磁场方向;就纬度而言很接近在此事件期间日球电流片的平均纬度.(2)传播的纬度范围(-60°— +40°)远比传播的经度范围(<—90°—+90°)小.(3)激波的能量分布有明显的东-西、南-北不对称性,它决定了激波传播的非对称特性.所研究的85个耀斑-激波的平均能量～2.7×1031尔格(单位立体角).上述结果与我们分析美国圣地亚哥IPS观测所得结果基本一致[3].      

日本"月女神"探测器的有效载荷(下)

6 月球磁强计(LMAG)和等离子体能量角与成分实验(PACE) 利用LMAG和PACE可以对目前和远古时期月球周围的磁场和等离子体环境及其演变进行研究.     

磁层顶的Kelvin-Helmholtz不稳定性(Ⅳ)可压缩不稳定波的若干特性

本文讨论了磁层顶可压缩K-H不稳定波的若干特性,包括磁场扰动和密度扰动的位相关系,扰动磁场的偏振特性,时间增长率的午前午后非对称性,空间增长率及磁层脉动的地方时效应和K-H不稳定波对IMF的响应。分析表明,上述诸特性对于了解磁层边界区MHD波的起源和K-H不稳定性同地磁脉动的关系十分重要。      

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.     

基于多用表磁感应开关测量方法研究

研究了磁感应开关的工作原理及其电气性能,提出了一种基于多用表磁感应开关电气性能测量方法,实现磁感应开关在空载和加载条件下性能指标的测量。试验验证表明,基于多用表方法能够对磁感应开关电气性能进行有效的测量,测量结果不确定度满足磁感应开关产品规范的要求。     

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.      

Modified gradiometer technique applied to Double Star (TC-1)

On TC-1 (Tan Ce 1), the equatorial spacecraft of the Double Star mission, a strong spin-synchronized magnetic interference from the solar panels was observed. In-flight correction techniques for spinning spacecraft that are based on minimizing spin tones in the spin-aligned component and in the magnitude of the ambient magnetic field are therefore not possible in this case. However, due to the fortunate situation that the spacecraft carries two flux-gate magnetometers on the same boom (at 0.5 m distance from each other), the spacecraft field effects could be removed from the spin-averaged data to achieve 0.2 nT relative accuracy, by using a gradiometer technique. Methodology and results are presented. The obtained accuracy allows the use of the data in multi-spacecraft studies together with the Cluster satellites.     

微阴极电弧推力器磁路设计

微阴极电弧推力器是一种利用真空条件下放电电弧烧蚀阴极材料产生较高电离度的高速等离子体,并在外加磁场作用下喷出以产生推力的微型电推力器。微阴极电弧推力器磁场设计是推力器设计中的重要工作之一,将影响推力器工作稳定性和工作性能。分别采用多匝通电螺线管计算公式、二维和三维数值仿真完成磁路设计,磁感应强度随线圈电流和线圈匝数增加而变大;当线圈电流15A、线圈匝数为600匝时,放电通道中心线磁感应强度最大值超过0.3T;采用特斯拉计测量磁感应强度,仿真结果与测量结果吻合较好。最后采用时间飞行法（TOF）测得等离子体速度随磁场增强而增加。     

利用Cluster卫星磁尾单事例研究具有复杂核心磁场结构的磁通量绳

2002年8月28日09:50UT-10:50UT,Cluster卫星在地球磁尾观测到一次导向场磁场重联事件.卫星观测到磁场重联扩散区附近清晰的霍尔（Hall）四极型磁结构.由于导向场的存在,该四极型结构被扭曲变形.在该磁场重联事件中,卫星观测到多个磁通量绳,大部分磁通量绳的核心场极性与导向场极性一致.但是,其中一例磁通量绳的核心场结构极性较复杂.该例磁通量绳中心区域核心场强度出现峰值,核心场极性和导向场极性一致;中心以外区域的核心场极性和导向场极性相反.这种复杂核心场结构以前未见报道.通过最小方向导数法,发现该磁通量绳的轴向是弯曲的.C1和C3卫星穿越了磁通量绳弯曲部分,探测到核心场极性变化;C2和C4卫星位于C1和C3卫星的北侧,仅穿越了磁通量绳弯曲处的一部分,故核心场具有单极性.      

Modeling the (upper) solar atmosphere including the magnetic field

The atmosphere of the Sun is highly structured and dynamic in nature. From the photosphere and chromosphere into the transition region and the corona plasma-β changes from above to below one, i.e., while in the lower atmosphere the energy density of the plasma dominates, in the upper atmosphere the magnetic field plays the governing role – one might speak of a “magnetic transition”. Therefore the dynamics of the overshooting convection in the photosphere, the granulation, is shuffling the magnetic field around in the photosphere. This leads not only to a (re-)structuring of the magnetic field in the upper atmosphere, but induces also the dynamic reaction of the coronal plasma, e.g., due to reconnection events. Therefore the (complex) structure and the interaction of various magnetic patches is crucial to understand the structure, dynamics and heating of coronal plasma as well as its acceleration into the solar wind.

The present article will emphasize the need for three-dimensional modeling accounting for the complexity of the solar atmosphere to understand these processes. Some advances on 3D modeling of the upper solar atmosphere in magnetically closed as well as open regions will be presented together with diagnostic tools to compare these models to observations. This highlights the recent success of these models which in many respects closely match the observations.     

铁磁流体润滑中的非牛顿流影响

利用外加磁场可以直接调节铁磁流体润滑膜的承载能力,因为在外磁场中铁磁流体的粘度增大. 实验研究表明,铁磁流体是一种非牛顿流体,它同时表现出Bingham塑性体和拟塑性体的特性. 铁磁流体的非牛顿流体行为受外磁场强度和方向的影响. 铁磁流体的本构方程可以表示为 τ(H,D)=τs(H)+η₁(H)D+η₂(H)D2.由于铁磁流体具有屈服剪应力τs(H),而可能出现"固态"核粘附于轴承表面上.铁磁流体的拟塑性体行为对核的生成条件有影响.在铁磁流体润滑的轴承中,纯剪切流截面C₀不同于普通Bingham塑性体润滑的轴承.作为一个实际的例子而给出铁磁流体润滑平板滑块的承载能力和摩擦力的解.      

Neutral atmosphere and crustal magnetization as factors determining differences in plasma convection and magnetic fields distribution in the ionospheres of Mars and Venus

The pattern of the magnetic field/plasma convection can be, to some extent, recovered from the magnetic field measurements by employing either theoretical or numerical models. We use the MAG/ER day-time measurements of the magnetic field at the altitudes from 90 to 180 km during the elliptical orbits of MGS. Analysis of the altitude variation of the characteristics of the large-scale magnetic fields, which were measured some distance away from strong crustal magnetic anomalies, is summarized. The low density of the Martian atmosphere together with the crustal magnetization result in critical differences in plasma convection which are followed by remarkable differences of the magnetic field features within the ionosphere of Venus and Mars (even in its northern hemisphere where the crustal magnetization is, on the average, low) and distribution of currents.