中国石油地质学创新发展论评

石油地质学是国家石油战略的组成部分,是国家石油安全的组成部分,必须予以高度重视。石油地质学来源于实践。但随着石油勘探开发实践的不断深入,仅仅依靠归纳和总结来自实践的认识已经无法满足人们对石油地质学在科学层面的理解和掌握。从沉积层获得的有关构造、生油、储层方面的知识无法全面解释在结晶基底和火山岩中发育油气藏的事实,而最新揭示出金属、非金属矿床、油气藏与深部构造和深部流体存在密切关系,为我们发展石油地质学提供了崭新的思路。欧洲惠更斯号探测器发现土卫六上存在甲烷湖的事实告诉我们,石油地质学的不仅仅是地质学问题,更是天文学问题。所以,及时吸收消化各学科最新成果,创新发展中国石油地质学,已是保障国家石油安全的当务之急。     

一个储量可再生的石油地质模型

最新石油地质基础研究表明,目前正在开采的油气藏可能存在大规模的油气补充,以往勘探地质模型、开发地质模型、三次采油地质模型都没有考虑到储量可增长的因素,可能需要修正。建议国家有关部门设立专项研究,以期为油气勘探开发部署和后期调整提供可靠的地质依据。     

Are There Magnetars in High-mass X-Ray Binaries?

Magnetars form a special population of neutron stars with strong magnetic fields and long spin periods.About 30 magnetars and magnetar candidates known currentl...     

The study of s-process nucleosynthesis based on barium stars, CEMP-s and CEMP-r/s stars

In order to get a broader view of the s-process nucleosynthesis we study the abundance distribution of heavy elements of 35 barium stars and 24 CEMP-stars, including nine CEMP-s stars and 15 CEMP-r/s stars. The similar distribution of [Pb/hs] between CEMP-s and CEMP-r/s stars indicate that the s-process material of both CEMP-s and CEMP-r/s stars should have a uniform origin, i.e. mass transfer from their predominant AGB companions. For the CEMP-r/s stars, we found that the r-process should provide similar proportional contributes to the second s-peak and the third s-peak elements, and also be responsible for the higher overabundance of heavy elements than those in CEMP-s stars. Which hints that the r-process origin of CEMP-r/s stars should be closely linked to the main r-process. The fact that some small r values exist for both barium and CEMP-s stars, implies that the single exposure event of the s-process nucleosynthesis should be general in a wide metallicity range of our Galaxy. Based on the relation between C _r and C _s, we suggest that the origin of r-elements for CEMP-r/s stars have more sources. A common scenario is that the formation of the binary system was triggered by only one or a few supernova. In addition, accretion-induced collapse(AIC) or SN 1.5 should be the supplementary scenario, especially for these whose pre-AGB companion with higher mass and smaller orbit radius, which support the higher values of both C _r and C _s.     

Transient accelerating scalar models with exponential potentials

We study a known class of scalar dark energy models in which the potential has an exponential term and the current accelerating era is transient. We find that, although a decelerating era will return in the future, when extrapolating the model back to earlier stages (z ■ 4), scalar dark energy becomes dominant over matter. So these models do not have the desired tracking behavior, and the predicted transient period of acceleration cannot be adopted into the standard scenario of the Big Bang cosmology. When couplings between the scalar field and matter are introduced, the models still have the same problem; only the time when deceleration returns will be varied. To achieve re-deceleration, one has to turn to alternative models that are consistent with the standard Big Bang scenario.     

Puzzling Origin of CEMP-r/s Stars: An Interpretation of Abundance and Enrichment of s- and r-Process Elements from Asymptotic Giant Branch Supernovae

CEMP-r/s stars at low metallicity are known as double-enhanced stars that show enhancements of both r-process and s-process elements. The chemical abundances of these very metal-poor stars provide us a lot of information for putting new restraints on models of neutron-capture processes. In this article, we put forward an accreted scenario in which the double enrichment of r-process and s-process elements is caused by a former intermediate-mass Asymptotic Giant Branch (AGB) companion in a detached binary system. As the AGB superwind is only present at the ultimate phase of AGB stars, there is thus a lot of potential that the degenerate-core mass of an intermediate-mass AGB star reaches the Chandrasekhar limit before the AGB superwind. In these circumstances, both s-process elements produced in the AGB shell and r-process elements synthesized in the subsequent explosion would be sprayed contemporaneously and accreted by its companion. Despite similarity to physical conditions of a core-collapse supernova, a major focus in this scenario is the degenerate C–O core surrounded by an envelope of a former intermediate-mass AGB donor that may collapse and explode. Due to the existence of an outer envelope, r-process nucleosynthesis is expected to occur. Hypothesizing the material-rich europium (Eu) accreted by the secondary via the wind from the supernova to be in proportion to the geometric fraction of the companion with respect to the exploding donor star, we find that the estimated yield of Eu (as representative of r-process elements) per AGB supernova event is about 1 × 10^?9 M _⊙ ～ 5 × 10^?9 M _⊙. Using the yields of Eu, the overabundance of r-process elements in CEMP-r/s stars can be accounted for. The calculated results show that the value of parameter f , standing for efficiency of wind pollution from the AGB supernova, will reach about 10⁴, which means that the enhanced factor is much larger than unity due to the impact of gravity of the donor and the result of the gravitational focusing effect of the companion.     

Taxonomy,Zonation and Correlation of the Graptolite Fauna across the Lower/Middle Ordovician Boundary Interval in the Yangtze Gorges Area,South China

The graptolite fauna across the Lower and Middle Ordovician boundary at the Huanghuachang GSSP section,Yichang and the Jianyangping section,Xingshan County is described. The taxonomy of the pendent didymograptids,the graptolite zonations across the base of Middle Ordovician and their correlations are discussed in this paper.The two revised graptolite zones,the Didymograptellus bifidus Zone and the Azygograptus suecicus Zone,can be well correlated to their equivalents elsewhere in the world.