基于扩展有限元分析的页岩水力压裂裂缝扩展规律探究

水力压裂是开采地下页岩气资源的有效技术手段,探究页岩水力压裂裂缝的扩展规律,可为页岩气的高效开采提供科学的指导依据。通过运用大型有限元软件ABAQUS中的扩展有限元模块,针对不同地应力差工况条件下均质页岩中初始裂缝的位置、方位角、数量和含层理页岩中层理的构造方向、内部倾角、岩性对水力裂缝扩展的影响进行探究。结果表明：对于垂向扩展的水力裂缝,水平主应力增大使裂缝更不易扩展,裂缝扩展长度减小、起裂压力增大;在注液体积流量相同时,向初始裂缝两端同时起裂所形成的水力裂缝长度大于仅向一侧起裂;当初始裂缝处于页岩中部且呈45°方向时,裂缝会向最大水平主应力方向偏转,且偏转程度随最大水平主应力的增大而增大;分时多簇压裂时,裂缝间的扩展会相互干扰,且会较大地影响裂缝扩展的形态和起裂压力,但对裂缝注液点裂缝宽度的影响较小;对于含水平和竖直构造层理的页岩,改变层理内部倾角,水力裂缝会出现不同程度偏转,且其偏转程度随着层理内部倾角的增大而减小;对于含45°方向构造层理的页岩,水力裂缝在层理分别为砂岩、煤岩和泥岩中的偏转程度依次增大,且裂缝偏移比随着最大水平主应力的增大而增大。     

济南四大泉群水化学特征及其成因分析

为明晰济南四大泉群水化学动态变化特征及成因,利用离子比例系数、PHREEQC模拟以及氢氧同位素反演等方法分析各泉群水化学成分特征及其形成过程。研究表明：（1）四大泉群阳离子Ca2+为优势离子,阴离子HCO3-为优势离子;（2）潭西泉和珍珠泉水化学类型稳定,而趵突泉和黑虎泉由HCO3—Ca型变为HCO3·SO4—Ca型;（3）四大泉群受地表水、寒武系凤山组-奥陶系岩溶水以及寒武系张夏组岩溶水混合补给,其中趵突泉、黑虎泉接受寒武系凤山组-奥陶系岩溶水补给占比略大,而潭西泉、珍珠泉接受寒武系张夏组岩溶水补给占比略大;黑虎泉滞留时间最短,循环交替强烈;（4）水岩相互作用强弱程度导致泉群水化学成分差异,溶解沉淀作用强度整体大于阳离子交换作用。趵突泉阳离子交换作用强度最弱,黑虎泉伴随有去白云化作用,潭西泉和珍珠泉水化学作用及强度类似,进一步印证潭西泉和珍珠泉有相同的补给来源及运移机制。该研究成果对水资源合理利用和岩溶大泉的保护具有重要意义。     

涠西南凹陷涠洲10-3油田及围区流三段沉积相研究

为了促进涠西南凹陷涠洲10-3油田及围区流三段油藏的滚动勘探开发,开展了油区沉积相精细研究。利用岩芯、录井、测井和地震等资料,在识别不同级别层序界面和湖泛面的基础上,将涠洲10-3油田及围区流三段划分为2个长期基准面旋回和8个中期基准面旋回,建立了高分辨率层序地层对比格架。在岩芯描述基础上,进行单井沉积相、连井沉积相、平面沉积相分析,认为研究区流三段发育冲积扇、扇三角洲和湖泊3种沉积相,并系统划分了沉积微相类型。探讨了碎屑流沉积的相带归属,将发育在河道中的碎屑流沉积划分为河道型碎屑流沉积,将单独产出的碎屑流沉积根据沉积环境不同划分为水上非河道化碎屑流沉积和水下非河道化碎屑流沉积。最后对各中期基准面旋回的沉积相展布特征和演化规律进行了探讨,并建立了符合研究区的沉积相模式。     

博斯腾湖滨柽柳(Tamarix ramosissina)生长对湖水位的敏感性

基于博斯腾湖1955—2012年湖水位变化资料,利用树木年轮法分析了博斯腾湖年和月水位变化与湖滨柽柳(Tamarix ramosissina)年轮生长关系,利用敏感度指数得出博斯腾湖滨柽柳年轮生长的敏感水位范围。结果表明:(1)1955—2012年博斯腾湖年平均水位经历了3个明显变化阶段,即1955—1987年下降至最低,1987—2002年上升至最高。受向下游生态输水影响,2002—2012年博斯腾湖水位快速下降。输水对博斯腾湖月平均水位和季节性水位变化有影响。(2)博斯腾湖滨柽柳年轮指数与当年的湖水位变化和前1年的湖水位变化均显著相关(p0.05)。柽柳年轮指数与前1年10月至当年4月各个月份的湖水位表现出显著相关(p0.05)。柽柳年轮指数与前1年冬季湖水位相关显著(p0.05),与当年春季3—4月月平均湖水位相关性显著,与当年夏季和秋季湖水位的相关性不显著。(3)博斯腾湖滨柽柳年轮生长对月湖水位变化响应比较敏感。当湖水位在1045.3m时,柽柳年轮指数灵敏度指数(Sk)存在最低值;当湖水位在1 046.3m时,Sk出现最高值。     

k=6,7,8,9的一类新几乎差族

C.Ding和J.Yin推广了几乎差集,定义了新的几乎差族的概念.通过有限域中分圆类的方法给出了几乎差族新的构造方法,并得到了k=6,7,8,9的一类新的几乎差族.     

Investigation on semi-direct and indirect climate effects of fossil fuel black carbon aerosol over China

A Regional Climate Chemistry Modeling System that employed empirical parameterizations of aerosol-cloud microphysics was applied to investigate the spatial distribution, radiative forcing (RF), and climate effects of black carbon (BC) over China. Results showed high levels of BC in Southwest, Central, and East China, with maximum surface concentrations, column burden, and optical depth (AOD) up to 14 μg?m^?3, 8 mg?m^?2, and 0.11, respectively. Black carbon was found to result in a positive RF at the top of the atmosphere (TOA) due to its direct effect while a negative RF due to its indirect effect. The regional-averaged direct and indirect RF of BC in China was about +0.81 and ?0.95 W?m^?2, respectively, leading to a net RF of ?0.15 W?m^?2 at the TOA. The BC indirect RF was larger than its direct RF in South China. Due to BC absorption of solar radiation, cloudiness was decreased by 1.33 %, further resulting in an increase of solar radiation and subsequently a surface warming over most parts of China, which was opposite to BC’s indirect effect. Further, the net effect of BC might cause a decrease of precipitation of ?7.39 % over China. Investigations also suggested large uncertainties and non-linearity in BC’s indirect effect on regional climate. Results suggested that: (a) changes in cloud cover might be more affected by BC’s direct effect, while changes in surface air temperature and precipitation might be influenced by BC’s indirect effect; and (b) BC second indirect effect might have more influence on cloud cover and water content compared to first indirect effect. This study highlighted a substantial role of BC on regional climate changes.     

Estimates of AGN Black Hole Mass and Minimum Variability Timescale

Black hole mass is one of the fundamental physical parameters of active galactic nuclei (AGNs), for which many methods of estimation have been proposed. One set of methods assumes that the broad-line region (BLR) is gravitationally bound by the central black hole potential, so the black hole mass can be estimated from the orbital radius and the Doppler velocity. Another set of methods assumes the observed variability timescale is determined by the orbital timescale near the innermost stable orbit around the Schwarzschild black hole or the Kerr black hole, or by the characteristic timescale of the accretion disk. We collect a sample of 21 AGNs, for which the minimum variability timescales have been obtained and their black hole masses (Mσ) have been well estimated from the stellar velocity dispersion or the BLR size-luminosity relation. Using the minimum variability timescales we estimated the black hole masses for 21 objects by the three different methods, the results are denoted by Ms, Mk and Md, respectively. We compared each of them with Mσindividually and found that: (1) using the minimum variability timescale with the Kerr black hole theory leads to small differences between Mσand Mk, none exceeding one order of magnitude, and the mean difference between them is about 0.53 dex; (2) using the minimum variability timescale with the Schwarzschild black hole theory leads to somewhat larger difference between Mσand Ms: larger than one order of magnitude for 6 of the 21 sources, and the mean difference is 0.74 dex; (3) using the minimum variability timescale with the accretion disk theory leads to much larger differences between Mσand Md, for 13 of the 21 sources the differences are larger than two orders of magnitude; and the mean difference is as high as about 2.01 dex.