荷载变量相关下直立式防波堤的可靠度

为了探讨独立或相关荷载变量对结构可靠指标(β)值的影响,利用广义随机空间极限状态曲面上任一点处切平面法线来确定可靠指标,从而将在欧洲通用的确定直立式防波堤可靠指标的Hasofer和Lind方法推广至适用于波浪水平力与浮托力之间相关的情况.对一座直立堤实例的核算表明,在变量相关情况下采用改进的JC法或推广的HL法得出可靠指标值符合良好,而荷载相关时的可靠指标值则明显低于假定荷载独立时的结果.     

利用示踪试验时间-浓度曲线分析岩溶管道结构特征

岩溶管道结构特征对岩溶水资源的合理取用、保护及地下工程安全施工均具有重要影响。目前在利用示踪试验曲线分析岩溶管道结构特征时,难以通过曲线叠加、钝锋、不规则上升和下降等形态准确解释多条岩溶管道连接关系、地下湖所处位置和地下水状态。运用地下水溶质运移理论,推导出岩溶管道流溶质运移模型,根据模型绘制三维溶质运移形态和理论时间-浓度曲线,结合水力学相关知识,对岩溶管道连接关系、地下湖位置及岩溶管道流形态变化对应的时间-浓度曲线进行解释。得出以下主要结论：（1）曲线出峰个数对应岩溶管道条数,由于管道径流长度及流速存在差异,双管道并联曲线存在3种模型,分别为2个孤立的单峰、下降曲线存在双峰叠加和2个连续上升的叠加峰;（2）单管道曲线下降梯度个数对应地下湖个数,多管道需结合管道个数和地下湖位置具体分析下降梯度和地下湖个数关系,根据地下湖位置将双管道并联岩溶管道划分4种类型,即地下湖存在于未分支管道、主管道、支管道、主管道和分支管道上;（3）曲线形态极速变化标志着管道流发生表流和承压流的相互转化。研究结果可为岩溶地区地下水保护及地下工程安全建设提供保障。     

黑龙江涌泉地区变质基性火山岩中钠质角闪石的成因及演化

根据野外地质特征确定出黑龙江涌泉地区具有洋壳性质的变质基性火山岩由火山熔岩和火山角砾岩两部分组成。这些基性火山岩至少发生了两期高压变质,两期高压变质形成的钠质角闪石具有不同成因。早期的钠质角闪石与岩石片理明显不协调、无方向性、在岩石中不均匀分布,可能是在佳木斯地块与松嫩地块拼合过程中形成;晚期的钠质角闪石构成了现存片理,可能与后期构造变形有关。由于后期变质、变形作用不均匀及火山角砾岩中物质成份的差异,使得部分火山熔岩和火山角砾岩中的角砾及部分胶结物早期高压变质特征得以保留。根据研究区内及相邻地区绿色片岩特征,确定绿色片岩是由经历高压变质的基性火山岩转变而形成。     

Retention of crab larvae in a coastal null zone

Alongshelf transport in the southern Middle Atlantic Bight is forced by buoyancy-driven currents originating in three large estuaries along the bight. These currents are strongest in the coastal ocean near the southern terminus of each estuary, while the analogous region on the northern side is characterized by weak subtidal flow. We used a combination of field observations and numerical modeling to test the hypothesis that these regions of weak subtidal flow are coastal null zones that serve as retention areas for larvae. The field study consisted of a four-day, shipboard investigation of the distribution of blue crab larvae (Callinectes sapidus) near the mouth of Delaware Bay (39°N, 75°W) in late summer, 2004. Hydrographic surveys of the study site were conducted with a hull-mounted, surface-measuring system. Results showed a sharp boundary between the null zone and the buoyancy-driven current to the south. Blue crab larvae were collected in surface plankton tows along a 30-km transect that encompassed these two areas. Stations with higher densities of larvae were clustered in the null zone during both ebb and flood tides. A numerical model was used to examine the physical mechanisms responsible for the observed distribution. Model results agreed with the field survey and showed that simulated larvae are aggregated in the null zone. The simulations also demonstrated that larvae spawned within the null zone have a much greater probability of settling in juvenile nursery habitat within the bay. The close agreement between field and model results provides consistent support for the hypothesis that coastal null zones associated with the buoyancy-driven circulation of large estuaries may allow retention of larvae in the vicinity of the natal spawning population.     

Optical spectroscopy of novae in M 31

We report results of a spectrophotometric survey of novae in M 31. The observations were carried out using the TNG at La Palma and the 1.82 m telescope of the INAF/OAPD at Asiago observatory. Low resolution spectra of the novae, obtained mainly in the early decline phase, allow us to classify the objects following the Tololo scheme (Williams 1992) (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Populations of supersoft X‐ray sources: Novae,tidal disruption,Type Ia supernovae,accretion‐induced collapse,ionization, and intermediatemass black holes?

Observations of hundreds of supersoft X‐ray sources (SSSs) in external galaxies have shed light on the diversity of the class and on the natures of the sources. SSSs are linked to the physics of Type Ia supernovae and accretion‐induced collapse, ultraluminous X‐ray sources and black holes, the ionization of the interstellar medium, and tidal disruption by supermassive black holes. The class of SSSs has an extension to higher luminosities: ultraluminous SSSs have luminosities above 10³⁹ erg s^–1. There is also an extension to higher energies: quasisoft X‐ray sources (QSSs) emit photons with energies above 1 keV, but few or none with energies above 2 keV. Finally, a significant fraction of the SSSs found in external galaxies switch states between observations, becoming either quasisoft or hard. For many systems “supersoft” refers to a temporary state; SSSs are sources, possibly including a variety of fundamentally different system types, that pass through such a state. We review those results derived from extragalactic data and related theoretical work that are most surprising and that suggest directions for future research (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Supersoft sources in M31: Comparing the XMM‐Newton deep survey,ROSAT and Chandra catalogues

To investigate the transient nature of supersoft sources (SSSs) in M 31, we compared SSS candidates ofthe XMM‐Newton Deep Survey, ROSAT PSPC surveys and the Chandra catalogues in the same field. We found 40 SSSs in the XMM‐Newton observations. While 12 of the XMM‐Newton sources were brighter than the limiting flux of the ROSAT PSPC survey, only two were detected with ROSAT ∼10 yr earlier. Five correlate with recent optical novae which explains why they were not detected by ROSAT. The remaining 28 XMM‐Newton SSSs have fluxes below the ROSAT detection threshold. Nevertheless we found one correlation with a ROSAT source, which had significantly larger fluxes than during the XMM‐Newton observations. Ten of the XMM‐Newton SSSs were detected by Chandra with <1– ∼6yr between the observations. Five were also classified as SSSs by Chandra. Of the 30 ROSAT SSSs three were confirmed with XMM‐Newton, while for 11 sources other classifications are suggested. Of the remaining 16 sources one correlates with an optical nova. Of the 42 Chandra very‐soft sources five are classified as XMM‐Newton SSSs, while for 22 we suggest other classifications. Of the remaining 15 sources, nine are classified as transient by Chandra, one of them correlates with an optical nova. These findings underlined the high variability of the sources of this class and the connection between SSSs and optical novae. Only three sources, were detected by all three missions as SSSs. Thus they are visible for more than a decade, despite their variability (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

On the relation between supersoft X‐ray sources and VY Scl stars: The cases of V504 Cen and VY Scl

We summarise our optical monitoring program of VY Scl stars with the SMARTS telescopes, and triggered X‐ray as well as optical observations after/during state transitions of V504 Cen and VY Scl (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Observational evidence for expansion in the SSS spectra of novae

For several novae, a bright X‐ray source with a spectrum resembling the class of Super Soft X‐ray Sources (SSS) has been observed a few weeks to months after outburst. Novae are powered by explosive nuclear burning on the surface of a white dwarf, and enough energy is produced to power a radiatively driven wind. Owing to the evolution of the opacity of the ejecta, the observable spectrum gradually shifts from optical to soft X‐rays (SSS phase). It has sometimes been assumed that at the beginning of the SSS phase no more mass loss occurs. However, high‐resolution X‐ray spectra of some novae have shown highly blue‐shifted absorption lines, indicating a significant expansion. In this paper, I show that all novae that have been observed with X‐ray gratings during their SSS phase show significant blue shifts. I argue that all models that attempt to explain the X‐ray bright SSS phase have to accommodate the continued expansion of the ejecta (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)