基于多尺度球面小波解算GPS应变场的方法及应用

提出了利用多尺度球面小波解算GPS应变场的方法,该方法通过建立不规则分布的小波基函数以凸显测站非均匀分布的特征,获取不同空间尺度的应变场.通过对模拟数据进行对比分析验证该方法的有效性,模拟结果显示,多尺度球面小波应变计算方法稳健性较好.在位移场中加入高斯随机误差(均值为0.0mm,标准差为0.5mm)对应变计算结果的影响可忽略不计.从原有位移场随机抽取的60%的数据解算应变场时,仍然能够获取比较可靠的结果,但如果出现大范围的数据空缺,则会对应变结果产生明显影响.基于华北地区GPS测站原始观测数据,通过高精度数据处理方法解算了该区域GPS速度场,根据多尺度球面小波方法,解算了该区域的应变率场及其误差,并分析了其空间分布特征.     

基于SIFT特征检测和密度峰值聚类的太阳活动区自动检测算法研究

太阳活动区是太阳大气中产生各种活动现象的区域,精确地检测和识别太阳活动区对理解太阳磁场的形成机制具有极为重要的科学意义.根据太阳活动区结构较为复杂的特点,基于尺度不变特征变换(ScaleInvariant Feature Transform, SIFT)和密度峰值聚类(Clustering by Fast Search and Find of Density Peaks,DPC)算法的优越性,提出了一种太阳活动区的自动检测和识别方法.首先,对太阳动力学天文台(Solar Dynamics Observatory, SDO)日震和磁场成像仪(Helioseismic and Magnetic Imager, HMI)的纵向磁图进行对比度增强;然后采用SIFT方法提取出全日面磁图中的特征点;最后利用DPC算法将特征点进行聚类,从而自动检测和识别出太阳活动区.研究结果表明, SIFT和DPC算法相结合的方法可以在不需要人工交互的情况下准确地自动检测出太阳活动区.     

逆断层中天然气运移特征的物理模拟

逆断层在活动期时易形成断层空腔,该空腔为天然气的穿层运移提供了畅通的通道,天然气在其中运移具涌流特征。如果断层空腔连通地表,天然气则大部分沿其逸出地表,仅有少量的天然气能注入断层两侧的相邻储层中。进入储层的天然气具有明显的选择性,气体首先向物性好、倾角陡和埋藏浅的储层中注入。如果没有其它动力,仅靠天然气自身浮力作用,断层下盘储层不能或很少能有天然气的注入。当断层处于静止期时,断层空腔消亡,天然气穿塑性层段的运移通道是破碎带中的岩石孔隙,天然气在其中的运移遵循达西渗流规律。天然气在断层带中的运移速度随断层充填物颗粒粒度的增加而呈指数关系增大,随断层倾角的增大呈指数关系增大,随断层充填物中泥质含量的增加呈幂函数关系减小。     

东南极冰盖Princess Elizabeth地区LGB69冰芯化学记录反映的南印度洋过去300 a大气环流变化

利用2002年中国南极考察期间在东南极冰盖Princess Elizabeth地区钻取的LGB69冰芯, 对其海盐离子与大气环流的关系进行了分析. 结果表明: 冰芯主要化学离子的经验正交函数(EOF)分解的第一特征向量(EOF1)可以作为描述海盐气溶胶的传输强度的代用指标, 可用于表征南印度洋准定常低压带海平面气压(SLP)的变化. 冰芯最近23 a(1979-2001年)的记录与SLP和低层风场的相关模态反映了海平面气压场准半年振荡(SAO)和南极大陆边缘下降风的季节特征. LGB69冰芯很好地记录了1708-2001年间南半球环状模(SAM)的变化特征, Na⁺时间序列呈现的3.5 a周期变化与SAM的周期变化具有很好地一致性. 在1970年SAM转为正位相后, 其与Na⁺的相关关系也由负相关转为正相关. LGB69冰芯的海盐离子可以作为重建过去近300 a海平面气压场和SAM变化的代用指标.     

The XMM‐Newton view of magnetars

Anomalous X‐ray Pulsars and Soft Gamma‐ray Repeaters are believed to be magnetars: isolated neutron stars powered by the decay of extremely high magnetic fields. We review some of the main results obtained with XMM‐Newton and discuss the prospects for future observations of this small but extremely interesting class of objects. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Electron reflectometry in the martian atmosphere

The technique of electron reflectometry, a method for remote estimation of planetary magnetic fields, is expanded from its original use of mapping crustal magnetic fields at the Moon to achieving the same purpose at Mars, where the presence of a substantial atmosphere complicates matters considerably. The motion of solar wind electrons, incident on the martian atmosphere, is considered in detail, taking account of the following effects: the electrons' helical paths around the magnetic field lines to which they are bound, the magnetic mirror force they experience due to converging field lines in the vicinity of crustal magnetic anomalies, their acceleration/deceleration by electrostatic potentials, their interactions with thermal plasma, their drifts due to magnetic field line curvature and perpendicular electric fields and their scattering off, and loss of energy through a number of different processes to, atmospheric neutrals. A theoretical framework is thus developed for modeling electron pitch angle distributions expected when a spacecraft is on a magnetic field line which is connected to both the martian crust and the interplanetary magnetic field. This framework, along with measured pitch angle distributions from the Mars Global Surveyor (MGS) Magnetometer/Electron Reflectometer (MAG/ER) experiment, can be used to remotely measure crustal magnetic field magnitudes and atmospheric neutral densities at ∼180 km above the martian datum, as well as estimate average parallel electric fields between 200 and 400 km altitude. Detailed analysis and full results, concerning the crustal magnetic field and upper thermospheric density of Mars, are left to two companion papers.     

Boundary layer in the MRI experiment PROMISE

One of the most convenient approaches to observe experimentally the magnetorotational instability (MRI) is to use a magnetized Taylor‐Couette setup. The flow of liquid metal between two rotating, concentric cylinders can become unstable in the presence of an external magnetic field. One of the issues which should be addressed when designing such an experiment is the influence of plates enclosing the cylinders fromthe top and the bottom. In this paper we discuss properties of the boundary layer which arises near these plates. Our primary concern is the importance of this layer in the MRI experiment PROMISE. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Can turbulent plane‐shear flows support large‐scale dynamos?

Turbulent plane‐shear flow is found to show same basic effects of mean‐fieldMHD as rotating turbulence. In particular, the mean electromotive force (EMF) includes highly anisotropic turbulent diffusion and alpha‐effect. Only magnetic diffusion remains for spatially‐uniform turbulence. The question is addressed whether in this case a self‐excitation of a magnetic field by so‐called sher‐current dynamo is possible and the quasilinear theory provides a negative answer. The streamaligned component of the EMF has the sign opposite to that required for dynamo. If, however, the turbulence is not uniform across the flow direction then a dynamo‐active α ‐effect emerges. The critical magnetic Reynolds number for the alpha‐shear dynamo is estimated to be slightly above ten. Possibilities for cross‐checking theoretical predictions with MHD experiments are discussed. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Results of a modified PROMISE experiment

The PROMISE experiment relies on the fact that the critical Reynolds number for the appearance of the magnetorotational instability (MRI) in liquid metal flows drastically decreases when the purely axial magnetic field is replaced by a helical one. We report the results of a modified version of this experiments in which the radial electrical boundary conditions are changed. Special focus is laid on the role of the radial jet region where the two Ekman vortices from the top and the bottom meet each other. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)