螺杆钻侧钻分支绕障技术处理绳索取心钻孔事故

绳索取心钻进施工中常出现卡钻、埋钻和钻具断裂事故。一些孔内事故处理需要很长时间,尤其是深孔事故发生后投入了大量的财力、人力进行处理,最终还不一定能取得成功。在此情况下,采用侧钻绕障而避开孔内事故钻具则是一种理想的选择,可大大缩短事故处理时间,避免钻孔报废带来的损失。重庆北碚龙车勘探区ZK6-2孔运用螺杆定向钻进侧钻分支绕障方法取得成功,并积累了宝贵的经验。     

大型港口集装箱船舶智能配载的集成算法研究

为解决集装箱码头智能化配载多业务规则集成优化问题,提出3层规划框架,重点研究第2层规划方法。该方法对资源分配规则,建立数学模型;对质量匹配规则和胎吊冲突规则,建立逻辑学模型;这些模型均以剪枝条件的形式融入到分支限界搜索中,而剪枝条件的正确性和有效性均有严格的证明保证。对于其它的业务规则,在生成和压缩解空间的过程中就已经充分考虑。同时并不忽略卸货港、尺寸、箱型等重要属性及其对配船位置的限制,实验结果验证算法的有效性。     

A search for magnetic fields in cool sdB stars

Hot cluster horizontal branch (HB) stars and field subdwarf B (sdB) stars are core helium burning stars that exhibit abundance anomalies that are believed to be due to atomic diffusion. Diffusion can be effective in these stars because they are slowly rotating. In particular, the slow rotation of the hot HB stars (T_eff > 11000 K), which show abundance anomalies, contrasts with the fast rotation of the cool HB stars, where the observed abundances are consistent with those of red giants belonging to the same cluster. The reason why sdB stars and hot HB stars are rotating slowly is unknown. In order to assess the possible role of magnetic fields on abundances and rotation, we investigated the occurrence of such fields in sdB stars with T_eff < 30 000 K, whose temperatures overlap with those of the hot HB stars. We conclude that large‐scale organised magnetic fields of kG order are not generally present in these stars but at the achieved accuracy, the possibility that they have fields of a few hundred Gauss remains open. We report the marginal detection of such a field in SB 290; further observations are needed to confirm it (© 2011 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

朝鲜北西部地质构造特征及主要断裂活动性

着重论述了朝鲜北西部五条主要断裂的活动性、简要地叙述了这些断裂的概略特征,认为北东向的鸭绿江东支断裂、清川江断裂为中、晚更新世有活动,早更新世有明显活动的断裂;北西向的载宁江断裂为中更新世有活动,早更新世有明显活动的断裂;在北西西向断裂中,长林断裂为早更新世—上新世活动断裂,南江断裂活动时代不详。其活动性最明显的为鸭绿江东支断裂和载宁江断裂,次为清川江断裂和长林断裂,再是南江断裂。最后,还讨论了这些断裂的形成与演化。     

东北地区地幔热柱构造与成矿成藏作用

东北地区处于古亚洲构造域和西太平洋构造域的叠合部位.该区地幔热柱存在8个地质标志:①南北以西伯利亚板块和华北板块太古代基底(断裂)为界,东西以变质核杂岩体分布为界,基本与日本海毗邻的范围为亚地幔柱的规模;②在佳木斯-牡丹江缝合线内见有科马提岩、苦橄岩,可能为地幔热柱的中心;③水系分布呈放射状及莫霍面分布为松辽盆地幔隆起一致;④典型的热穹隆状态;⑤以花岗岩为主的火成岩省;⑥中生代基性玄武岩基本落入Nb/Ta-Nb图解的地幔柱范围;⑦形成坍塌裂谷特征;⑧岩石圈地幔呈蘑菇云状上涌,地震层析资料证实与太平洋板块俯冲具有相辅相成关系.中生代地幔热柱成矿成藏作用的时空分布具有同时代、同火成岩构造控制,山岭成矿,盆地成藏特征.从He及Ar同位素组成阐明金属矿床与油气田的同源性,分析了幔枝构造是在地表的表现形式,无疑对当今深部找矿及海相油气田的勘查具有理论指导意义.     

The distance to Galactic globular clusters through RR Lyrae pulsational properties

By adopting the same approach outlined by De Santis & Cassisi, we evaluate the absolute bolometric magnitude of the zero-age horizontal branch (ZAHB) at the level of the RR Lyrae variable instability strip in selected Galactic globular clusters. This allows us to estimate the ZAHB absolute visual magnitude for these clusters and to investigate its dependence on the cluster metallicity. The derived M _V (ZAHB)–[Fe/H] relation, corrected in order to account for the luminosity difference between the ZAHB and the mean RR Lyrae magnitude, has been compared with some of the most recent empirical determinations in this field, such as the one provided by Baade–Wesselink analyses, RR Lyrae periods, Hipparcos data for field variables and main-sequence fitting based on Hipparcos parallaxes for field subdwarfs. As a result, our relation provides a clear support to the 'long' distance scale. We discuss also another method for measuring the distance to Galactic globular clusters. This method is quite similar to the one adopted for estimating the absolute bolometric magnitude of the ZAHB but it relies only on the pulsational properties of the Lyrae variables in each cluster. The reliability and accuracy of this method have been tested by applying it to a sample of globular clusters for which, owing to the morphology of their horizontal branch (HB), the use of the commonly adopted ZAHB fitting is a risky procedure. We notice that the two approaches for deriving the cluster distance modulus provide consistent results when applied to globular clusters, the RR Lyrae instability strip is well populated. As the adopted method relies on theoretical predictions on both the fundamental pulsational equation and the allowed mass range for fundamental pulsators, we give an estimate of the error affecting present results, owing to systematic uncertainties in the adopted theoretical framework.