新疆哈密黄山─镜儿泉地区金矿床（点）矿物标型特征的研究

本文通过镜下鉴定，结合电子探针分析、Ｘ衍射分析等，总结了研究区各金矿床（点）的矿物物性、成分、分布等特征。矿物学的研究表明，整个成矿过程和构造动力变质密切相关。     

龙口桑岛附近海域表层沉积物分布特征

根据桑岛附近海域184个表层沉积物样品的粒度测量结果,分析了表层沉积物类型、分布特征和粒度参数变化规律,并探讨了影响沉积物分布的主要因素。结果表明,桑岛附近海域表层沉积物主要包括砂质粉砂、砂质砾、砾石等7种类型,砂质粉砂分布广泛,含砾的粗粒沉积物主要分布在桑岛周边近岸,细粒组分高值区主要在远岸地区。沉积物分选程度总体上呈中等,偏态值基本都是正值。桑岛南侧水道和依岛北侧表层沉积物起动流速小于最大潮流流速,潮流作用在此处明显;砂质海岸和桑岛北侧海岸沉积物主要受波浪作用影响。     

平湖油气田低渗透储层测井评价研究

平湖油气田P11储层开发是平湖油气田增储提产的重要目标,也是当前平湖油气田开发面临的难题之一。由于埋藏深,储层物性条件差,试油自然产能低下,储层流体性质复杂,气油比低,凝析油含量高,密度大,储层温度高,压力系数高,给测井解释和评价带来很大困难,对开发方案的实施提出了挑战。根据岩心分析资料,从成岩作用、沉积作用等方面对平湖组放鹤亭P11储层低渗原因进行了分析;对P11储层的测井响应特征进行了总结,对P11储层＂四性＂关系、孔隙度结构进行剖析,对储层孔隙度、渗透率、饱和度等参数进行了研究,得到一套适合P11储层测井解释评价的方法,为P11储层的开发提供参数依据和测井解释服务。     

消频散变换反演海底地声参数

提出1种将消频散变换应用到海底地声参数反演的方法。对单一水听器接收声压信号进行消频散处理后,根据群延时差建立代价函数,反演得到主要海底参数,最后根据贝叶斯统计理论给出了待反演地声参数的边缘后验概率密度。对单层波导进行仿真证明这种新方法的有效性。     

Effects of stocking density on the growth and immunity of Atlantic salmon salmo salar reared in recirculating aquaculture system(RAS)

Atlantic salmon reared in recirculating aquaculture system(RAS) may lead to inappropriately high stocking density, because ?sh live in a limited space. Finding the suitable stocking density of Atlantic salmon reared in RAS is very important for RAS industry. In this paper, the in?uence of stocking density on growth and some stress related physiological factors were investigated to evaluate the ef fects of stocking density. The ?sh were reared for 220 days at ?ve densities(A: 24 kg/m^3; B: 21 kg/m^3; C: 15 kg/m^3; D: 9 kg/m^3 and E: 6 kg/m^3). The results show that 30 kg/m^3 might be the maximum density which RAS can af ford in China. The stocking densities under 30 kg/m^3 have no ef fect on mortality of Atlantic salmon reared in RAS. However, the speci?c growth rate(SGR), ?nal weight and weight gain in the high density group were signi?cantly lower than the lower density groups and middle density groups. Moreover, feed conversion rate(FCR) had a negative correlation with density. Plasma hormone T_3 and GH showed signi?cant decrease with the increase of the stocking density of the experiment. Furthermore, thyroid hormone(T 3), GH(growth hormone) activities were decreased with stocking density increase. However, plasma cortisol, GOT(glutamic oxalacetic transaminase) and GPT(glutamic pyruvic transaminase) activities were increase with stocking density increase. And the stocking density has no ef fects on plasma lysozyme of Atlantic salmon reared in RAS. These investigations would also help devise effcient ways to rear adult Atlantic salmon in China and may, in a way, help spread salmon mariculture in China.     

周期性饥饿对褶皱臂尾轮虫实验种群特征参数的影响

实验设置了一直投喂、周期性饥饿1,2,3,4d和一直饥饿6个处理组,采用轮虫单个体培养,检验周期性饥饿对褶皱臂尾轮虫(Brachionus plicatilis)实验种群特征参数的影响.结果表明:一直投喂组的生殖价最高,对轮虫种群的潜在增长最有利,随饥饿强度的增大,生殖价减小.不同处理下,轮虫个体寿命与其生殖期之间存在显著的正相关(r=0.747).轮虫在受到饥饿后,寿命略有增长,但不同处理对轮虫的平均寿命(10.8~13.1d)和生殖期(6.3~8.3d)均未达到显著差异(P>0.05).饥饿强度增大时,轮虫个体的总产幼数、总产卵量显著下降(P<0.05),产第1幼、最后1幼、第1卵、最后1卵时间显著延长(P<0.05);同时,种群参数的世代时间(T)随饥饿强度增加而增大,内禀增长率(r_m)、周限增长率(λ)和净生殖率(R₀)却明显下降.     

Cosmological constraints from the X-ray gas mass fraction in relaxed lensing clusters observed with Chandra

We present precise measurements of the X-ray gas mass fraction for a sample of luminous, relatively relaxed clusters of galaxies observed with the Chandra observatory, for which independent confirmation of the mass results is available from gravitational lensing studies. Parametrizing the total (luminous plus dark matter) mass profiles using the model of Navarro, Frenk & White, we show that the X-ray gas mass fractions in the clusters asymptote towards an approximately constant value at a radius r ₂₅₀₀, where the mean interior density is 2500 times the critical density of the Universe at the redshifts of the clusters. Combining the Chandra results on the X-ray gas mass fraction and its apparent redshift dependence with recent measurements of the mean baryonic matter density in the Universe and the Hubble constant determined from the Hubble Key Project, we obtain a tight constraint on the mean total matter density of the Universe,     , and measure a positive cosmological constant,     . Our results are in good agreement with recent, independent findings based on analyses of anisotropies in the cosmic microwave background radiation, the properties of distant supernovae, and the large-scale distribution of galaxies.     

The Cepheid period–luminosity zero-point from radial velocities and Hipparcos proper motions

A value for the zero-point (ρ) of the Cepheid period–luminosity relation, <  M _V  >= 2.81 log P  + ρ, is deduced by comparing the value of the Oort constant, A , derived from radial velocities with that derived from Hipparcos proper motions. We find in this way that ρ =−1.47 ± 0.13, in excellent agreement with the value derived from Hipparcos trigonometrical parallaxes, ρ = −1.43 ± 0.10, by Feast &38; Catchpole in a recent paper.     

Composite spectra XIX: HD 208253, a long‐period binary whose hot secondary has enhanced strontium and barium

We separate and analyse the component spectra of the composite‐spectrum binary HD 208253. We find that the cool primary is an evolving star of spectral type G7 III, while its hot secondary is an early‐A dwarf. The giant is currently near the lowest point of the red‐giant branch and is slightly less luminous than its dwarf companion. We provide a set of precise radial‐velocity measurements for both stars. The double‐lined orbit which we derive from them shows that the component mass ratio is close to unity (q = 1.05 ± 0.01). We deduce the physical properties of both stars, determine their respective masses to be 2.75 ± 0.07 Me (giant) and 2.62 ± 0.07 Me (dwarf), and show that the orbit's inclination is within a degree or two of 68°. The spectrum of the A‐type component has quite component has quite narrow lines (we infer a rotational velocity of 18 km s^–1), though since the period of the orbit is well over 1 year that component cannot be in synchronous rotation. An intriguing property of the dwarf is its enhanced Sr and Ba, though it does not exhibit the other spectral peculiarities that would signal a classical Am star. While by no means unique amongst the multitude of oddities exhibited by A and early‐F stars, this dwarf which we have uncovered in a long‐period binary offers valuable constraints and challenges to stellar‐evolution theory. (© 2013 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

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

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.