一种用于CPT磁力仪的VCSEL 激光管参数自动调节方法

为了解决手动调节VCSEL激光管运行参数困难的问题,提出了一种用于CPT磁力仪的VCSEL激光管参数自动调节方法.首先,在稳定原子气室温度的基础上,通过步进增加激光管的驱动电流并探测光强,确定扫描电流的范围;其次,在初始工作温度基础上增加激光管温度步进,重复扫描三角波驱动电流,并全范围搜寻吸收峰;当首次读取到吸收峰后,利用调节电流精确锁定在当前工作温度条件下吸收峰对应的电流值,同时微调温度,调整吸收峰到最佳位置;最后,记录当前的激光管工作参数,完成整个VCSEL激光管参数自动调节过程.采用上述方法能够快速实现VCSEL激光管的测试及工作参数的设置,提高了工作效率和整机性能.     

Science objectives of the magnetic field experiment onboard Aditya-L1 spacecraft

The Aditya-L1 is first Indian solar mission scheduled to be placed in a halo orbit around the first Lagrangian point (L1) of Sun-Earth system in the year 2018–19. The approved scientific payloads onboard Aditya-L1 spacecraft includes a Fluxgate Digital Magnetometer (FGM) to measure the local magnetic field which is necessary to supplement the outcome of other scientific experiments onboard. The in-situ vector magnetic field data at L1 is essential for better understanding of the data provided by the particle and plasma analysis experiments, onboard Aditya-L1 mission. Also, the dynamics of Coronal Mass Ejections (CMEs) can be better understood with the help of in-situ magnetic field data at the L1 point region. This data will also serve as crucial input for the short lead-time space weather forecasting models.The proposed FGM is a dual range magnetic sensor on a 6?m long boom mounted on the Sun viewing panel deck and configured to deploy along the negative roll direction of the spacecraft. Two sets of sensors (tri-axial each) are proposed to be mounted, one at the tip of boom (6?m from the spacecraft) and other, midway (3?m from the spacecraft). The main science objective of this experiment is to measure the magnitude and nature of the interplanetary magnetic field (IMF) locally and to study the disturbed magnetic conditions and extreme solar events by detecting the CME from Sun as a transient event. The proposed secondary science objectives are to study the impact of interplanetary structures and shock solar wind interaction on geo-space environment and to detect low frequency plasma waves emanating from the solar corona at L1 point. This will provide a better understanding on how the Sun affects interplanetary space.In this paper, we shall give the main scientific objectives of the magnetic field experiment and brief technical details of the FGM onboard Aditya-1 spacecraft.     

The Cassini Magnetic Field Investigation

The dual technique magnetometer system onboard the Cassini orbiter is described. This instrument consists of vector helium and fluxgate magnetometers with the capability to operate the helium device in a scalar mode. This special mode is used near the planet in order to determine with very high accuracy the interior field of the planet. The orbital mission will lead to a detailed understanding of the Saturn/Titan system including measurements of the planetary magnetosphere, and the interactions of Saturn with the solar wind, of Titan with its environments, and of the icy satellites within the magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

Simultaneous observations of the plasma density on the same field line by the CPMN ground magnetometers and the Cluster satellites

By applying the cross-phase method and the amplitude-ratio method to magnetic field data obtained from two ground stations located close to each other, we can determine the frequency of the field line resonance (FLR), or the field line eigenfrequency, for the field line running through the midpoint of the two stations. From thus identified FLR frequency we can estimate the equatorial plasma mass density (ρ)$(\rho )$ by using the T05s magnetospheric field model [Tsyganenko, N.A., Sitnov, M.I. Modeling the dynamics of the inner magnetosphere during strong geomagnetic storms, J. Geophys. Res. 110, A03208, 2005] and the equation of Singer et al. [Singer, H.J., Southwood, D.J., Walker, R.J., Kivelson, M.G. Alfven wave resonances in a realistic magnetospheric magnetic field geometry, J. Geophys. Res. 86 (A6) 4589–4596, 1981].     

一种Mx构型氦光泵磁力仪的磁共振理论分析与实验验证

从亚稳态氦原子的Liouville方程和Bloch方程出发,研究了基于Mx构型的亚稳态氦原子的光磁双共振过程,建立了光探测磁共振线型的理论模型,并通过实验对幅值信号与相位信号的磁共振线型仿真结果进行验证,实测曲线与理论预测匹配较好。对共振线宽进行了估算,讨论了影响磁力仪工作灵敏度的磁力仪设计参数,这对Mx构型氦光泵磁力仪的研制有重要的指导意义。     

原子磁力仪的空间应用及发展趋势

在太空探索中,磁场测量为很多重要的科学研究提供了数据支撑。空间探测器和磁测卫星均多次采用原子磁力仪作为磁场测量的主载荷,原子磁力仪在空间磁场测量中发挥着不可替代的作用。回顾了用于空间磁场测量的原子磁力仪的发展历程,总结了不同种类原子磁力仪的技术特点,分析了空间应用原子磁力仪载荷的发展趋势。     

恒定弱磁标准装置设计原理

恒定弱磁标准装置是用来复现高稳定度的恒定弱磁场,并对所复现的弱磁场进行精确测量的装置。恒定弱磁标准装置是由线圈系统、光泵地磁补偿系统、恒流源系统、磁场测量系统等组成。装置采用先进的Cs光泵磁强计补偿技术,在线圈系统的工作区中产生高稳定度的恒定弱磁场,磁场波动均方差小于0.1 nT。通过高稳定度恒流源和线圈系统可以复现1~1.105nT的磁场。通过He-Cs光泵磁共振仪、频率计数器及计算机构成的磁场测量系统可以对所复现的弱磁感应强度量值进行精确的测量,标准测量不确定度为0.07~0.1 nT。     

一型国产无人机直升机铯光泵航磁系统补偿方法研究和试验

随着无人机平台的逐渐成熟,近年来无人机广泛应用于航空物探领域。文章设计了一型无人机航磁系统,采用国产铯光泵磁力仪,载机平台为100 kg级汽油动力无人直升机,基于直升机的操作特性研究了不同于固定翼飞机的定点悬停补偿方法。依据《航空磁测技术规范》进行了地面静态噪声测试、磁补偿飞行、动态噪声测试及切割线飞行。结果表明,采用定点悬停的磁补偿方法,系统的磁补偿精度、动态噪声水平及航磁总精度同样能够达到《航空磁测技术规范》要求的一类设备水平,且更易于操作,从而该航磁系统也可应用于大比例尺低飞航磁项目中。     

反馈磁场均匀性对磁通门磁强计的影响分析

针对磁通门传感器的特点, 研究了反馈线圈对磁通门传感器探测数据的影响, 并对比了几种典型结构的传感器. 磁通门传感器要求激励线圈工作在均匀磁场环境下, 非均匀场会引入误差信号. 根据磁通门原理进行了理论推导, 非均匀性会导致反馈原理工作的磁通门传感器线性系数发生变化. 针对应用于空间磁场探测的几种磁通门传感器常见结构, 即分立结构型、亥姆霍兹型和紧凑球面型等, 分析了传感器内部磁场的均匀性及对磁场探测的影响. 经仿真计算分析发现, 紧凑球型传感器的内部均匀性和稳定性优于分立结构传感器, 更有利于空间磁场探测.      

基于磁强计测量的微小卫星轨道姿态 耦合确定方法

针对基于磁强计测量的微小卫星, 提出了基于串并联混合策略的轨道姿态 耦合确定方法。滤波初期,考虑到估计误差较大,采用先地磁场大小测量的轨道确定、 后地磁场矢量测量的姿态确定的串联策略;稳定后,采用基于矢量测量的轨道、姿态同 步确定的并联策略。为降低轨道、姿态确定的相互影响,设计了基于信息的鲁棒Kalman 滤波,通过自动调节增益矩阵处理两个滤波系统间的影响。仿真表明,该方法在提高鲁 棒性的同时,还能适当提高状态估计的精度。