遥感地质学教学改革3W原则及支撑创新创业训练的探索

在地球大数据与空间对地观测技术飞速发展的时代背景下,遥感地质学课程需要紧密围绕培养创新型人才、服务全球可持续发展开展教学改革与评估.本文以中国海洋大学为例,提出可具推广性的教学改革与评估3W原则,即为什么要开课(Why)、讲什么内容(What)、时间如何安排(When),并探讨了近年来遥感地质学课程建设与毕业设计选题在支撑大学生创新创业训练方面的作用与成效.     

地铁施工对济南白泉泉群流量的影响

为研究地铁建设对济南白泉泉群的影响，在综合分析白泉泉域地质、水文地质条件的基础上，假定研究区岩溶强径流带位置及水力性质，利用FEFLOW软件建立地下水流数值模型。以规划地铁M1号线为研究对象，分析了济南东站、梁王站、梁王东站分别施工及3个站同时施工4种情景下，采用施工降水或施工降水+人工回灌两种施工方式对白泉泉群流量的影响。结果表明：单独采用施工降水的施工方式使得白泉泉群流量衰减，其中3个站同时施工对泉流量的影响最大，泉流量最大衰减达5.48%；各站分别施工时，济南东站对泉流量影响最大，泉流量较未施工时减少了0.043×10⁴ m³/d。采用施工降水+人工回灌的施工方式，能够有效缓解泉流量的衰减，各车站施工时的泉流量衰减由仅施工降水时的2.26%~5.48%降低至0.08%~1.21%。岩溶强径流带有利于地下水形成优势径流，促进白泉泉群补给，一定程度上缓解因地铁施工引起的泉流量衰减。     

秦岭南缘勉略带构造属性及晚古生代地质背景:来自碎屑锆石U-Pb年代学的制约

勉略构造带作为秦岭造山带内重要的构造边界,关于其构造属性及晚古生代以来的地质背景,一直是学术界争论的焦点。碎屑锆石U-Pb年代学在限定地层单元的最大沉积年龄、研究区域构造岩浆事件及约束构造地质背景等方面行之有效。基于此,通过对勉略带内五郎坪北侧两河口变沉积地层和侵入其中的变形花岗岩脉体进行LA-ICP-MS锆石U-Pb年代学研究。获得2件变形花岗岩脉的结晶年龄均为406±1Ma。碎屑锆石主年龄谱分别为422～456Ma和558～826Ma,峰值年龄为441Ma和771Ma、813Ma,次级年龄谱分别为942～1495Ma和1658～2981Ma,峰值年龄不明显。依据最小一组碎屑锆石的峰值年龄(441Ma),和侵入其中的变形花岗岩脉(406±0.6Ma),限定该变沉积地层形成时代为406～441Ma(S_1-D_1)。碎屑锆石年龄谱显示该套变沉积地层物质来源较为复杂,其中秦岭造山带及扬子板块北缘早古生代、新元古代岩浆岩为其提供了74%±的物源,古老变质基底为其提供了26%±的物源。通过与区域上已有资料对比,认为勉略构造带内晚古生代沉积地层形成环境与邻区大致相同,且本次所获得的变沉积岩碎屑锆石年龄谱也与邻区泥盆系相似。综合认为,勉略构造带与邻区在晚古生代应属同一构造环境,晚古生代"勉略海盆"应当包括整个南秦岭。     

雄安新区地热地质模型探究：来自地球物理的证据

雄安新区内地热资源丰富，区内有牛驼镇地热田、容城地热田和高阳地热田，地热资源开发利用较早，但是对其深部热源机制仍未形成统一观点。为了研究雄安新区内地热田深部热源机制，在新区及外围进行了深反射地震和长周期大地电磁探测，对取得的同剖面的深反射地震和大地电磁数据进行处理和综合解释，探明了研究区从地表至莫霍面范围内地质构造和电性结构。下地壳结构在深反射地震剖面与大地电磁剖面上有很好的对应关系。电阻率低值区对应着在深反射地震剖面上存在一系列反射同相轴，且同相轴可以延续到莫霍面，电阻率高值区对应着在深反射地震剖面上无明显连续反射同相轴，尤其是在莫霍面之上呈现地震反射近似"空白区"。结合区域地热资料构建了研究区深部地热地质模型，对新区内深部地热机制进行了解释。该模型为"二元"生热模型，其热源包含两个部分，深部地幔热源和地壳放射性元素衰变生热。放射性元素衰变生热占地表热流的接近30%，而幔源热流在地表热流中的占比可达约70%。在牛驼镇下方，莫霍面以上，由于地幔热物质上涌造成下地壳上隆，幔源岩浆底侵作用于下地壳形成了局部热异常，该热异常具有低速高导的地球物理特征，认为是牛驼镇地热田和容城地热田的深部热源；以区域断裂为热通道，大地热流由深部向上传导、扩散到牛驼镇凸起和容城凸起顶部，对碳酸盐岩储水层进行加热，形成地热储层；上覆新近系沉积地层是良好的热盖层。     

碳中和目标下关键矿产在清洁能源转型中的作用、供需分析及其建议

在"碳中和"目标的驱动下，全球能源系统向清洁化、低碳化甚至无碳化发展已是大势所趋。针对向清洁能源转型的需求，采用了统计对比、分类汇总、综合分析等方法，分析研究了关键矿产在电池、电网、低碳发电和氢能等行业中的作用和需求。结合当前关键矿产产量的地理集中度高、项目开发周期长、资源质量下降等矿产供应和投资计划不能满足清洁能源转型的需求等问题，提出确保关键矿产多样性供应，推动价值链各环节的技术创新，扩大回收利用，增强供应链弹性和市场透明度，将更高的环境、社会和治理标准纳入主流程及加强生产者和消费者之间的国际合作等建议。     

敦煌北部岩浆-变质杂岩构造环境初步探讨:对中亚造山带南缘扩展方式的启示

中亚造山带南缘如何向南扩展，对深入理解增生型造山作用和大陆地壳生长机制以及中亚构造域与特提斯构造域的衔接具有重要科学意义。作为中亚造山带南缘的关键构造单元，敦煌构造带大地构造属性长期备受关注且颇有争议。传统观点认为敦煌构造带是古亚洲洋南侧的前寒武纪稳定大陆地块，以刚性块体的形式参与了中亚造山带南缘的最终拼贴过程。然而，近年来研究认为敦煌构造带卷入了古亚洲洋南部的俯冲增生造山过程，属于中亚造山带南缘的增生系统。显然，这一争议限制了对中亚造山带南缘向南扩展方式及增生造山过程的理解。敦煌北部三危山地区出露一套古生代岩浆-变质杂岩，是解开这一争论的关键。本文综合前人研究基础及新的资料，归纳了这套岩浆-变质杂岩的野外岩石-构造组合、地球化学和年代学等方面特征：该岩浆-变质杂岩整体显示"二元结构"特征，即较老的增生杂岩为基底，弧岩浆岩侵入或不整合覆盖其上；其中岩浆岩属于中钾-高钾钙碱性系列中酸性岩浆岩，富集大离子亲石元素（LILE）和轻稀土元素（LREE），亏损高场强元素（HFSE），与典型的弧岩浆岩类似，并且微量元素组成特征反映中酸性岩浆的源区与俯冲沉积物部分熔融有关；岩浆作用大致归为510Ma、460~410Ma和370~360Ma三期。岩浆岩中结晶锆石不一致的ε_Hf（t）值（既有正值，又有负值）以及继承锆石的存在表明，岩浆源区既有古老地壳物质的加入，也有新生地壳物质的形成。以上这些特征与发育在增生杂岩之上的增生弧十分类似，因此本文提出敦煌北部岩浆-变质杂岩的属性为古生代增生弧，并且该增生弧与其南部的红柳峡俯冲增生杂岩共同勾勒出敦煌构造带自北向南增生弧-增生杂岩的基本构造格架，即敦煌构造带的大地构造属性实为造山带而非稳定地块。结合区域地质背景及敦煌地区与北山地区古生代至早中生代构造-热事件的对应关系，认为敦煌造山带属于中亚造山带中段南缘的增生系统，中亚造山带中段以增生弧-增生杂岩的形式向南扩展至敦煌地区。     

The boundary value problem of Poisson’s equation with Stokes’ boundary condition

The following Poisson’s equation with the Stokes’ boundary condition is dealt with $$\left\{ \begin{gathered} \nabla ^2 T = - 4\pi Gp outside S, \hfill \\ \left. {\frac{{\partial T}}{{\partial h}} = \frac{1}{\gamma }\frac{{\partial y}}{{\partial h}}T} \right|_s = - \Delta g, \hfill \\ T = O\left( {r^{ - 3} } \right) at infinity, \hfill \\ \end{gathered} \right.$$ whereS is reference ellipsord. Under spherical approximation transformation, the ellipsoidal correction terms about the boundary condition, the equation and the density in the above BVP are respectively given. Therefore, the disturbing potentialT can he obtained if the magnitudes aboveO(ε⁴) are neglected.     

Investigation by backscatter radar of artificial irregularities produced in ionospheric plasma heating experiments

The artificial ionospheric turbulence occurs in the ionosphere illuminated by high power HF radio waves. There are a lot of irregularities stretched along the geomagnetic field in this region. The investigation of the artificially disturbed ionospheric region is based on the reception of back scattered signals (BSS) which permits the basic parameters of this region to be estimated and its inhomogeneous structure to be described.Experiments were carried out using ‘Sura’ heating facility in the frequency range of ? = 4.7–9 MHz (ordinary mode) with the effective radiated power P_eff = 50–70 MW beamed vertically upwards. The most important dynamic and statistical BSS characteristics (the built-up time, the relaxation and autocorrelation times, the BSS amplitude spatial correlation function and power spectra) were measured using probe waves in the frequency range of that made it possible to obtain the basic parameters of the artificial irregularities. The model representation of a disturbed region in a form of a periodic structure gives a possibity to evaluate the scale of the structure, the whole size of the disturbance and its power and to calculate the main BSS characteristics.     

The appearance of polarization in radiation from hot stars due to the faraday rotation effect as a possible method of determining stellar magnetic fields

The effect of Faraday rotation is shown to lead to the appearance of linear polarization of stellar radiation scattered in an optically-thin circumstellar electron-magnetized shell, even in the case when the shell is spherical. The spectral dependence of the polarization degree is evaluated for scattering in (i) a spherically-symmetric magnetized shell with a power-law radial dependence of the electron density, and (ii) a non-spherical ellipsoidal uniform envelope. The position of maximum in the polarization spectrum permits us to determine the magnetic field magnitude on a star surface. If the rotational and magnetic axes do not coincide, the periodic variability of the polarization will be observed with the period of stellar rotation. Some Be-stars, such as Cas, 48 Lib, EW Lac, Aqr, HD 45677, X Per, are proposed as candidates to be investigated for magnetic fields, as well as some stars of the T Tau-type. This method may be also applied to supernovae shells.     

Microwave radiation from magnetic stars

Cyclotron microwave emission from magnetic stars is considered, assuming that they have coronae with the temperatureT10⁷ K and the emission measureEM10⁵⁴ cm^–3. It has been shown that the cyclotron radiation from a star with a dipole magnetic field has a specific spectrum with a maximum in the frequency rangesv _o/2 >v >sv _o/2 (s being the number of cyclotron harmonic, andv _o the gyrofrequency corresponding to the polar magnetic field) and radiation flux decreasing towards lower frequencies asv _4/3. The frequency of the spectrum maximum depends on the angle between the line-of-sight and the magnetic axis of the star. The observed radiation from a rotating magnetic star can be modulated with a modulation depth of about 0.2 at frequencies near maximum. The radiation is partially circularly-polarized in the sense of an extraordinary mode. The degree of polarization is almost constant at frequenciesv >sv _o/2 and increases with frequency atv >sv _o/2. The estimation of cyclotron radio fluxes of the nearest magnetic stars shows that they are observable in microwaves by means of modern radio astronomy.