Submillimeter-wave and observations of the event on 28 November, 2001

We present a detailed study of a 1B/M6.9 impulsive flare combining high time resolution (1 ms) and instantaneous emission source localization observations at submillimeter frequencies (212 GHz), obtained with the solar submillimeter telescope (SST), and Hα data from the Hα solar telescope for argentina (HASTA). The flare, starting at 16:34 UT, occurred in active region (AR) 9715 (NOAA number) on November 28, 2001, and was followed by an Hα surge. We complement our data with magnetograms from the Michelson Doppler Imager (SOHO/MDI). SST observed a short impulsive burst at 212 GHz, presenting a weak bulk emission (of about 90 sfu) composed of a few shorter duration structures. The integrated Hα and the 212 GHz light curves present a remarkable agreement during the impulsive phase of the event. The delay between both curves stays below 12 s (the time resolution of the Hα telescope). The flare as well as the surge are linked to new flux emergence very close to the main AR bipole. Taking into account the AR magnetic field evolution, we infer that magnetic field reconnection, occurring at low coronal levels, could have been at the origin of the flare; while in the case of surge this would happen at the chromospheric level.     

On core surface flows inferred from satellite magnetic data

Satellite-data allows the magnetic field produced by the dynamo within the Earth’s core to be imaged with much more accuracy than previously possible with only ground-based data. Changes in this magnetic field can in turn be used to make some inferences about the core surface flow responsible for them. In this paper, we investigate the improvement brought to core flow computation by new satellite-data based core magnetic field models. It is shown that the main limitation now encountered is no longer the (now high) accuracy of those models, but the “non-modelled secular variation” produced by interaction of the non-resolvable small scales of the core flow with the core field, and by interaction of the (partly) resolvable large scales of the core flow with the small scales of the core field unfortunately masked by the crustal field. We show how this non-modelled secular variation can be taken into account to recover the largest scales of the core flow in a consistent way. We also investigate the uncertainties this introduces in core flows computed with the help of the frozen-flux and tangentially geostrophic assumptions. It turns out that flows with much more medium and small scales than previously thought are needed to explain the satellite-data-based core magnetic field models. It also turns out that a significant fraction of this flow unfortunately happens to be non-recoverable (being either “non-resolvable” because too small-scale, or “invisible”, because in the kernel of the inverse method) even though it produces the detectable “non-modelled secular variation”. Applying this to the Magsat (1980) to Ørsted (2000) field changes leads us to conclude that a flow involving at least strong retrograde vortices below the Atlantic Hemisphere, some less-resolved prograde vortices below the Pacific Hemisphere, and some poorly resolved (and partly non-resolvable) polar vortices, is needed to explain the 1980-2000 satellite-era average secular variation. The characteristics of the fraction of the secular variation left unexplained by this flow are also discussed.     

南半球对流层气候年代际变化及其与太阳活动的联系

通过南半球对流层温度场谱分析和逐次滤波分析发现，南半球对流层大气温度场半个多世纪以来呈现明显的持续升温趋势，升温幅度由低层到高层逐步增加，其中地面层1 000 hPa年升温率为0.013℃/a，对流层中部500 hPa年升温率为0.019℃/ a，对流层上部300 hPa年升温率为0.036℃/ a；滤除南半球大气温度场的趋势变化，发现南半球大气温度场从地面层直至对流层顶广泛盛行着十分显著的与太阳磁场磁性22年周期变化相一致的变化周期。太阳磁场磁性周期变化趋势略有超前，分析认为，这是南半球对流层大气气候系统对太阳磁场周期性变化的响应。进一步分析还发现，南半球从地面层1 000 hPa到对流层顶，再到平流层中部10 hPa各层次大气温度变化22年周期分量振荡位相基本一致，周期振幅由低层到高层迅速增大，说明太阳磁场变化对对流层高层比低层影响大，对平流层影响更大。其中地面层1 000 hPa温度场的22年变化周期是在滤除趋势变化和11年周期之后才显现出来的，所以太阳磁场磁性周期变化对地面层气候的影响较小并且经常处于被掩盖状态；南半球地面层1 000 hPa温度场滤除趋势变化之后显示出十分显著的与太阳活动11年周期相一致的变化周期，分析认为，这是南半球对流层大气气候系统对太阳活动11周期性变化的响应。对流层上层300 hPa温度场滤除趋势变化和22年周期之后也显示出11年变化周期，而对流层中部500 hPa则无此周期反应，说明太阳活动11年周期对地面层1 000 hPa大气气候影响最明显，对流层中上层影响较弱。     

宁东煤田枣泉矿井综合物探效果

为探明宁东煤田枣泉矿井首采区煤层自然范围及充水性，根据采区内地球物理物征，采用高精度磁法，直流电测深法和激发极化法进行综合勘探。在磁法勘探中结合测区曲线特征，建立数据体模型，正演计算烧变岩边界；电法勘探利用烧变岩含水后电阻率降低的特征确定其含水范围及富水性。     

高精度磁测在马家店铁矿找矿中的应用

在柳河马家店铁矿中应用高精度磁法勘探,证明了磁法在寻找磁铁矿上具有显著的效果。文章通过论述磁异常特征,结合本区的地质情况,对所取得的磁异常进行定性研究,同时结合基础地质工作,在磁异常上实施工程验证,成功发现铁矿床,总结该区铁矿成矿规律,为今后物探、地质相结合的综合找矿起到了一定的指导作用。     

利用重磁资料研究深部构造与金矿成矿关系

本文探讨了在山西省利用区域重磁资料研究深部构造与金矿成矿的关系及成矿环境的有利标志。研究结果表明，山西省的区域重、磁场以北东、北北东向为特点，中太古界为主要磁源层。根据磁场特征．用统计方法可将前寒武纪构造分为若干隆起和断陷，它们对金矿成矿起到了一定控制作用。另外，利用区域重力资料计算了山西省莫霍面深度，结果表明，莫霍面由东南向北西逐渐变深，莫霍面和岩石圈的结构控制了不同类型岩浆岩的展布，为选择金矿成矿有利地区提供了依据。并提出叠加型异常是重要的找矿靶区。     

宁沪高速公路句容段两侧土壤磁化率异常与重金属元素的关系研究

高速公路两侧土壤的磁化率从路中央向两侧具有逐渐降低的特征,相对应的样品中的重金属Cu、Pb、Zn、N i、Cr、Fe等元素的含量也具有从路中心向两侧逐渐降低的现象。相关分析表明,土壤磁化率与土壤中的Cu、Pb、Zn、N i、Cr、Fe的相关性显著,因而可以利用磁化率异常来指示高速公路两侧土壤的重金属污染状况。元素的赋存形态分析表明铁锰氧化物态与残渣态是Cu、Pb、Zn、N i、Cr、Fe的主要赋存形式;各元素的形态分析结果与土壤磁化率的相关统计分析表明,高速公路两侧土壤的磁化率与可交换态中的Cu、Pb、Zn、铁锰氧化物态中的Fe、Pb、Zn、有机还原态中的Cu、Cr、Fe、Zn和残渣态中的Cu、Pb、Zn、Cr、Co、N i具有明显的相关性。     

武汉天兴洲近代沉积物的磁性特征及其环境意义

利用多磁性参数(包括质量磁化率、频率磁化率、饱和等温剩磁、退磁系数以及热磁曲线)及磁组构分析,以长江中游武汉天兴洲近代河流沉积物为研究对象, 探讨了近100年以来沉积物磁性参数变化特征及其对长江中上游水文变化及气候环境的指示.结果表明,上部组合带(0.60~1.50 m)和下部组合带(2.40~3.30 m)沉积物的磁性载体以亚铁磁性矿物磁铁矿为主,同时存在少量较稳定的不完整反铁磁性物质,中部(1.50~2.40 m)亚铁磁性矿物相对较少,且剖面上部沉积物的超顺磁(SP)颗粒对沉积物χ贡献较大.整个沉积剖面自下而上磁性矿物含量呈“C”字型变化,反映了“软”-“硬”-“软”的磁性特性.沉积物磁组构组合带研究显示,历史时期沉积环境水动力强度、颗粒排列有序化程度以及长江流速发生了明显的变化,沉积环境水动力强度经历了“不稳定”－“稳定”－“不稳定”的变化过程,反映了长江古水文状况的变化.近代沉积物磁性特征变化格局与1900年以来以来长江中上游“暖湿”-“温凉”-“暖湿”气候环境变化和“强降水”-“弱降水”-“强降水”以及长江汉口站流量变化过程相吻合.这一研究成果为深刻认识历史时期长江流域气候环境变迁其及对长江古水文和沉积环境的影响提供了重要的参考资料.