砂泥岩间互地层等效岩石力学参数计算模型及其应用

以地层岩石的变形分析为基础,从能量的角度出发,利用应变能理论及能量守恒定律推导出了等效岩石力学参数的一般计算公式,并建立了测井资料计算模型;利用该模型计算了库车坳陷克拉A气田目的层系巴什基奇克组的等效岩石力学参数,并以计算结果为基础进行了应力场及储层裂缝的数值模拟;最后讨论了等效岩石力学参数测井资料计算模型的优点及适用条件。模拟结果显示,储层裂缝集中发育在背斜高点及单斜构造部位,与气田目前的开发实践基本一致,表明了所建模型的合理性;等效岩石力学参数适用于区域性的横向应力场及储层裂缝预测,不适于预测局部或垂向上的储层裂缝分布规律。     

TWR-01型天气雷达回波特征参数的提取和应用

TWR-01型天气雷达是小型数字化雷达,具备GIS和GPS功能,可适应移动式、固定式的增雨防雹作业指挥和气象保障服务.TWR-01型天气雷达回波特征参数的提取技术是基于影像的目标轮廓提取方法.目标轮廓提取方法在图像识别与图像分析中占有重要地位,广泛应用于测量和遥感领域.TWR-01型天气雷达同波特征参数提取的技术方法是...     

环境磁学研究现状和进展

环境磁学是八十年代逐步发展起来的具有学科交叉特点的边缘学科。它主要应用岩石和矿磁学研究磁性颗粒的搬运、沉积以及转化受大气圈、水圈和岩石圈环境变化影响的过程。近年来，环境磁学已提供了大量有关全球变化过程以及人类活动对环境影响等重要资料，其研究范畴迅速扩展，已成为当今地学的前沿学科之一。     

Long‐term photometry of three active red giants in close binary systems: V2253 Oph,IT Com and IS Vir

We present and analyze long‐term optical photometric measurements of the three active stars V2253 Oph, IT Com and IS Vir. All three systems are single‐lined spectroscopic binaries with an early K giant as primary component but in different stages of orbital‐rotational synchronization. Our photometry is supplemented by 2MASS and WISE near‐IR and mid‐IR magnitudes and then used to obtain more accurate effective temperatures and extinctions. For V2253 Oph and IT Com, we found their spectral energy distributions consistent with pure photospheric emission. For IS Vir, we detect a marginal mid‐IR excess which hints towards a dust disk. The orbital and rotational planes of IT Com appear tobe coplanar, contrary to previous findings in the literature. We apply a multiple frequency analysis technique to determine photometric periods, and possibly changes of periods, ranging from days to decades. New rotational periods of 21.55±0.03 d, 65.1±0.3 d, and 23.50±0.04 d were determined for V2253 Oph, IT Com, and IS Vir, respectively. Splitting of these periods led to tentative detections of differential surface rotations of δP/P ≈ 0.02 for V2253 Oph and 0.07 for IT Com. Using a time‐frequency technique based on short‐term Fourier transforms we present evidence of cyclic light variations of length ≈ 10 yr for V2253 Oph and 5–6 yr for IS Vir. A single flip‐flop event has been observed for IT Com of duration 2–3 yr. Its exchange of the dominant active longitude had happened close to a time of periastron passage, suggesting some response of the magnetic activity from the orbital dynamics. The 21.55‐d rotational modulation of V2253 Oph showed phase coherence also with the orbital period, which is 15 times longer than the rotational period, thus also indicating a tidal feedback with the stellar magnetic activity. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Composite spectra XIX: HD 208253, a long‐period binary whose hot secondary has enhanced strontium and barium

We separate and analyse the component spectra of the composite‐spectrum binary HD 208253. We find that the cool primary is an evolving star of spectral type G7 III, while its hot secondary is an early‐A dwarf. The giant is currently near the lowest point of the red‐giant branch and is slightly less luminous than its dwarf companion. We provide a set of precise radial‐velocity measurements for both stars. The double‐lined orbit which we derive from them shows that the component mass ratio is close to unity (q = 1.05 ± 0.01). We deduce the physical properties of both stars, determine their respective masses to be 2.75 ± 0.07 Me (giant) and 2.62 ± 0.07 Me (dwarf), and show that the orbit's inclination is within a degree or two of 68°. The spectrum of the A‐type component has quite component has quite narrow lines (we infer a rotational velocity of 18 km s^–1), though since the period of the orbit is well over 1 year that component cannot be in synchronous rotation. An intriguing property of the dwarf is its enhanced Sr and Ba, though it does not exhibit the other spectral peculiarities that would signal a classical Am star. While by no means unique amongst the multitude of oddities exhibited by A and early‐F stars, this dwarf which we have uncovered in a long‐period binary offers valuable constraints and challenges to stellar‐evolution theory. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

高分辨率非线性储层物性参数反演方法和应用

对于陆相沉积环境下的复杂隐蔽岩性储层,由于观测信息不准确,如信息重叠、信息缺失和噪音污染,以及岩石物理关系模糊等原因,储层横向预测存在不惟一性、不稳定性和不确定性.基于线性假定的常规储层横向预测技术已不适用于复杂隐蔽岩性储层的勘探.本文采用一种非线性储层岩性物性褶积模型,建立波阻抗与孔隙度/泥质含量的函数关系;通过多级结构分解和双向边沿子波检测来刻画复杂岩石物理关系;通过Caianiello褶积神经网络实现确定性反演、统计反演和非线性理论三者有机结合;最后联合应用基于逆算子的反演方法和基于正算子的重建算法实现了综合地质、测井和地震波阻抗信息进行高分辨率储层物性参数反演.非线性储层物性参数反演采用多井约束机制和分频反演方式,在陆相和近海油气勘探资料的实际应用中,取得了明显应用效果.     

2008汶川Ms8.0地震发生的深层过程和动力学响应

汶川Ms8.0强烈地震发生在一条现今并不活动的龙门山构造带上,造成了以汶川、映秀为中心及其周边地域的严重破坏和人员的重大伤亡.然而强烈震发生前却未见有可能的确切征兆或浅表层异常活动,即浅层过程与地震发生的深层过程并不匹配.为此对这次强烈地震"孕育"、发生和发展的深层过程进行了分析和探讨,初步研究表明:①在印度洋板块与欧亚板块陆—陆碰撞、挤压作用下,喜马拉雅造山带东构造结向NNE方向顶挤、楔入青藏高原东北缘,迫使高原深部物质向东流展,在受到以龙门山为西北边界的四川盆地阻隔下,一部分物质则转而向东南侧向运移;②龙门山地带在地形上差达3500±500m左右,而地壳厚度在龙门山西北部为60±5km左右,四川盆地为40±2km左右,而龙门山地带与其东、西两侧相比则为地壳厚度变化幅度达15～20km的突变地域,即为应力作用的耦合地带;③中、下地壳和地幔盖层物质以地壳低速层、低阻层(深20～25km)为第一滑移面,以上地幔软流层顶面为第二滑移面,且在四川盆地深部"刚性"物质阻隔下,深部壳、幔物质以高角度在龙门山构造带和四川盆地的耦合地带向上运移(或称逆冲),且在龙门山地表三条断裂构成的断裂系向下延伸到20km左右深处汇聚,二者强烈碰撞、挤压、震源介质破裂;在物质与能量的强烈交换下,应力得到释放,故形成了这次Ms8.0强烈地震.为此从深部初步揭示了这次强烈地震"孕育"、发生和发展的深层动力过程.     

2008汶川Ms8.0地震发生的深层过程和动力学响应

汶川M_s8.0强烈地震发生在一条现今并不活动的龙门山构造带上,造成了以汶川、映秀为中心及其周边地域的严重破坏和人员的重大伤亡.然而强烈震发生前却未见有可能的确切征兆或浅表层异常活动,即浅层过程与地震发生的深层过程并不匹配.为此对这次强烈地震“孕育”、发生和发展的深层过程进行了分析和探讨,初步研究表明：①在印度洋板块与欧亚板块陆—陆碰撞、挤压作用下,喜马拉雅造山带东构造结向NNE方向顶挤、楔入青藏高原东北缘,迫使高原深部物质向东流展,在受到以龙门山为西北边界的四川盆地阻隔下,一部分物质则转而向东南侧向运移;②龙门山地带在地形上差达3500±500 m左右,而地壳厚度在龙门山西北部为60±5 km左右,四川盆地为40±2 km左右,而龙门山地带与其东、西两侧相比则为地壳厚度变化幅度达15~20 km的突变地域,即为应力作用的耦合地带;③中、下地壳和地幔盖层物质以地壳低速层、低阻层（深20~25 km）为第一滑移面,以上地幔软流层顶面为第二滑移面,且在四川盆地深部“刚性”物质阻 隔下,深部壳、幔物质以高角度在龙门山构造带和四川盆地的耦合地带向上运移（或称逆冲）,且在龙门山地表三条断裂构成的断裂系向下延伸到20 km左右深处汇聚,二者强烈碰撞、挤压、震源介质破裂;在物质与能量的强烈交换下,应力得到释放,故形成了这次M_s.0强烈地震.为此从深部初步揭示了这次强烈地震“孕育”、发生和发展的深层动力过程.     

黏弹性双相介质参数反演的同伦方法

本文以介质的动态时域响应（位移、速度、加速度）作为反演的依据,对黏弹性双相介质的材料参数进行了反分析研究.根据附加条件,并考虑到由于测量误差和测量数据的不充分造成的反演问题的不适定性,将黏弹性双相介质的参数反演问题转化为非线性泛函的极小值问题,然后应用大范围收敛的同伦方法求出使泛函极小的根作为反问题的解.最后,以二维半空间黏弹性双相介质模型为例进行了数值反演分析,数值结果表明本文方法在参数的反演过程中目标函数稳定收敛,且具有一定的抗“噪声”干扰性能;与利用速度和加速度信息反演的结果相比,利用位移信息反演的结果具有较高的精度和抗噪声能力.     

Simulation of the full two rigid body problem using polyhedral mutual potential and potential derivatives approach

Herein we investigate the coupled orbital and rotational dynamics of two rigid bodies modelled as polyhedra, under the influence of their mutual gravitational potential. The bodies may possess any arbitrary shape and mass distribution. A method of calculating the mutual potential’s derivatives with respect to relative position and attitude is derived. Relative equations of motion for the two body system are presented and an implementation of the equations of motion with the potential gradients approach is described. Results obtained with this dynamic simulation software package are presented for multiple cases to validate the approach and illustrate its utility. This simulation capability is useful both for addressing questions in dynamical astronomy and for enabling spacecraft missions to binary asteroid systems.