渤、黄海风生流场季节循环时空模态与变异

根据1978—2015年渤、黄海沿岸观测风应力场与二维非线性垂直平均风生流模式,以及旋转经验正交函数（REOF）、调和分析等方法,研究了渤、黄海月平均风生流速度势、流函数场季节循环时空模态与年际变异.渤、黄海月平均风生流速度势、流函数场主要有两种时空模态,季节周期分量是时空模态的主要分量.由于风应力场季节循环变异,渤海流函数场季节时空循环变异程度大于速度势场,速度势、流函数场第二模态是季节变异的主要分量,黄海速度势场季节时空循环变异程度大于流函数场,速度势场第二模态是季节变异的主要分量.由于月平均风应力场强度年际变化显著线性减弱,渤、黄海季节平均风生流场强度年际变化也显著减弱.渤、黄海暖流与冷水团季节生消是风生流水平环流与垂直对流对冷 暖水体输送与汇集共同作用的结果,渤、黄海春、夏季辐合上升环流延缓及减弱了浅层暖水向深层传播,是春、夏季冷水团与温跃层形成的重要动力因素,因此,速度势是研究渤、黄海风生流场十分重要的因素.冬季渤海中部、黄海东部反气旋型及辐散下沉环流与黄海中部气旋型环流、辐合上升环流是黄海暖流季节转换与强度的主要动力控制因素,夏季黄海东部气旋型环流、辐合上升环流与黄海中部反气旋型环流、辐散下沉环流是黄海冷水团季节转换与强度的主要动力控制因素.     

基于非迭代海-气通量算法的蒸发波导预测模型研究

蒸发波导易发生在海洋等水体之上.为了深入研究蒸发波导预测模型的诊断预报技术,本研究依据目前最新的非迭代海-气通量算法,建立了非迭代通量算法蒸发波导预测模型-NEW模型,进而对新模型进行了敏感性试验,且用我国近海试验数据进行了检验.最后将NEW模型与目前使用广泛、效果较好的4种蒸发波导模型(即P-J模型、Babin模型、NPS模型和伪折射率模型)进行了对比分析,得到了不同模型蒸发波导高度随气象海洋要素变化的规律,结果表明非迭代通量算法模型与传统模型对不同海洋气象要素的敏感性响应是一致的.不稳定层结条件下NEW模型对蒸发波导的诊断结果接近于Babin模型和NPS模型,而稳定条件下略高于NPS模型.试验表明NEW模型可以有效地诊断预报蒸发波导.本研究系统阐述了非迭代通量算法模型的建立和适用情况,为蒸发波导预测诊断算法的更新和模型发展提出了新的思路.     

大亚湾1987年与1989年海水特征的差异

本文利用大亚湾1987年与1989年海洋生态零点调查的资料,对该湾海水特征进行了分析。结果表明,冬季湾内存在着一个反气旋式环流的流动路径;夏季于不同年份该湾底层水向上涌升现的强弱有差异,南海沿岸底层水对大亚湾的入侵是明确的;春夏两季,局部气象条件对湾内的海水特征有明显影响。     

南海某海区海底沉积物物理、声学和弹性性质

报道了南海某海区３个区块海底沉积物若干项声学物理性质，讨论和分析了沉积物的物理力学参数，声学和弹性参数之间的关系。     

Surface circulation derived from drifting buoys in mid- and low-latitude Pacific

1 INTRODUCTION Measuring the velocity of ocean currents is one of the most important tasks in physical oceanography research. Many centuries ago, mariners had begun to obtain the sea surface cur- rents from vessel drift records. As early as in 1870s instr…     

Observational Characteristics of Radio Emission Related to Multi-polar Magnetic Configuration

We present a, large complex radio burst and its associated fast tune structures observed on 2001 April 10 in the frequency range of 0.65-7.6 GHz. The NoRH radio image observation shows very complex radio source structures which include preexisting, newly emerging, submerging/cancelling polarities and a bipolar, a tripolar (a 'bipolar + remote unipolar'), and a quadrupolar structure. This suggests that the radio burst is generated from a very complicated loop structure. According to the spectral and image observations, we assume that the beginning of this flare was caused by a single bipolar loop configuration with a 'Y-type' re-connection structure. A composite of radio continuum and fast time structures is contained in this flare. The various fast radio emission phenomena include normal and reverse drifting type III bursts, and slowly drifting and no-drift structures. The tripolar configurations may form a double-loop with a 'three-legged' structure, which is an important source of the various types of fast time structures. The two-loop reconnection model can lead simultaneously to electron acceleration and corona heating. We have also analyzed the behaviors of coronal magnetic polarities and the emission processes of different types radio emission qualitatively. Interactions of a bipolar or multi-polar loop are consistent with our observational results. Our observations favor the magnetic reconnection configurations of the 'inverted Y-type' (bipolar) and the 'three-legged' structures (tripolar or quadrupolar).     

Two Sympathetic Homologous CMEs on 2002 May 22

Sympathetic coronal mass ejections (CMEs) usually occur in different active regions connected by interconnecting magnetic loops, while homologous CMEs occur within the same active region with an almost the same background magnetic field, and so are similar in shapes. Two sympathetic CMEs erupted within 3 hours on 2002 May 22, originating from the same active region, AR 9948. Their multi-wavelength data were collected and analyzed. It is suggested that emerging flux triggered the occurrence of the first CME and the corresponding flare, the reconnection inflow of which in turn triggered the eruption of the second CME. Based on the fact that the two sympathetic CMEs have many similarities, in their shapes, their low-lying dimming areas, etc., we tentatively propose, for the first time, the phenomenon of sympathetic homologous CMEs.     

A Check on the Cardassian Expansion Model with Type－IaSupernovae Data

We use the magnitude-redshift relation for the type Ia supernova datacompiled by Riess et al. to analyze the Cardassian expansion scenario. This sce-nario assumes the universe to be flat, matter dominated, and accelerating, but contains no vacuum contribution.The best fitting model parameters are H0=65.3kms^-1 Mpc^-1, n= 0.35 and Ω= 0.05. When the highest redshift supernova,SN 1997ck, is excluded, H0 remains the same, but n becomes 0.20 and Ωm, 0.15, and the matter density remains unreasonably low. Our result shows that this particular scenario is strongly disfavoured by the SNeIa data.