全张量磁梯度数据的斜导数特征值边界识别方法研究   总被引：1，自引：0，他引：1       下载免费PDF全文

郭华  韩松  郑强  梁韧  段然  刘浩军  李西子 《地球物理学报》2019,62(9):3580-3590

本文提出了一种全张量磁梯度数据的斜导数边界识别方法，该方法利用全张量磁梯度数据定义了北向斜导数、东向斜导数和垂向斜导数.模型试验表明，北向和东向斜导数无法有效识别磁性异常体边界，异常形态复杂虚假异常较多，而垂向斜导数在高纬度斜磁化或者垂直磁化条件下可以清晰而准确得识别地质体的边界，具有一定的深度识别能力.与现有磁张量梯度的边界识别方法相比，识别效果好，可以有效均衡不同深度地质体的响应.将上述方法应用于大兴安岭地区实测航磁三分量数据转换得到的全张量数据，获得了研究区浅部磁性体的分布，并与三分量数据进行联合解释，取得良好的地质效果.  相似文献   

重庆红池坝地电场变化分析     

董蕾  龚丽文 《大地测量与地球动力学》2018,38(9):986-990

利用磁静日时序叠加方法和FFT频谱分析方法对红池坝地电场观测资料进行逐月处理，并与巫山建坪台地磁观测资料进行对比，分析红池坝地电场静日变化特征；计算红池坝台站磁暴期间产生的感应电场，与地电场观测数据对比，分析地电暴的特征。结果表明，静日随着月份的变化，相位发生变化，与巫山建坪地磁Sq变化一致；1月、2月、11月、12月的地电场日变幅明显小于其他月份；地电场显著周期成分与磁静日地磁场相同，并且通过周期成分的逐月对比分析得到，地电场与地磁D分量的不同周期成分的频谱值随时间的变化基本一致；某一方向的地电暴与该垂直方向的磁暴和该地区的电性结构有关；地电暴观测值与地磁感应电流计算值呈线性关系；地电暴变化与K值呈指数关系。  相似文献   

浑河断裂地球物理场特征及地震活动性     

张鐘月  万波  彭虎  田德欣 《世界地质》2020,39(1):176-184

浑河断裂是辽宁省内一条重要的北东向地震构造带,断裂两侧的地球物理重磁场存在差异。通过浑河断裂的区域重力场与磁场研究,认为浑河断裂既控制了深、浅部岩石地层的发育,同时浑河断裂的重力场、磁场分布随着深、浅部地层岩性发育的差异而有所变化。浑河断裂的重力场和磁场梯度带主要位于抚顺以西至沈阳一带,浑河断裂历史以来有记录的最大破坏性地震位于重力梯度变化较大的沈阳段。综合浑河断裂地球物理场特征及区域地质资料,浑河断裂虽然活动性一般,但抚顺地区的采煤活动对断裂的活动性有一定影响。近些年抚顺地区频发的沉降、滑坡和地裂缝等地质灾害应当引起对浑河断裂活动性研究的重视。  相似文献   

重磁处理解释系统软件设计与关键实现技术          下载免费PDF全文

郑元满  姚长利  李泽林  刘强 《地球物理学报》2019,62(10):3744-3759

重磁探测是金属矿勘探的主要手段之一，其处理和解释方法技术已得到很大的发展，研发与其相适应的重磁软件是重要的研究课题.在国家863课题的支持下，我们设计并研发了重磁处理解释集成化软件系统.在分析国内外现有软件不足的基础上，我们对重磁软件系统所应具有的操作行为进行了针对性的设计，提出了具有特色的功能设计思路，并进行了针对性的研发实现.为满足深部矿产资源勘探需求和精细化解释需要，提出了更加具有针对性的软件设计解决方案，研发了特色的处理解释模块，核心突出软件的实时可视化和协同交互操作，使软件系统能高效地服务于使用者的目标任务.在优化改进处理、正反演算法的基础上，提出多核并行化方案并实现，提高了软件整体运行速度.最终形成了将数据管理、数据可视化、数据处理及解释有机结合的特色软件系统，为金属矿探测提供了一个高效、有力的工具.  相似文献   

基于手机位置数据的四川九寨沟7.0级地震人流分析     

李东平  黄乐  陈海鹏  刘倩倩 《中国地震》2017,33(4):602-612

2017年8月8日四川九寨沟7.0级震后,浙江省地震局利用大数据采集了1031.99万条手机位置记录和4.46万个空间格网位置。本文结合24hr连续定位的手机数据,使用手机位置数据分别对九寨沟灾区人口从时间和地理维度上进行了量化分析,估计了多维人口分布的偏差,同时,探讨了剔除微观误差数据用户来估算灾区通讯基站退服分布的方法。该项工作为震后快速获取灾区人口实时动态分布提供了有效途径,同时也为地震灾害评估提供了较准确的依据。  相似文献   

Effect of superstrong magnetic field on electron screening at the crusts of neutron stars     

刘晶晶 《海洋学报(英文版)》2010,29(9)

The influences of electron screening (ES) and electron energy correction (EEC) are investigated by superstrong magnetic field (SMF). We also discuss in detail the discrepant factor between our results and those of Fushiki, Gudmundsson and Pethick (FGP) in SMF. The results show that SMF has only a slight effect on ES when B < 10⁹ T on the surfaces of most neutron stars. Whereas for some magnetars, SMF influence ES greatly when B > 10⁹ T . For instance, due to SMF the ES potential may be increased about 23.6% and the EEC may be increased about 4 orders of magnitude at ρ/μ_e = 1.0×10⁶ mol/cm³ and T₉ = 1. On the other hand, the discrepant factor shows that our results are in good agreement with FGP's when B < 10⁹ T . But the difference will be increased with increasing SMF.  相似文献   

煤层瓦斯富集区核磁共振探测技术研究     

童雪瑞  姜志海  刘树才  李毛飞  王文闯 《地质论评》2024,70(S1):141-142

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What SDO tells us about structure and evolution of coronal bright points     

N. V. Karachik  E. Minenko  I. Sattarov  A. A. Pevtsov  C. T. Sherdonov 《Astronomische Nachrichten》2014,335(10):1037-1042

Using magnetograms and coronal images from two instruments on board the Solar Dynamics Observatory (SDO), we study structure and evolution of a limited number of coronal bright points (CBPs). Our results show that the relation between CBPs and their magnetic footpoints is not simple. In some cases, CBP may appear as a bright portion of a larger loop (with clearly identifiable footpoints), and in some cases, an isolated CBP may develop between magnetic poles, which might not be the closest ones to each other or which might not be involved in the magnetic flux cancellation. We suggest that the magnetic connectivity responsible for formation of isolated coronal bright points is governed by the orientation of the large‐scale magnetic field. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

Ultraviolet spectroscopic study of EU UMa and ST LMi from HST and IUE observations     

《New Astronomy》2015

We present the first orbit-resolved ultraviolet spectroscopic observations of the two polar systems EU UMa and ST LMi obtained with the Hubble Space Telescope Faint Object Spectrograph (HST FOS) and International Ultraviolet Explorer (IUE) during their intermediate- and low-luminosity states in the period between 1982 and 2003. Different line profiles of the two systems showing variations of line fluxes at different orbital phases are presented. This paper focuses on the C IV emission line at 1550 Å produced in the accretion stream, presenting calculations of spectral line fluxes, ultraviolet luminosities, and accretion rates for the two systems. Our analysis of the spectroscopic data reveals changes with orbital phase of the emission line profiles that correspond to the light curve variations of both EU UMa and ST LMi in the optical and infrared bands. The variations of line fluxes are attributed to variations of both density and temperature as a result of a changing rate of mass transfer from the secondary star to the white dwarf. The ultraviolet luminosity and accretion rate of EU UMa are smaller than the ultraviolet luminosity and accretion rate of ST LMi.  相似文献   

Dynamo saturation in direct simulations of the multi‐phase turbulent interstellar medium     

A. Bendre  O. Gressel  D. Elstner 《Astronomische Nachrichten》2015,336(10):991-1004

The ordered magnetic field observed via polarised synchrotron emission in nearby disc galaxies can be explained by a mean‐field dynamo operating in the diffuse interstellar medium (ISM). Additionally, vertical‐flux initial conditions are potentially able to influence this dynamo via the occurrence of the magnetorotational instability (MRI). We aim to study the influence of various initial field configurations on the saturated state of the mean‐field dynamo. This is motivated by the observation that different saturation behaviour was previously obtained for different supernova rates. We perform direct numerical simulations (DNS) of three‐dimensional local boxes of the vertically stratified, turbulent interstellar medium, employing shearing‐periodic boundary conditions horizontally. Unlike in our previous work, we also impose a vertical seed magnetic field. We run the simulations until the growth of the magnetic energy becomes negligible. We furthermore perform simulations of equivalent 1D dynamo models, with an algebraic quenching mechanism for the dynamo coefficients. We compare the saturation of the magnetic field in the DNS with the algebraic quenching of a mean‐field dynamo. The final magnetic field strength found in the direct simulation is in excellent agreement with a quenched α) dynamo. For supernova rates representative of the Milky Way, field losses via a Galactic wind are likely responsible for saturation. We conclude that the relative strength of the turbulent and regular magnetic fields in spiral galaxies may depend on the galaxy's star formation rate. We propose that a mean field approach with algebraic quenching may serve as a simple sub‐grid scale model for galaxy evolution simulations including a prescribed feedback from magnetic fields. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献