南海南部次表层叶绿素a质量浓度最大值及其影响因子*     

廖秀丽  戴明  巩秀玉  刘华雪  黄洪辉 《热带海洋学报》2018,37(1):45-56

文章分析了2013年南海南部4个季节航次的叶绿素a (Chl a)调查数据, 结果显示: 150m以浅水柱Chl a质量浓度均值分别为早春0.14mg•m^-3、初夏0.12mg•m^-3、初秋0.18mg•m^-3、初冬0.16mg•m^-3。早春和初夏偏低的原因与早春风速小, 初夏水温高, 不利于水体的垂直混合, 限制了深层海水中丰富的营养盐向上层水体补充有关。4个季节中海水次表层Chl a质量浓度最大值层(SCML)均出现在50m和75m, 这两个水层的Chl a质量浓度差异小, 季节变化不大, 平均值变化范围分别为0.24~0.26mg•m^-3和0.22~0.26mg•m^-3。受混合层深度和温跃层上界深度的共同影响, 50m水层Chl a质量浓度主要受制于深层富营养盐海水的向上补充, 75m水层Chl a质量浓度受水温的影响明显。  相似文献   

PS测井在机场隧道地基勘查中的应用          下载免费PDF全文

范伟顺 《山东国土资源》2018,34(1)

PS测井技术是地震勘探方法之一,也是一种简便、快速、准确的原位测试技术。该文介绍了单孔法PS测井的原理及其在铁路工程勘察中的应用,主要包括根据等效剪切波,进行建筑抗震场地类别划分,铁路工程抗震场地类别划分。根据岩土动力学参数,达到评价岩体质量和划分围岩类别目的,利用剪切波速法估算岩土的承载力基本值。通过青岛机场隧道场地的工程实例说明了PS测井技术在岩土工程勘察设计中的应用情况及应用效果。  相似文献   

Cosmological constraints from the local X-ray luminosity function of the most X-ray-luminous galaxy clusters     

S. W. Allen  R. W. Schmidt  A. C. Fabian  H. Ebeling 《Monthly notices of the Royal Astronomical Society》2003,342(1):287-298

  相似文献   

Polar shapelets     

Richard Massey  Alexandre Refregier 《Monthly notices of the Royal Astronomical Society》2005,363(1):197-210

  相似文献   

Merging of low-mass systems and the origin of the fundamental plane     

E.A. Evstigneeva  R.R. de Carvalho  A.L. Ribeiro  H.V. Capelato 《Astrophysics and Space Science》2003,284(2):487-490

We present the preliminary results of a study of how small stellar systems merge to form larger ones. As we display the families of galaxies in the μ_e - R_e plane (effective surface brightness versus effective radius) we realize that different morphological types occupy different loci, evidencing the different physical mechanisms operating in each family. As proposed by Capaccioli et al. (1992) this diagram is the logical equivalent of the HR diagram for stars. Here we take some initial steps in understanding of how we can establish the evolutionary tracks, solely due to dynamical processes, in the μ_e - R_e plane, ultimately making a dwarf elliptical to turn into a normal elliptical galaxy. This revised version was published online in August 2006 with corrections to the Cover Date.  相似文献   

小行星(360)Carlova自转参数的测定     

王晓彬  张西亮 《天文学报》2006,47(2):202-211

小行星自转参数的资料不仅可以为小行星碰撞演化提供数据,还可以为太阳系的演化研究提供依据．利用云南天文台1米望远镜对主带碳类小行星(360)Carlova进行了新的CCD测光观测,结合前人的测光资料,利用Epoch-方法对(360)的自转参数进行了反演计算,得到该小行星自转的恒星周期为0．25780417±0．00000003天,自转轴的黄道坐标为(95°±3,°40°±1°)．新的结果与前人的结果相比较为一致,其精度稍高于以前的估算结果．  相似文献   

New evidence for a linear colour–magnitude relation and a single Schechter function for red galaxies in a nearby cluster of galaxies down to M*+ 8     

S. Andreon  J.-C. Cuillandre  E. Puddu  Y. Mellier 《Monthly notices of the Royal Astronomical Society》2006,372(1):60-68

  相似文献   

Erratum: Towards cosmological concordance on galactic scales     

Frank C. van den Bosch  H. J. Mo  Xiaohu Yang 《Monthly notices of the Royal Astronomical Society》2004,348(2):736-736

  相似文献   

WR 7a: a V Sagittae or a qWR star?     

A. S. Oliveira  J. E. Steiner  D. Cieslinski 《Monthly notices of the Royal Astronomical Society》2003,346(3):963-967

The star WR 7a, also known as SPH 2, has a spectrum that resembles that of V Sagittae stars although no O  vi emission has been reported. The Temporal Variance Spectrum – TVS – analysis of our data shows weak but strongly variable emission of O  vi lines which is below the noise level in the intensity spectrum.
Contrary to what is seen in V Sagittae stars, optical photometric monitoring shows very little, if any, flickering. We found evidence of periodic variability. The most likely photometric period is   P _phot= 0.227(±14) d  , while radial velocities suggest a period of   P _spec= 0.204(±13) d  . One-day aliases of these periods can not be ruled out. We call attention to similarities with HD 45166 and DI Cru (= WR 46), where multiple periods are present. They may be associated to the binary motion or to non-radial oscillations.
In contrast to a previous conclusion by Pereira et al., we show that WR 7a contains hydrogen. The spectrum of the primary star seems to be detectable as the N  v 4604 Å  absorption line is visible. If so, it means that the wind is optically thin in the continuum and that it is likely to be a helium main sequence star.
Given the similarity to HD 45166, we suggests that WR 7a may be a qWR – quasi Wolf–Rayet – star. Its classification is WN4h/CE in the Smith, Shara & Moffat three-dimensional classification system.  相似文献   

Measuring shapes of galaxy images – I. Ellipticity and orientation     

Nurur Rahman  Sergei F. Shandarin 《Monthly notices of the Royal Astronomical Society》2003,343(3):933-948

  相似文献