The study of proto-magnetar winds

The velocity profiles and properties of proto-magnetar winds are investigated.It is found that the corotation of wind matter with magnetic field lines significantly affects r-process nucleosynthesis and could lead to long duration γ-ray bursts and hyper-energetic supernovae.     

六盘山群沉积物磁化率记录的早白垩世气候变化

白垩纪气候环境研究对认识现今全球环境格局的形成具有重要意义,现有的白垩纪环境变化记录均来自海洋沉积物,本文通过对我国中部六盘山地区六盘山群地层沉积与岩石磁化率测量分析,获得了128.15～115.82Ma期间陆相沉积物记录的气候变化信息。结果显示磁化率值总体较低,以125Ma为界大致可以分为前低后高两个阶段;结合岩石磁学测量及沉积相、岩石中铁含量与磁化率变化关系分析,认为岩石磁化率主要与源区磁性矿物的种类及含量有关,据此揭示六盘山地区在该时间段气候总体为干热环境,并可分为128.15～125Ma间气候相对湿热和125～115.82Ma间气候相对温湿两个阶段。磁化率记录的这种气候转变与海洋沉积物记录的全球海平面温度变化趋势一致,但相对海平面温度由升高到降低的转折时间提前约1.7Ma。     

内蒙大井铜多金属矿床岩矿石磁参数研究

通过对大井矿区岩矿石标本进行磁参数测试、岩矿鉴定和主要成矿元素的化学分析,运用数理统计和相关分析的方法,分析了大井矿区岩矿石磁性的分布规律及产生磁性的主要矿物,并指出了该区进行高精度磁测的可行性,对引起磁异常零乱特征作了剖析,最后以南矿区实例说明磁测工作的应用效果。     

大比例尺高精度航磁异常查证方法的探讨

大比例尺、高精度航空磁测具有飞行高度低、定位误差小,磁测精度高的特点。在寻找深部隐伏矿时,查证高精度航磁异常可以省去地面面积性磁测环节,节省异常查证费用和加快异常查证速度。     

应用地面高精度磁法测量成果在贵州罐子窑-茅口地区圈定铅锌铜金找矿远景区

本文通过对贵州罐子窑-茅口地区地面高精度磁测资料数据处理、化极和延拓,对圈定的弱磁异常进行地质解释,推断一些弱磁异常可能与浅成辉绿岩或热液活动有关。结合地物化遥成果,圈定了花贡铅锌金找矿远景区、罐子窑铅锌找矿远景区和花嘎铅锌铜金找矿远景区。而异常查证结果表明,所发现的铅锌矿化蚀变带均出现在推断的隐伏构造或隐伏侵入体附近,表明物、化探异常的出现应与深部岩浆和构造活动为成矿提供了热源和成矿空间有关,为寻找铅锌矿提供了间接找矿依据。     

高温超导TEM瞬变磁场拟二维反演及应用效果

随着高温超导技术的应用及完善,在TEM测量中直接观测瞬变磁场信号已成为现实,而瞬变磁场数据反演解释方法成为当前急需解决的问题。在借鉴感应电动势资料反演解释方法的基础上,全面阐述了基于瞬变磁场的视电阻率定义,研究了TEM瞬变磁场拟二维反演技术,并从理论模型及实测资料两个方面验证了方法技术的实用性,为促进高温超导TEM的发展提供了方法技术支撑。     

Spatial Variations in Particle Size and Magnetite Concentration on Cedar Beach: Implications for Grain-Sorting Processes, Western Lake Erie, Canada

<正>This study examined spatial variations in the concentration,grain size and heavy mineral assemblages on Cedar Beach(Lake Erie,Canada).Magnetic studies of heavy mineral-enriched,dark-reddish sands present on the beach showed that magnetite(～150μm) is the dominant magnetic mineral.Surficial magnetic susceptibility values defined three zones:a lakeward region close to the water line(Zone 1),the upper swash zone(Zone 2) and the region landwards of the upper swash zone (Zone 3).Zone 2 showed the highest bulk and mass susceptibility(κ,χ) and the highest mass percentage of smaller grain-size(250μm) fractions in the bulk sand sample.Susceptibility(i.e.κandχ) values decreased and grain size coarsened from Zone 2 lakewards(into Zone 1) and landwards (into Zone 3),and correlated with the distribution of the heavy mineral assemblage,most probably reflecting preferential separation of large,less dense particles by waves and currents both along and across the beach.The eroded western section of Cedar Beach showed much higher concentrations of heavy minerals including magnetite,and finer sand grain sizes than the accreting eastern section, suggesting that magnetic techniques could be used as a rapid,cost-effective way of examining erosion along sensitive coastline areas.     

Towards an understanding of the Of?p star HD 191612: optical spectroscopy

We present extensive optical spectroscopy of the early-type magnetic star HD 191612 (O6.5f?pe–O8fp). The Balmer and He  i lines show strongly variable emission which is highly reproducible on a well-determined 538-d period. He  ii absorptions and metal lines (including many selective emission lines but excluding He  ii λ4686 Å emission) are essentially constant in line strength, but are variable in velocity, establishing a double-lined binary orbit with   P _orb= 1542 d, e = 0.45  . We conduct a model-atmosphere analysis of the spectrum, and find that the system is consistent with a ∼O8 giant with a ∼B1 main-sequence secondary. Since the periodic 538-d changes are unrelated to orbital motion, rotational modulation of a magnetically constrained plasma is strongly favoured as the most likely underlying 'clock'. An upper limit on the equatorial rotation is consistent with this hypothesis, but is too weak to provide a strong constraint.     

Peculiarities of entropy and magnetosonic waves in optically thin cosmic plasma

The stability problem for small magnetohydrodynamic (MHD) perturbations in an optically thin, perfectly conducting uniform plasma with a cosmic abundance of elements is solved in the linear approximation. The electron heat conduction along the magnetic field and the proton heat conduction across the field are taken into account. We have shown for the first time that the entropy waves can grow exponentially, while the magnetosonic waves are damped in a wide range of physical conditions closest to the conditions in stellar coronae with the proper allowance for radiative losses. Slow magnetosonic waves are damped particularly rapidly. For the solar corona, the calculated damping decrement of slow magnetosonic waves agrees well with the averaged one in 11 quasi-periodic events observed from the TRACE satellite in extreme ultraviolet radiation. Other possible astrophysical applications of the results obtained are briefly discussed.