海洋功能区划与海洋生态红线关系探讨

海洋生态红线制度是我国"五位一体"文明建设的具体要求。为进一步在自然科学与人文科学的联结点上探求深入开展生态红线工作的可能性,文章对比了实施多年的海洋功能区划与历史新阶段提出的海洋生态保护红线的概念和内涵,剖析了两者之间的区别与联系,指出海洋功能区划与海洋生态红线区划在法律地位和管控制度等方面具有一致性,在划分目标、空间管理及划分方法上具有差异性,海洋功能区划以"使用"为主,海洋生态红线以"保护"引领。在此基础上,建议未来海洋生态红线工作的开展可从海洋功能区划借鉴经验,建立完善的管控评估制度,确立生态保护红线的优先地位,处理好海洋功能区划与海洋生态红线区划的关系。同时,海洋生态红线区划应以维持海洋生态系统结构稳定和提高海洋生态系统服务功能为目标,将区域资源环境承载力评估作为一项参考指标,限制低承载区的开发利用,保证海洋生态环境健康可持续发展。     

Probability Distribution of the Hull Motion and Mooring Line Tension of Two Floating Systems

The statistical and distribution characteristics of the responses of a floater and its mooring lines are essential in designing floating/mooring systems.In general,the dynamic responses of offshore structures obey a Gaussian distribution,assuming that the structural system,and sea loads are linear or weakly nonlinear.However,mooring systems and wave loads are considerably nonlinear,and the dynamic responses of hull/mooring systems are non-Gaussian.In this study,the dynamic responses of two types of floaters,semi-submersible and spar platforms,and their mooring lines are computed using coupled dynamic analysis in the time domain.Herein,the statistical characteristics and distributions of the hull motion and mooring line tension are discussed and compared.The statistical distributions of the dynamic responses have strong non-Gaussianity and are unreasonably fitted by a Gaussian distribution for the two floating and mooring systems.Then,the effects of water depth,wave parameters,and low-frequency and wave-frequency components on the non-Gaussianity of the hull motion,and mooring line tension are investigated and discussed.A comparison of the statistical distributions of the responses with various probability density functions,including the Gamma,Gaussian,General Extreme Value,Weibull,and Gaussian Mixture Model(GMM)distributions,shows that the GMM distribution is better than the others for characterizing the statistical distributions of the hull motion,and mooring line tension responses.Furthermore,the GMM distribution has the best accuracy of response prediction.     

High-resolution H i and radio continuum observations of the SNR G290.1−0.8

We have observed the supernova remnant (SNR) G290.1−0.8 in the 21-cm H  i line and the 20-cm radio continuum using the Australia Telescope Compact Array (ATCA). The H  i data were combined with data from the Southern Galactic Plane Survey to recover the shortest spatial frequencies. In contrast, H  i absorption was analysed by filtering extended H  i emission, with spatial frequencies shorter than 1.1 kλ. The low-resolution ATCA radio continuum image of the remnant shows considerable internal structure, resembling a network of filaments across its 13-arcmin diameter. A high-resolution ATCA radio continuum image was also constructed to study the small-scale structure in the SNR. It shows that there are no structures smaller than ∼17 arcsec, except perhaps for a bright knot to the south, which is probably an unrelated object. The H  i absorption study shows that the gas distribution and kinematics in front of SNR G290.1−0.8 are complex. We estimate that the SNR probably lies in the Carina arm, at a distance 7 (±1) kpc. In addition, we have studied nearby sources in the observed field using archival multiwavelength data to determine their characteristics.     

C-type shocks in the interstellar medium: profiles of CH+ and CH absorption lines

We have computed optical absorption-line profiles of CH⁺ and CH, as predicted by a model of a C-type shock propagating in a diffuse interstellar cloud. Both these species are produced in the shock wave in the reaction sequence that is initiated by C⁺(H₂, H)CH⁺. Whilst CH⁺ flows at the ion speed, CH, which forms in the dissociative recombination reaction CH⁺₃(e⁻, H₂)CH, flows at a speed which is intermediate between those of the ions and the neutrals. The predicted velocity shift between the CH⁺ and CH line profiles is found to be no more than approximately 2 km s⁻¹, which is smaller than has previously been assumed. We also investigate OH and HCO⁺, finding that the correlation between their column densities, recently observed in the diffuse interstellar medium, can be reproduced by the model.     

一种改进的粘土亚塑性本构模型

简要地介绍了Herle和Kolymbas针对黏土建立的亚塑性本构模型的方法。结合黏土的特性以及对响应包络线的分析,详细地列出了HK模型几个尚未解决的问题,并对该模型3个参数分别进行了改进,建立了改进后的HK亚塑性公式以及参数的确定方法。改进后的模型继承了HK模型参数少、易确定以及公式简洁等特点,使HK模型不仅具有严密的数学和力学基础,而且具有较好的实际意义。     

山东省滨海湿地生态价值评估

本文依据Google Earth近2年的遥感影像以及2013年的资源3号卫星影像数据,并结合他人前期研究资料,对山东省滨海湿地的分布和类型进行了研究,使用ArcGIS软件测算出滨海湿地总面积约为5 124km2,其中自然湿地占35.23%,人工湿地占64.77%。根据山东省湿地实际状况,以及湿地的地理位置、成因、水文、生物等要素的差异,将山东省滨海湿地划分为十种类型,并在此基础上,针对滨海湿地不同的生态服务功能类型,采取了不同的方法进行初步价值评估。结果表明,山东省滨海湿地生态服务总价值约3 303亿元,约占山东省2013年GDP的6.04%。其中物质生产价值约占总价值的50.70%,其次为环境调节价值,约占48.24%,社会服务价值只占1.06%。这表明,山东省滨海湿地蕴含较高的经济和生态潜力,能带来较高的经济效益和生态效益,但是社会服务功能价值量相对偏低,有待于进一步重视和开发。     

高力罕凹陷地浸砂岩型铀成矿条件浅析及远景预测

高力罕凹陷为二连盆地乌尼特坳陷的一个组成部分,由有相似构造发育史的分散小湖盆(洼槽)集合而成的沉积盆地。结构复杂,表现出分割性强,多洼槽多沉积中心,岩相变化大的特点。通过对高力罕凹陷的构造特征、结构特征、沉积特征、岩性发育特征及铀成矿条件的分析,认为高力罕凹陷具有良好的铀矿找矿前景。提出该地区的找矿方向,具有一定的参考意义。     

活动星系核与类星体中致密天体的形成与并合：伽玛爆发与引力辐射

频繁的超新星爆发可用以解释活动星系核与类星体的超高金属丰度。星团中的恒星与吸积盘相互作用导致致密天体中子星和黑洞的形成率很高,这些致密天体与红巨星很容易形成双星系统,而后形成（ＮＳ／ＢＨ,ＮＳ／ＢＨ） 双星由于引力辐射最终导致并合而形成伽玛射线爆发。我们估计了伽玛射线爆的爆发频率,发现与观测相符。     

洞庭湖区域雷暴大风分型及预报分析研究

使用S波段双偏振天气雷达资料,对2021年5月15日洞庭湖区一次强对流过程的多单体风暴阶段和飑线阶段分阶段进行了分析,并重点对前阶段的超级单体风暴I2进行了分时段分析,结果表明：(1) I2初始发展时段,水平反射率因子(Z_H)＞55 dBz区域、差分反射率因子(Z_DR)柱(＞2.5 dB)扩展至湿球零度层WBZ高度,对应区域差分相移率(K_DP)较大(＞1.7 °·km^-1)、相关系数CC在0.9~0.99,说明该时段降水相态是以夹杂着大雨滴的水凝物为主。(2) I2冰雹碰并增长时段,Z_H强度和发展高度急速增长,垂直液态水含量VIL出现明显跃增,Z_H强中心(＞60 dBz区域)扩展至-10℃高度以上,对应的Z_DR降至低于0,Z_DR柱(＞2.5 dB)扩展至-10℃高度;CC下降、K_DP出现“空洞”,说明该时段降水以固态粒子为主,且处于增大时段。(3) I2成熟降雹时段,Z_H强中心(＞60 dBz)底部降至WBZ高度以下、CC局部低至0.8、对应区域存在Z_DR负值区、K_DP空洞,说明冰雹下落的拖曳作用削弱上升气流的强度,预示冰雹即将落地。(4)飑线阶段和多单体风暴阶段不同,飑线阶段K_DP值异常偏大、Z_DR大于1。(5)飑线阶段的极端大风发生前,55 dBz强回波、27 m·s^-1速度大值区扩展至1 km以下,强回波区域K_DP明显偏大,与强下沉气流相对应。另外,高空降水粒子在下降过程中融化导致的强降水拖曳作用加剧了极端大风的产生。

     

培育密度和投饵量对长牡蛎壳黑选育品系幼虫生长存活及附着变态的影响

为探究长牡蛎(Crassostrea gigas)壳黑选育品系规模化繁育适宜的培育密度和投饵量,本研究以长牡蛎野生群体幼虫为对照组,分析了不同培育密度(3、7和15个/mL)和不同初始投饵量(0.4、0.8和1.6×10~3cells·ind^-1·d^-1)对长牡蛎壳黑选育品系幼虫生长、存活及附着的影响。研究显示,培育密度和投饵量对长牡蛎幼虫的生长速率、存活率和附着率有显著交互作用(P<0.05)。在培育密度3和7个/mL实验组,长牡蛎幼虫生长速率随投饵量增加而显著增大(P<0.05),并在培育密度7个/mL、投饵量1.6×10~3cells·ind^-1·d^-1实验组达到最大值。而在培育密度15个/mL实验组,投饵量增加对长牡蛎幼虫的生长速率无显著影响(P> 0.05)。且在培育密度15个/mL、投饵量1.6×10~3cells·ind^-1·d^-1实验组长牡蛎壳黑品系幼虫存活率和附着率最低。但在培育密度15个/mL实验组长牡蛎壳黑选育品系幼虫的壳高始终高于野生群体幼虫。且除投饵量0.4×10~3cells·ind^-1·d^-1实验组外,长牡蛎壳黑选育品系幼虫生长速率、存活率和附着率均高于野生群体幼虫。研究结果表明,长牡蛎壳黑选育品系幼虫最适培育条件为培育密度7个/mL、投饵量1.6×10~3cells·ind^-1·d^-1,增加投饵量可促进长牡蛎幼虫生长,但过高的培育密度会与投饵量产生拮抗作用,抑制幼虫生长,不利于幼虫存活和附着。与长牡蛎野生群体相比,壳黑选育品系幼虫能适应更高的培育密度环境,在饵料充足的条件下,其幼虫的生长、存活及附着性状均优于野生群体。