Blazar天体中光学射电大爆发的频谱演化

本文讨论Ｂｌａｚａｒ天体中光学射电大爆发频谱演化的理论模型．考虑沿喷流传播的相对论性激波所注入或加速的相对论性电子，受到康普顿、同步辐射和绝热膨胀三种损耗，并计及相对论电子能谱的高能截断．假定喷流轴线与观测者方向构成很小角度．文中给出了大爆发频谱三阶段连续演化的特性，即康普顿阶段，同步辐射阶段和绝热膨胀阶段的爆发特性．频谱演化用（Ｓｍ－ｖｍ）关系表达（见图２，图中Ｓｍ为频谱反转流量，ｖｍ为反转频率），它与一些Ｂｌａｚａｒ天体中观测到的典型形式相符合．     

IOD Modoki事件对华南后汛期降水异常的影响及可能机理

利用1979—2019年CN05.1中国区域高分辨率降水格点数据、英国Hadley中心观测海温数据、ERA5逐月大气再分析资料及大气环流模式,研究了华南后汛期期间(7—9月)IOD Modoki事件与华南后汛期降水异常的关系及可能机理。观测资料结果表明,华南后汛期降水异常与热带印度洋中部(东和西部)海温异常呈显著正(负)相关关系,表现为印度洋IOD Modoki或印度洋三极子事件的空间分布型。滤除ENSO信号影响后,华南后汛期降水异常仍和IOD Modoki存在较为密切的联系。IOD Modoki正异常对华南后汛期降水异常的影响有以下途径,一方面,异常水汽从热带印度洋东部向西输送至热带中印度洋后,在北半球受科氏力作用向东输送至华南地区,为华南地区提供了充足的水汽条件,并且对华南地区降水正异常的主要水汽辐合贡献为平均水汽的水平扰动散度项和扰动引起的平均水汽垂直平流项。另一方面,热带东南印度洋海温负异常,通过Mastuno-Gill响应引起对流层低层自热带东南印度洋至热带中印度洋有东南风异常,增强了70°E附近的越赤道气流,在北半球向东输送至西北太平洋,这引起了华南地区对流层低层气旋式环流异常。另外,热带东印度洋对流层低(高)层异常辐散(辐合),华南地区低(高)层异常辐合(辐散)增强了东亚地区的局地Hadley环流,有利于华南地区降水的产生。再者,IOD Modoki引起南亚季风区受异常下沉运动控制,并通过季风-荒漠机制引起副热带北大西洋东部、北非荒漠区及地中海西部周围正涡度异常,激发了沿急流向下游传播的准静止Rossby波,增强了日本海高压异常和华南及邻近地区对流层低层气旋式环流异常。上述原因均有利于华南地区降水的产生,反之亦然。上述结果在数值模式中亦得到了验证。     

Characteristics and evolution of lacustrine turbidite of Chang-7 Member of Yanchang Formation in northern Shaanxi

Lacustrine turbidite of Chang-7 Member in the studied area consists of sihstone and fine sandstone with respect to grain size, which is feldspathic lithie sandstone, syrosem arkose and arkose with respect to mineral constitution affected by provenance. There are such apparent signatures as lithology, sedimentary structure, sedimentary sequence and well logs, to recognize turbidite. During the paleogeographic evolution of Chang-7 Member, lake basin and deep lake are both at their maximum extent during Chang-73 stage, resulting in the deposition of Zhangjiatan shale with widespread extent and of turbidite with fragmental-like. Deep lake line is gradually moving toward lake center and turbidite sand bodies are gradually turning better with better lateral continuity, connectivity and more thickness, from stages of Chang-73, Chang-72 and Chang-7t, which can be favorable reservoir in deep-water.     

Environmental evolution of Gongwang Mountains during Holocene in northeastern Yunnan, China

This paper presents the study on two continuous glacio-lacustrine sedimentary deposits, Laotanfang （3 597 m） and Shibantang （3 689 m） located on the southern and northern sides of Hulifang peak in Yunan, China. Environmental change indexes are constructed for each deposit, based on grain size, geochemical and pollen analysis, environmental magnetic susceptibility, and 14C dating. The study of climatic environmental change since the Holocene epoch in this region shows that the climate fluctuated at different stages during the early Holocene, that is, the climate was cool and wet during 8.4-7. 7r ka, cold and wet during 7.7-6. 5 ka, cold and dry during 6. 5-4.7 ka, cool and wet during 4.7-2. 1 ka, warm and wet during 2. 1-1.0 ka, and warmer and wet since 1 ka. These findings reflect the overlapping influences of the southwest and southeast monsoons in different times during the Holocene in the north part of southwestern China are in accord with other Holocene climate change models in this part of China.     

胶州湾女姑山水域夏季赤潮高发期浮游植物群落结构特征

根据 1998年 5～ 8月夏季赤潮高发期间 ,胶州湾女姑山水域浮游植物群落结构的种群组成特征和演替变化对赤潮的发生和种群变动特点进行初步研究。结果表明 ,夏季女姑山水域的浮游植物主要由硅、甲藻组成 ,硅藻在细胞和物种丰度上都占优势。浮游植物优势种在调查期间出现明显的演替现象 ,水温的升高和营养条件的变化是引起物种演替的主要原因。浮游植物细胞丰度在夏季呈明显的增长趋势 ,从 5月份 6.3× 10 5个cell/m3 增至 8月份的 6.7× 10 6个cell/m3 ;其中 ,由于赤潮的爆发 ,细胞丰度的最高峰出现在 7月份 ,为 1.5× 10 7个 /m3 。在赤潮爆发期间 ,赤潮原因种高齿状藻和中肋骨条藻发生了明显的演替现象 ,不同细胞大小的优势种和营养条件的变化是发生物种演替的主要原因。叶绿素a的浓度和细胞丰度的变化共同反映了赤潮发生的全部过程。     

随钻测量、随钻测井与录井工具

摆动阀泥浆脉冲器本身可以产生较高频率的载波,成为高速泥浆脉冲传输的较好选择。由于工作时负载力矩复杂,影响因素众多,为电机输出特性研究带来较大困难。利用在井下工作时的动力学平衡方程,通过水循环实验方式测量得到摆动阀电机在最大转矩比电流控制方式下的位置角度和输出电流数据,进而计算井下工作时电机输出转矩和输出功率,并对其影响因素进行综合分析。结果表明,受惯性转矩、弹性转矩和动态水力转矩的影响,电机输出转矩在不同工作频段表现为不同特征;低频段时,电机输出转矩的变化幅度随载波频率的增大而减小,输出功率随载波频率的增大而缓慢增大;中低频段时,电机输出转矩和输出功率在该频段幅度变化较小,相对比较稳定;高频段时,电机输出转矩和输出功率均随频率的增大而快速增大。可以通过增大扭杆刚度系数和降低摆动阀转子轴系转动惯量的方式降低电机在高频段的输出,以保证电机在额定转矩和额定功率下可以控制摆动阀在井下实现高频快速的摆动,产生稳定高载波频率下的泥浆脉冲压力波形,实现高频载波的目的,为随钻测井数据的高速传输提供了保障。

     

Evidence for chemical evolution in spectra of high redshift galaxies

Using a sample of 57 VLT FORS spectra in the redshift range 1.37< z < 3.40 and a comparison sample with 36 IUE spectra of local ( ) starburst galaxies we derive CIV equivalent width values and estimate metallicities of starburst galaxies as a function of redshift. Assuming that a calibration of the CIV equivalent widths in terms of the metallicity based on the local sample of starburst galaxies is applicable to high-z objects, we find a significant increase of the average metallicities from about 0.16 Z _⊙ at the cosmic epoch corresponding to z ≈ 3.2 to about 0.42 Z _⊙ at z ≈ 2.3. A significant further increase in metallicity during later epochs cannot be detected in our data. Compared to the local starburst galaxies our high-redshift objects tend to be overluminous for a given metallicity. This revised version was published online in August 2006 with corrections to the Cover Date.     

Structure through colour: a pixel approach towards understanding galaxies

We present a study of pixel colour–magnitude diagrams (pCMDs) for a sample of 69 nearby galaxies chosen to span a wide range of Hubble types. Our goal is to determine how useful a pixel approach is for studying galaxies according to their stellar light distributions and content. The galaxy images were analysed on a pixel-by-pixel basis to reveal the structure of the individual pCMDs. We find that the average surface brightness (or projected mass density) in each pixel varies according to galaxy type. Early-type galaxies exhibit a clear 'prime sequence' and some pCMDs of face-on spirals reveal 'inverse-L' structures. We find that the colour dispersion at a given magnitude is found to be approximately constant in early-type galaxies but this quantity varies in the mid and late types. We investigate individual galaxies and find that the pCMDs can be used to pick out morphological features. We discuss the discovery of 'Red Hooks' in the pCMDs of six early-type galaxies and two spirals and postulate their origins. We develop quantitative methods to characterize the pCMDs, including measures of the blue-to-red light ratio and colour distributions of each galaxy and we organize these by morphological type. We compare the colours of the pixels in each galaxy with the stellar population models of Bruzual & Charlot to calculate star formation histories for each galaxy type and compare these to the stellar mass within each pixel. Maps of pixel stellar mass and mass-to-light ratio are compared to galaxy images. We apply the pCMD technique to three galaxies in the Hubble Ultra Deep Field to test the usefulness of the analysis at high redshift. We propose that these results can be used as part of a new system of automated classification of galaxies that can be applied at high redshift.