共查询到19条相似文献,搜索用时 234 毫秒
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提出了采用多根对称分布载流导线构成原子分束器的方法,包括三导线和四导线磁导引。阐述了原子分束器的分束机制,用Ansoft Maxwell 2D软件计算给出了部分载流导线移动到不同位置时的磁场分布图。通过分析了导引中心的变化,发现只要通过改变载流导线之间的相对位置就可以来实现从单路到双路导引和三路导引的转换。由此分别设计由3根对称分布载流导线构成的原子双路分束器和4根对称分布载流导线构成三路分束器,然后运用Monte Carlo方法模拟验证其原子分束功能。最后以三线对称分布分束器为基础构成Mach-Zehnder原子磁干涉仪。 相似文献
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为了研究冷原子在磁导引中的运动规律,设计优化导体结构、电流和偏置磁场,本文根据毕奥-萨伐尔定律计算理想化导体的常规数值解,并由Matlab和VC混合编程设计出导线磁场计算工具;根据麦克斯韦方程组选择Ansoft MaxweU计算宽导线、复杂结构导体、通交变电流等情况的有限元数值解.取宽度为100μm,高度为10μm的宽... 相似文献
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在空间探测过程中,采用高灵敏无自旋交换弛豫(SERF)原子磁强计在行星表面进行磁场测量是原位物质成分分析的有效手段之一。为了提高SERF原子磁强计的磁场测量灵敏度,必须减小外界磁场扰动对其原子自旋SERF态质量的影响,基于SERF原子磁强计的测量原理,设计了一套主动磁补偿系统。首先,通过测量驱动激光光强获得3个方向的磁场信息;在此基础上,控制电流源和线圈主动产生一个与外界磁场扰动大小相同、方向相反的磁场来补偿扰动,以提高原子自旋SERF态的质量;最后,结合现有的SERF原子磁强计实验平台进行了实验验证。实验结果表明,与手动补偿方式相比,采用本文所述的主动磁补偿系统,可以实时跟踪磁场补偿点,降低系统信号的噪声,补偿了外界磁场的扰动,验证了磁强计主动磁补偿技术的有效性,为后续样机的研制奠定了技术基础。 相似文献
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目前,对原子气室内自旋极化率的空间操控与测量已有不少研究,但是对这类研究缺乏系统的分析、整理和综述。通过对文献的梳理,将现有的操控与测量方法分为三类,即光操控/磁测量方法、磁操控/光测量方法和光操控/光测量方法。分别对这三类方法进行了叙述,尤其是对笔者所在小组提出和研究的光操控/光测量方法进行了详细的介绍。该方法采用时空双重调制技术和正交隔离技术,实现了13.7μm线宽的自旋极化率空间操控与测量。此结果不仅远小于之前毫米量级的空间分辨率,而且突破了无扩散干扰距离的限制。基于上述实验进展,对原子气室内自旋极化率操控与测量的空间分辨率理论极限进行了初步分析。 相似文献
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相较于传统线圈,原子磁强计作为低频电磁波通信信号磁传感接收器具有体积小、灵敏度高的优势。基于射频-光双共振原理实现原子的宏观极化和相干进动,并通过探测磁矩横向分量来获得待测磁场信息,最终实现一台灵敏度500 fT/Hz1/2@1~5 Hz,响应带宽3.5 kHz的原子磁强计。并利用该原子磁强计作为磁传感器对频率200 Hz、磁场分量幅度10 nT的电磁波开展了通过探测磁场分量接收通信信号的实验,实现码率200/s的电磁波通信信号的接收,验证了该磁强计作为接收机接收低频电磁波通信信号的能力。 相似文献
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磁光阱是一种冷却陷俘原子的装置,磁光阱实验参数的优化是冷原子实验中基础且重要的工作,人工手动优化参数需耗费大量时间,且很难确保最终参数是全局最优的。基于贝叶斯优化的机器学习方法是一种对目标表达式未知、非凸、多峰的量子物理系统进行参数优化的有效方案,该过程通常远快于人工手动调节,且有更大概率找到全局最优值。提出了一种基于贝叶斯优化方法的冷原子多参数自主实时优化实验方案,该方案通过成本函数构造、控制程序编写、贝叶斯算法优化等形成一个可自主优化的闭环系统。实验结果表明,经过约30 min的迭代优化,所提方案可有效完成磁光阱系统的多参数优化,并得到最优的实验结果;所提方案验证了贝叶斯优化方法在多参数物理系统中应用的可行性,通过改进成本函数,还可应用于其他的复杂多参数实验物理系统最优参数快速确定。 相似文献
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冷原子干涉陀螺仪是下一代超高精度陀螺仪的重要发展方向,有望在新一代惯性导航技术中开辟全新的技术途径.冷原子干涉陀螺仪在高性能武器和深空探测等领域有广泛的应用前景,首要应用方向是最高价值的战略级大型武器平台,包括弹道导弹、战略核潜艇、远程战略轰炸机等.围绕冷原子干涉陀螺仪的相关技术进行专利分析研究,包括技术分布、申请趋势、申请区域和重点申请人分析,旨在了解该技术领域的技术发展现状和分布情况,并通过对重点专利的解读,预测该技术的发展趋势,并对我国冷原子干涉陀螺仪技术的发展提出建议. 相似文献
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R. Lundin D. Winningham S. Barabash R. Frahm D. Brain H. Nilsson M. Holmström M. Yamauchi J. R. Sharber J.-A. Sauvaud A. Fedorov K. Asamura H. Hayakawa A. J. Coates Y. Soobiah C. Curtis K. C. Hsieh M. Grande H. Koskinen E. Kallio J. Kozyra J. Woch M. Fraenz J. Luhmann S. Mckenna-Lawler S. Orsini P. Brandt P. Wurz 《Space Science Reviews》2006,126(1-4):333-354
Aurora is caused by the precipitation of energetic particles into a planetary atmosphere, the light intensity being roughly proportional to the precipitating particle energy flux. From auroral research in the terrestrial magnetosphere it is known that bright auroral displays, discrete aurora, result from an enhanced energy deposition caused by downward accelerated electrons. The process is commonly referred to as the auroral acceleration process. Discrete aurora is the visual manifestation of the structuring inherent in a highly magnetized plasma. A strong magnetic field limits the transverse (to the magnetic field) mobility of charged particles, effectively guiding the particle energy flux along magnetic field lines. The typical, slanted arc structure of the Earth’s discrete aurora not only visualizes the inclination of the Earth’s magnetic field, but also illustrates the confinement of the auroral acceleration process. The terrestrial magnetic field guides and confines the acceleration processes such that the preferred acceleration of particles is frequently along the magnetic field lines. Field-aligned plasma acceleration is therefore also the signature of strongly magnetized plasma. This paper discusses plasma acceleration characteristics in the night-side cavity of Mars. The acceleration is typical for strongly magnetized plasmas – field-aligned acceleration of ions and electrons. The observations map to regions at Mars of what appears to be sufficient magnetization to support magnetic field-aligned plasma acceleration – the localized crustal magnetizations at Mars (Acuña et al., 1999). Our findings are based on data from the ASPERA-3 experiment on ESA’s Mars Express, covering 57 orbits traversing the night-side/eclipse of Mars. There are indeed strong similarities between Mars and the Earth regarding the accelerated electron and ion distributions. Specifically acceleration above Mars near local midnight and acceleration above discrete aurora at the Earth – characterized by nearly monoenergetic downgoing electrons in conjunction with nearly monoenergetic upgoing ions. We describe a number of characteristic features in the accelerated plasma: The “inverted V” energy-time distribution, beam vs temperature distribution, altitude distribution, local time distribution and connection with magnetic anomalies. We also compute the electron energy flux and find that the energy flux is sufficient to cause weak to medium strong (up to several tens of kR 557.7 nm emissions) aurora at Mars. Monoenergetic counterstreaming accelerated ions and electrons is the signature of field-aligned electric currents and electric field acceleration. The topic is reasonably well understood in terrestrial magnetospheric physics, although some controversy still remains on details and the cause-effect relationships. We present a potential cause-effect relationship leading to auroral plasma acceleration in the nightside cavity of Mars – the downward acceleration of electrons supposedly manifesting itself as discrete aurora above Mars. 相似文献
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Qiucheng YANG Cheng CHENG Ali Abd EL-ATY Chunmei LIU Shenghan HU Yao QIN Tao LI Cong WU Yong XU Xunzhong GUO 《中国航空学报》2022,35(1):226-237
This study aims at investigating the impact of using the Magnetorheological Elastomers(MREs) medium to improve the formability of T-shaped Inconel 718 tubes during the bulging process. Besides, the influence of the punch size and the intensity of the magnetic field on the branch height and wall thickness distribution of the T-shaped Inconel 718 tubes are also explored. The results showed that the parts formed by the punch with a length of 5 mm in the pressurization zone have better forming quali... 相似文献
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Maxim L. Khodachenko Valerii V. Zaitsev Albert G. Kislyakov Alexander V. Stepanov 《Space Science Reviews》2009,149(1-4):83-117
Coronal loops, which trace closed magnetic field lines, are the primary structural elements of the solar atmosphere. Complex dynamics of solar coronal magnetic loops, together with action of possible subphotospheric dynamo mechanisms, turn the majority of the coronal loops into current-carrying structures. In that connection none of the loops can be considered as isolated from the surroundings. The current-carrying loops moving relative to each other interact via the magnetic field and currents. One of the ways to take into account this interaction consists in application of the equivalent electric circuit models of coronal loops. According to these models, each loop is considered as an equivalent electric LCR-circuit with variable inductive coefficients L, capacitance C, and resistance R, which depend on shape, scale, position of the loop with respect to neighbouring loops, as well as on the plasma parameters in the magnetic tube. Such an approach enables to describe the process of electric current dynamics in the groups of coronal loops, as well as the related dynamical, energy release and radiation processes. In the present paper we describe the major principles of LCR-circuit models of coronal magnetic loops, and show their application for interpretation of the observed oscillatory phenomena in the loops and in the related radiation. 相似文献
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光磁共振测量地磁场的改进方法 总被引:3,自引:0,他引:3
根据光磁共振原理,通过光抽运,形成原子的能级分布偏极化,再加入射频信号打破塞曼能级偏极化分布,形成并输出光磁共振信号。然后,同时改变扫场和水平磁场方向,调节水平电流大小,再次获得光磁共振信号。根据2次测得的水平亥姆霍兹线圈电流,计算等效磁感强度。由仪器的垂直电流,计算地磁场垂直分量。二者合成,即可得出当地磁感强度。改进后,此方法克服了以往先测定朗德因子再测定地磁场的缺点。 相似文献