羌塘盆地中央隆起带的重磁场证据及其构造意义

对于羌塘盆地是否存在横贯东西的中央隆起带,目前学术界仍有分歧.本文提供的最新高精度航空重、磁资料证实存在呈东西向贯通羌塘盆地的中央隆起带,并对该带的构造特征进行了精细刻画.隆起带受南北两侧深大断裂控制,其空间跨度（宽度）由西向东逐渐收敛,并被一组近南北向的隐伏断裂系切割、左滑错动.重、磁场资料还显示中央隆起带在双湖东、西两侧存在明显差异：西段基底大规模隆起,基岩深度一般在3~5 km以内,明显浅于南北羌塘坳陷7~15 km的基底埋深;东段基底隆起幅度明显降低,主要表现为潜伏的低隆起,其中双湖—雅曲段基底埋深5~7 km,雅曲—岗尼段基底埋深7~9 km;即中央隆起带基底自西向东"台阶状"降低,隆起的幅度和分布范围受到近南北向断裂控制.构造分层表明,与南羌塘地块相比,北羌塘地块的基底隆起幅度小、稳定性更好.南北羌塘基底地球物理属性的显著差异说明羌塘盆地并不存在统一的前寒武系变质基底,中央隆起带的形成应该与古特提斯洋关闭时形成的混杂岩带有关.     

Galactic Spiral Arms and Dynamo Control Parameters

We discuss the effects of galactic spiral arms on the -coefficient, turbulent diffusivity and turbulent energy density of the interstellar turbulence. We argue that the -coefficient and the dynamo number are larger in the interarm regions, whereas the kinetic energy density of turbulence is larger in the arms; the turbulent magnetic diffusivity can be only weakly affected by the spiral pattern.     

山东省区域地球物理场

山东省各岩石磁性及密度参数基本可分为高、中、低 3类。山东省磁性结晶基底为泰山岩群、荆山群、胶东岩群、胶南岩群。以沂沭断裂带为界 ,山东省区域地球物理场分为鲁东区和鲁西区。鲁东区进一步划分为 3个次级区 ,即北部区、中部区和南部区。鲁西区进一步划分为 5个次级区 ,即鲁北重磁缓变区、鲁西南重高磁高区、中部弧形重磁场区、鲁西中部重低磁高区、鲁中南条带状重磁场区。各区地球物理场由于地质原因各具特点。山东省莫氏面总体呈东浅西深的缓变带 ,在该缓变带的背景上 ,呈周边地区条带状幔隆、中部幔坳的特征。山东省居里面呈近南北向带状分布 ,有德州聊城菏泽隆起带、滨州淄博滕州深坳带、蓬莱海阳千里岩响水隆起带。鲁中隆起北部碰撞带为山东省特殊的构造地带 ,其特征为侵入岩体沿该带断续出现、岩体围岩或岩体内铜及多金属矿化较为普遍、地热田沿该带时有分布、地形上为南部山区和北部平原的分界地带。胶莱盆地内 ,蓼兰—高密缺失莱阳群层位 ;中生代早期 ,盆地东北部与西南部是盆地的沉积中心 ,至晚期盆地中心北移 ,第三纪沉积中心则为平度蓼兰附近 ;盆地较深部位位于诸城凹陷、平度凹陷。胶莱盆地的次级构造单元可划分为 11个 ,七级镇构造带控制了胶莱盆地的成生和发展。山东省岩浆岩通常表     

基于应力腐蚀和腐蚀疲劳的焊缝磁记忆信号分析

为了研究不同腐蚀条件下的焊缝磁记忆特征信号,对20号钢板状焊缝试件进行残余应力腐蚀、35kN恒拉伸应力腐蚀和35kN静载、25kN动载拉拉腐蚀疲劳对比实验,分析焊缝正、反面磁记忆信号的变化规律,获得焊缝腐蚀发展进程中应力腐蚀与腐蚀疲劳各自对应的磁记忆特征信号.结果表明:在应力腐蚀状态下,不同拉伸载荷对应的磁记忆信号特征不同,35kN恒拉伸应力腐蚀与残余应力腐蚀相比,焊缝区磁记忆信号峰峰值及其梯度更大,磁记忆曲线分布的分散度更大;35kN静载、25kN动载拉拉腐蚀疲劳与35kN恒拉伸应力腐蚀相比,焊缝区磁记忆曲线上下波动多,过零点次数多,磁记忆曲线分布的分散度小.这为磁记忆技术在焊缝工程检测的定性与定量分析提供基础数据.     

重庆红池坝地电场变化分析

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。     

铁磁形状记忆合金研究进展与展望（Ⅱ）：本构模型

阐述了铁磁形状记忆合金（Ferromagnetic Shape Memory Alloy,简写为FSMA）本构模型研究的重要性。以时间为顺序,重点介绍了FSMA本构模型研究的发展历程和研究现状。仔细分析了各种FSMA本构模型在理论基础、适用范围、精度以及复杂程度等方面的特点,讨论了各种理论应用于FSMA本构模型的局限性,指出了它们在面向应用时存在的问题。研究表明,由于FSMA兼具磁致形状记忆效应、热弹性形状记忆效应等多种独特性能,使对其本构模型的研究存在一定困难,进一步的研究还有待开展。最后指出,对既能揭示FSMA微观机理又能预测其宏观热磁力学行为的本构模型、描述FSMA所有特性的统一模型、面向应用的FSMA简化本构模型等问题,尚有待深入研究。     

在工作程度高的地区如何筛选矿致磁异常

分析了在工作程度高的地区进一步筛选矿致磁异常的可能性;提出了在工作程度高的地区筛选矿致磁异常的优先顺序建议。     

利用双视角消除太阳矢量磁场观测中的180◦不确定性

随着"环日轨道器"(Solar Orbiter, SO)的在轨运行,太阳磁场观测进入了双视角遥测的时代.对利用太阳磁场的双视角观测改正矢量磁图中存在的横场(垂直于视线方向的磁场分量) 180°不确定性进行了模拟,首先模拟了对解析解得到磁图的双视角观测,然后利用"日震学和磁学成像仪"(Helioseismic and Magnetic Imager, HMI)在不同时间观测到的一个老化黑子的磁图模拟了双视角观测.发现要改正一个磁图中横场方向的180°不确定性,在观测上只需要另外一个平行于视线方向的磁场即纵向磁场观测的协助.利用HMI的磁场观测模拟,估算显示30°的张角能够改正50 Gs磁场中的180°不确定性.更大的张角虽然更有利于更弱磁场的改正,但是考虑到投影效应的不利影响, 30°左右的张角应该是未来空间设备进行多视角观测太阳磁场的最佳张角.     

Day-side ionospheric conductivities at Mars

We present estimates of the day-side ionospheric conductivities at Mars based on magnetic field measurements by Mars Global Surveyor (MGS) at altitudes down to ∼100 km during aerobraking orbits early in the mission. At Mars, the so-called ionospheric dynamo region, where plasma/neutral collisions permit electric currents perpendicular to the magnetic field, lies between 100 and 250 km altitude. We find that the ionosphere is highly conductive in this region, as expected, with peak Pedersen and Hall conductivities of 0.1-1.5 S/m depending on the solar illumination and induced magnetospheric conditions. Furthermore, we find a consistent double peak pattern in the altitude profile of the day-side Pedersen conductivity, similar to that on Titan found by Rosenqvist et al. (2009). A high altitude peak, located between 180 and 200 km, is equivalent to the terrestrial peak in the lower F-layer. A second and typically much stronger layer of Pedersen conductivity is observed between 120 and 130 km, which is below the Hall conductivity peak at about 130-140 km. In this altitude region, MGS finds a sharp decrease in induced magnetic field strength at the inner magnetospheric boundary, while the day-side electron density is known to remain high as far down as 100 km. We find that such Titan-like behaviour of the Pedersen conductivity is only observed under regions of strongly draped magnetospheric field-lines, and negligible crustal magnetic anomalies below the spacecraft. Above regions of strong crustal magnetic anomalies, the Pedersen conductivity profile becomes more Earth-like with one strong Pedersen peak above the Hall conductivity peak. Here, both conductivities are 1-2 orders of magnitude smaller than the above only weakly magnetised crustal regions, depending on the strength of the crustal anomaly field at ionospheric altitudes. This nature of the Pedersen conductivity together with the structured distribution of crustal anomalies all over the planet should give rise to strong conductivity gradients around such anomalies. Day-side ionospheric conductivities on Mars (in regions away from the crustal magnetic anomalies) and Titan seem to behave in a very similar manner when horizontally draped magnetic field-lines partially magnetise a sunlit ionosphere. Therefore, it appears that a similar double peak structure of strong Pedersen conductivity could be a more general feature of non-magnetised bodies with ionised upper atmospheres, and thus should be expected to occur also at other non-magnetised terrestrial planets like Venus or other planetary bodies within the host planet magnetospheres.     

Type Ia supernovae and remnant neutron stars

On the basis of the current observational evidence, we put forward the case that the merger of two CO white dwarfs produces both a Type Ia supernova explosion and a stellar remnant, the latter in the form of a magnetar. The estimated occurrence rates raise the possibility that many, if not most, Type Ia supernovae might result from white dwarf mergers.