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。     

支持向量机(SVM)及其在场预测中的应用

介绍一种新的非线性回归分析方法--SVM回归.利用EOF能分解数据场和SVM回归分析可建立因子与预报量非线性关系的优势,设计预报方案：（1） 将因子场和预报场分别用方差标准化、EOF场展开,提取两场时间系数;（2） 用SVM回归分析实现因子场时间系数对预报场时间系数非线性预测;（3） 由预测的预报场时间系数与对应空间函数反演原场.用交叉检验的方法,对1960～2003年1月热带海表温度场预报汛期（6～8月）华中区域降水场进行试验.SVM回归44年独立预报平均技巧评分10.4%,较随机预报具有明显的技巧水平,优于经典回归.     

电离层电场的半年变化对F2区峰值电子浓度的影响

利用一个电离层理论模式,模拟了太阳活动低年、地磁宁静情况下,中低纬和赤道地区电离层F2区峰值电子浓度(NmF2)的半年变化规律,重点讨论了电离层电场对NmF2半年变化的影响.模拟结果表明,当输入的电场没有周年和半年变化时,磁赤道地区电离层NmF2本身就具有一定的半年变化特征,而在稍高的纬度上,NmF2半年变化的强度较弱.当输入的电场具有一定的半年变化时,电离层NmF2的半年变化强度有明显的改变,且这种改变随地方时和地磁纬度不同有明显的差别.在地磁赤道附近的电离层赤道槽地区,从上午到午夜的时间内,具有半年变化的电场对电离层NmF2半年变化的强度是减弱的作用,在其他的时间内,电场对电离层NmF2半年变化强度是加强的作用.而在稍高纬度的电离层驼峰地区,情况明显不同.从上午一直到翌日日出前,具有半年变化的电场对电离层NmF2半年变化的幅度都是加强的作用.在其他的时间内,电场对电离层NmF2半年变化的幅度是减弱的作用.同时,研究表明电离层电场对NmF2半年变化的作用和“赤道喷泉”现象强烈相关.     

复杂地表条件下共反射面元（CRS）叠加方法研究

在地表地形复杂的情况下,静校正不易做好,这是制约山地资料处理质量的一个很重要的因素.复杂地表共反射面元（CRS）叠加不需对叠前数据做静校正,而且在得到叠加剖面后可以利用叠加得到的波场参数剖面实现基准面重建.地震数据的试算表明,复杂地表CRS叠加得出的剖面与常规处理剖面相比有着较高的信噪比和同相轴连续性.与水平地表CRS叠加不同的是,在复杂地表CRS叠加的时距公式中,波场三参数耦合,难以通过简化CRS道集的方法将它们全部分离并逐个优化.引入模拟退火算法后,有效地解决了这一组合优化的难题.     

锦45块储层流动单元

正确地划分储层流动单元,对预测剩余油分布、调整开发方案、提高采收率都具有重要意义。采用多参数的聚类分析和模糊综合评价相结合的方法进行储层流动单元的划分,在此基础上应用BP网络技术对流动单元进行预测。研究表明,本区储层可以划分为Ⅰ、Ⅱ、Ⅲ、Ⅳ 4类流动单元:其中Ⅰ类是该区储集性能最好的储层流动单元,虽然开发程度较高,大部分井已经关闭,但个别井目前仍具有一定的生产能力;Ⅱ类是该区储集性能较好的储层流动单元,水淹的程度较低,还存有一定的剩余油,是目前油田生产的主要区域;Ⅲ类是该区储集性能较差的流动单元,开发效果一般,动用程度较差,所以是油田进一步挖潜的区域;Ⅳ类是该区储集性能最差的流动单元,原始含油性很差,因此不是剩余油分布的主要区域。对各类流动单元特征进行了精细的分析,为油田综合治理提供了详细的地质依据。     

Subdiffusive transport in intergranular lanes on the Sun. The Leighton model revisited

In this paper we consider a random motion of magnetic bright points (MBP) associated with magnetic fields at the solar photosphere. The MBP transport in the short time range [0–20 minutes] has a subdiffusive character as the magnetic flux tends to accumulate at sinks of the flow field. Such a behavior can be rigorously described in the framework of a continuous time random walk leading to the fractional Fokker-Planck dynamics. This formalism, applied for the analysis of the solar subdiffusion of magnetic fields, generalizes the Leighton’s model.      

Wave Transformation and Scattering on Stationary Charged Particles in a Magnetoactive Plasma. II

The transformation of upper-hybrid, lower-hybrid, and magnetosonic waves on a heavy charged particle lying at the plane boundary of a magnetoactive plasma is considered. The angular distribution of the radiation resulting from wave transformation is investigated. The transformation of a low-frequency magnetosonic wave is suggested as a possible mechanism for pulsar radio emission.     

Towards self-consistent models of isolated neutron stars

We propose a self–consistent model to explain all observational properties reported so far on the isolated neutron star (INS) RX J0720-3125 with the aim of giving a step forward towards our understanding of INSs. For a given magnetic field structure, which is mostly confined to the crust and outer layers, we obtain theoretical models and spectra which account for the broadband spectral energy distribution (including the apparent optical excess), the X-ray pulsations, and for the spectral feature seen in the soft X-ray spectrum of RX J0720-3125 around 0.3 keV. By fitting our models to existing archival X-ray data from 6 different XMM–Newton observations and available optical data, we show that the observed properties are fully consistent with a normal neutron star, with a proper radius of about 12 km, a temperature at the magnetic pole of about 100 eV, and a magnetic field strength of 2–3×10¹³ G. Moreover, we are able to reproduce the observed long–term spectral evolution in terms of free precession which induces changes in the orientation angles of about 40 degrees with a periodicity of 7 years. In addition to the evidence of internal toroidal components, we also find strong evidence of non–dipolar magnetic fields, since all spectral properties are better reproduced with models with strong quadrupolar components.      

On Solar Intermediate Drift Radio Bursts at Decimeter and Meter Wavelength

Fiber – or intermediate drift – bursts are a continuum fine structure in some complex solar radio events. We present the analysis of such bursts in the X17 flare on 28 Oct. 2003. Based on the whistler wave model of fiber bursts we derive the 3D magnetic field structures that carry the radio sources in different stages of the event and obtain insight into the energy release evolution in the main flare phase, the related paths of nonthermal particle propagation in the corona, and the involved magnetic field structures. Additionally, we test the whistler wave model of fiber bursts for the meter and the decimeter wave range. Radio spectral data (Astrophysikalisches Institut Potsdam, Astronomical Observatory Ond?ejov) show a continuum with fibers for ≈?6 min during the main flare phase. Radio imaging data (Nançay Radio Heliograph) yield source centroid positions of the fibers at three frequencies in the spectrometer band. We compare the radio positions with the potential coronal magnetic field extrapolated from SOHO/MDI data. Given the detected source site configuration and evolution, and the change of the fiber burst frequency range with time, we can also extract those coronal flux tubes where the high-frequency fiber bursts are situated even without decimeter imaging data. To this aim we use a kinetic simulation of whistler wave growth in sample flux tubes modeled by selected potential field lines and a barometric density model. The whistler wave model of fiber bursts accurately explains the observations on 28 Oct. 2003. A laterally extended system of low coronal loops is found to guide the whistler waves. It connects several neighboring active regions including the flaring AR 10486. For varying source sites the fiber bursts are emitted at the fundamental mode of the plasma frequency over the whole range (1200?–?300 MHz). The present event can be understood without assuming two different generation mechanisms for meter and decimeter wave fiber bursts. It gives new insight into particle acceleration and propagation in the low flare and post-CME corona.