鲁西隆起与歧口凹陷耦合机制

山区固体矿产地质研究和盆地油气地质研究是地质学两个重要的研究领域,但是由于部门的划分而导致两者研究各有侧重,从而使两者研究的结合和借鉴远远不够。鲁西隆起由南至北分别展布有尼堒山-母子山、蒙山、徂莱山-新甫山-孟良岗、泰山-鲁山-沂山等四个隆起,而隆起之间则分布有泗平、汶蒙、肥城、莱芜等四个相邻的断陷,断陷与隆起之间均发育典型的铲状断裂,并控制着中新世的箕状断陷沉积;而歧口凹陷则以南大港和北大港潜山构造带为界划分为歧南、歧北、板桥三个次级凹陷,它们均呈北侧陡且深、南侧缓而浅的箕状不对称形态,具有"北断南超"的特点。其形态特征完全可以与鲁西隆起区的隆坳构造进行对比。笔者从幔枝构造的视角研究认为它们是鲁西隆起与歧口凹陷之山盆耦合形成的主要构造形迹。     

Vilnius Photometry of Red Giant Stars in the Open Cluster NGC 7789

Photoelectric Vilnius seven-color photometry is presented and analyzed for a sample of 24 red giant branch and clump stars in the open cluster NGC 7789. For each star we have determined photometric spectral type, absolute magnitude, interstellar reddening, effective temperature, metallicity, and surface gravity. From averages over the stars in the sample we find the mean reddening to the cluster E _Y−V = 0.21± 0.02 (s.d.), or E _B−V = 0.25, and the apparent distance modulus (m−M) _V = 12.21± 0.10 (s.d.), which yield a distance of 1840 pc. The mean overall metallicity is found to be [Fe/H] = −0.18± 0.09 (s.d.). The clump stars, on average, appear to be slightly more metal-rich than the other red giants, which is most probably caused by evolutionary changes of carbon and nitrogen molecular bands falling in the photometric passbands. A difference in mass between the two groups of stars has also been detected, which suggests that the clump stars might have undergone extra mass loss before reaching their core He-burning phase of evolution.     

挤扩支盘桩在厂房基础中的应用

结合某厂房桩基工程挤扩支盘桩施工情况,介绍了挤扩支盘桩的施工工艺,根据施工中出现的问题提出了挤扩支盘桩施工时应注意的事项,并对比分析了支盘桩与普通灌注桩的技术经济指标,支盘桩具有明显的优势。     

Expected planets in globular clusters

We argue that all transient searches for planets in globular clusters have a very low detection probability. Planets of low-metallicity stars typically do not reside at small orbital separations. The dependence of planetary system properties on metallicity is clearly seen when the quantity   I _e ≡ M _p[ a (1 − e )]²  is considered;   M _p, a   and e are the planet mass, semimajor axis and eccentricity, respectively. In high-metallicity systems, there is a concentration of systems at high and low values of I _e , with a low-populated gap near   I _e ∼ 0.3 M _J au²  , where M _J is Jupiter's mass. In low-metallicity systems, the concentration is only at the higher range of I _e , with a tail to low values of I _e . Therefore, it is still possible that planets exist around main-sequence stars in globular clusters, although at small numbers because of the low metallicity, and at orbital periods of ≳10 d. We discuss the implications of our conclusions on the role that companions can play in the evolution of their parent stars in globular clusters, for example, influencing the distribution of horizontal branch stars on the Hertzsprung–Russell diagram of some globular clusters, and in forming low-mass white dwarfs.     

The outer-halo globular cluster NGC 6229 – IV. Variable stars

We present time-series B , V photometry of NGC 6229, obtained with the purpose of providing the first extensive CCD variability study of this cluster. As a result, we were able to obtain periods for all NGC 6229 variables, with the exception of five stars from the candidate list of Borissova et al. located very close to the cluster centre. Two stars suspected to be variables by Carney, Fullton and Trammell are first-overtone RR Lyrae (RRc) stars, whereas seven of the 12 candidates of Borissova et al. are confirmed variables – three of them being fundamental RR Lyrae (RRab) pulsators, two first-overtone pulsators, one an eclipsing binary (most likely an Algol system) and one a bright star whose variability status could not be satisfactorily determined. A new image subtraction method (ISM) suggested by Alard has been employed which, together with the Welch–Stetson technique, has allowed us to discover twelve new RR Lyrae variables in the cluster, for which ephemerides are provided. Ten of these are RRabs, whereas the other two are RRcs. As originally suggested by Mayer, NGC 6229 is clearly an Oosterhoff type I globular cluster. We also confirm that V8 is a Population II Cepheid of the W Virginis type, and suspect that this is the case for V22 as well. The physical properties of the NGC 6229 RR Lyrae population are contrasted with those of M3 (NGC 5272) using several different methods, including a standard period-shift analysis. Possible differences between these two clusters are discussed.