开鲁盆地奈曼凹陷北部地区下白垩统地层剥蚀量恢复及其对油气藏的影响

恢复地层剥蚀厚度是研究盆地演化史和进行油气资源评价的重要基础工作。奈曼凹陷作为开鲁盆地中一个重要的沉积凹陷,整体勘探程度不高。本文运用地震地层厚度趋势法辅之以构造沉积综合法恢复了奈曼凹陷北部地区下白垩统九佛堂组上段和下段的古地层厚度及地层剥蚀量分布范围;同时结合奈曼地区构造演化特征和沉积相特征确定了奈曼凹陷北部地区的沉降中心位于奈10井区域,明确了九佛堂组时期原始沉积相展布特征。在物源供给方面,北部物源受搬运距离远及剥蚀难以存留的影响未能沉积,主要来自于西部陡坡带发育的扇三角洲相沉积及东部缓坡带发育的辫状河三角洲相沉积。此外,研究还发现奈曼凹陷北部地区下白垩统古地层厚度地质模型特征为北东向受抬升剥蚀最严重,剥蚀范围广,剥蚀厚度大。此次研究对于揭示该区域的构造演化历史及油气成藏过程有一定的参考价值。同时,本次研究方法的应用对于类似沉积盆地的剥蚀量恢复研究也具有借鉴意义。

     

History of Star Formation and Chemical Enrichment in the Milky Way Disk

Based on a physical treatment of the star formation law similar to that given by Efstathiou, we have improved our two-component chemical evolution model for the Milky Way disk. Two gas infall rates are compared, one exponential, one Gaussian. It is shown that the star formation law adopted in this paper depends more strongly on the gas surface density than that in Chang et al. It has large effects on the history of star formation and gas evolution of the whole disk. In the solar neighborhood, the history of chemical evolution and star formation is not sensitive to whether the infall rate is Gaussian or exponential. For the same infall time scale, both forms predict the same behavior for the current properties of the Galactic disk. The model predictions do depend on whether or not the infall time scale varies with the radius, but current available observations cannot decide which case is the more realistic. Our results also show that it would be inadequate to describe the gradient evolution along the Gala     

The galaxy luminosity–size relation and selection biases in the Hubble Ultra Deep Field

We use the Hubble Ultra Deep Field to study the galaxy luminosity–size  ( M – R _e )  distribution. With a careful analysis of selection effects due to both detection completeness and measurement reliability, we identify bias-free regions in the   M – R _e   plane for a series of volume-limited samples. By comparison to a nearby survey also having well-defined selection limits, namely the Millennium Galaxy Catalogue, we present clear evidence for evolution in surface brightness since   z ∼ 0.7  . Specifically, we demonstrate that the mean, rest-frame B -band  〈μ〉 _e   for galaxies in a sample spanning 8 mag in luminosity between   M _B =−22  and −14 mag increases by ∼1.0 mag arcsec⁻² from   z ∼ 0.1  to 0.7. We also highlight the importance of considering surface brightness-dependent measurement biases in addition to incompleteness biases. In particular, the increasing, systematic underestimation of Kron fluxes towards low surface brightnesses may cause diffuse, yet luminous, systems to be mistaken for faint, compact objects.     

川西地区近期大地垂直形变场演化与地壳运动特征

本文利用四川西部地区近二十年来的水准资料,分析了该区近期大地垂直形变场演化状况。指出了川西地区自八十年代后期以来继承性构造运动增强,断裂控制区域升、降差异运动加剧的地壳运动特征;同时,鲜水河断裂带之乾宁-康定一带已形成闭锁区。     

半干旱区生态风险时空演变及其影响因素的地理探测——以宁夏盐池县为例

深入探究半干旱区景观格局变化规律,明确其生态风险时空演变特征与影响因素,对优化半干旱区景观格局、防范和治理生态风险、促进区域可持续高质量发展具有重要意义。以宁夏回族自治区盐池县为例,基于2000—2020年土地利用数据,通过景观格局指数构建生态风险模型,结合地统计分析和地理探测器模型,对其景观格局变化及生态风险时空演变与影响因素进行综合研究。结果表明：（1） 2000—2020年盐池县耕地和未利用地面积下降,其余地类均呈增加趋势,其中建设用地扩张速度最快,年均增长率为6.90%。（2） 2000—2020年盐池县景观斑块数、斑块密度、景观形状指数和香浓多样性指数上升,最大斑块指数和蔓延度指数下降,表明景观格局呈破碎化、复杂化和分散化的发展态势。（3） 2000—2020年盐池县生态风险指数由0.1465下降至0.1312,其中高、较高和中等风险区面积占比分别下降5.25%、24.21%和5.44%,而低和较低风险区面积占比分别增加14.11%和20.79%,空间上呈现出北高南低的分布格局。（4） 随着社会需求的日益增长和人类活动的加剧,自然因素对生态风险空间分异格局的影响逐渐弱化,而社会经济因素作用不断增强。     

南疆尼雅地区4000a来的地化元素分布特征与古气候环境演化的初步研究

通过应用因子分析法对尼雅剖面中的多种地化元素和氧化物的分析,在R、Q型因子分析的基础上,提取出古气候信息。初步的研究表明:近4000a来,尼雅地区气候环境仍以干旱化为主,但此期间出现过多次不同程度的干湿变化,大致可分为5个气候期:4.0~3.0kaB P.相对暖干期;3.0~2.2kaB.P.相对冷湿期;2.2~1.6kaB.P.相对暖干期;1.6~1.0kaB.P.相对冷湿期;1.0kaB.P.左右之后的相对暖干期。     

北京市二手房价格时空演变特征

城市住宅价格时空格局及演变特征是衡量城市房地产市场发展均衡性的重要指标。针对海量的互联网实时房产数据,本文构建了一种长时序时空大数据挖掘方法。首先,利用挂牌数据和成交数据,进行了泛在网络地产数据的可用性验证;其次,提出了“混合像元”的多尺度栅格模型,以构建基于栅格系统的房产统计特征描述,形成了多源网络房产数据融合方法;然后分别采用莫兰指数和地理探测器分析房价的空间自相关性和分异性,并基于P-Bshade和邻近栅格时空插值算法解决了稀疏房产数据的融合与插值问题,构建了长时序房地产时空栅格数据库;最后,以北京六环范围内为研究区域,通过栅格区划算法进行了二手房价格时空演变格局的挖掘分析。     

Has the crab pulsar magnetic field grown after its birth?

We investigate the evolution of rotation period and spindown age of a pulsar whose surface magnetic field undergoes a phase of growth. Application of these results to the Crab pulsar strongly indicates that its parameters cannot be accounted for by the field growth theories.