关于Diophantine方程的解     

乐茂华 《广东海洋大学学报》2004,24(4):47-48

对于正整数a ,设S(a)是Smarandache函数。证明了 :方程S(1·2 ) +S(2·3) +… +S(x(x +1) ) =S(x(x +1) (x +2 ) /3)仅有正整数解x =1。  相似文献   

对应分析在法国Douarnenez海湾拟庸鲽食性研究中的应用(Ⅱ)     

林学群  ChristianDENIEL  AlainLAUREC  FranoiseLEMENN 《海洋科学》1994,18(1):29-32

２．４拟庸蝶食性的对应分析２．４．１观察量和变量的分组观察量（捕食鱼类）依不同季节（冬、夏季）、不同性别（雌雄性）和不同性成熟状态（幼鱼和成鱼）来分组，因此得到８（２３）个观察量。对应分析的变量（饵料）首先根据个体生态的不同分为６个类型：游走多毛类，隐居多毛类，双壳类，不大游动的甲壳类（端足目和等足目），爬行甲壳类（十足国短尾部）和棘皮动物。其他６个类型的饵料生物（类、纽虫类、小型游泳甲壳类、腔肠动物、鱼类及苔藓虫类顺在分组时剔除，其原因为它们的出现可能少了些。考虑到捕食鱼类和饵料双壳类贝壳厚度…  相似文献   

南海北部浮游植物生物量的研究特点及影响因素   总被引：8，自引：0，他引：8  

乐凤凤  宁修仁 《海洋学研究》2006,24(2):60-69

介绍了浮游植物生物量变化的研究方法。综述了南海北部浮游植物生物量在营养盐、光照、季风等理化因子影响下出现的变化特点。该海域生态环境复杂,由富营养的珠江口、沿岸带、北部湾和广阔的陆架及贫营养的开阔海区等不同生态区组成,因此浮游植物群落和生物量有其自身复杂的空间和时间变化特点。  相似文献   

数字水准仪标尺编码原理研究     

陈耿彪  WU Jian-zhong  乐韵斐 《测绘学报》2008,37(3):0-402

数字水准仪的标尺编码规则直接影响其测量精度.基于现有几种数字水准仪标尺编码的特点,归纳出标尺条码的编码衡量指标:信息密度、分辨率和纠错能力.以条码的最大编码容量与单个码区长度之比值衡量其承载的信息密度;利用光学系统的点扩散函数研究条码图像的分辨率,即相邻边缘的相互影响,得出码元相邻边缘的间距相等时,影响最小的结论;用相关系数或编码所用函数本身的性质表征条码的纠错能力.依据编码指标建立一套新的标尺编码规则:以格雷码为数值码,固定宽度的码元为参考码,两者交替组合.分析表明,该种编码不但信息密度大,分辨率高,而且纠错能力强.  相似文献   

Isotopic compositions of oxygen, iron, chromium, and nickel in cosmic spherules: Toward a better comprehension of atmospheric entry heating effects     

Cécile Engrand  Kevin D. McKeegan  Gregory F. Herzog  Laurence E. Nyquist 《Geochimica et cosmochimica acta》2005,69(22):5365-5385

Large, correlated, mass-dependent enrichments in the heavier isotopes of O, Cr, Fe, and Ni are observed in type-I (metal/metal oxide) cosmic spherules collected from the deep sea. Limited intraparticle variability of oxygen isotope abundances, typically <5‰ in δ¹⁸O, indicates good mixing of the melts and supports the application of the Rayleigh equation for the calculation of fractional evaporative losses during atmospheric entry. Fractional losses for oxygen evaporation from wüstite, assuming a starting isotopic composition equal to that of air (δ¹⁸O = 23.5‰; δ¹⁷O = 11.8‰), are in the range 55%-77%, and are systematically smaller than evaporative losses calculated for Fe (69%-85%), Cr (81%-95%), and especially Ni (45%-99%). However, as δ¹⁸O values increase, fractional losses for oxygen approach those of Fe, Cr, and Ni indicating a shift in the evaporating species from metallic to oxidized forms as the spherules are progressively oxidized during entry heating. The observed unequal fractional losses of O and Fe can be reconciled by allowing for a kinetic isotope mass-dependent fractionation of atmospheric oxygen during the oxidation process and/or that some metallic Fe may have undergone Rayleigh evaporation before oxidation began.In situ measurements of oxygen isotopic abundances were also performed in 14 type-S (silicate) cosmic spherules, 13 from the Antarctic ice and one from the deep sea. Additional bulk Fe and Cr isotopic abundances were determined for two type-S deep-sea spherules. The isotopic fractionation of Cr isotopes suggest appreciable evaporative loss of Cr, perhaps as a sulfide. The oxygen isotopic compositions for the type-S spherules range from δ¹⁸O = −2‰ to + 27‰. The intraspherule isotopic variations are typically small, ∼5% relative, except for the less-heated porphyritic spherules which have preserved large isotopic heterogeneities in at least one case. A plot of δ¹⁷O vs. δ¹⁸O values for these spherules defines a broad parallelogram bounded at higher values of δ¹⁷O by the terrestrial fractionation line, and at lower values of δ¹⁷O by a line parallel to it and anchored near the isotopic composition of δ¹⁸O = −2.5‰ and δ¹⁷O = −5‰. Lack of independent evidence for substantial evaporative losses suggests that much of this variation reflects the starting isotopic composition of the precursor materials, which likely resembled CO, CM, or CI chondrites. However, the enrichments in heavy isotopes indicate that some mixing with atmospheric oxygen was probably involved during atmospheric entry for some of the spherules. Isotopic fractionation due to evaporation of incoming grain is not required to explain most of the oxygen isotopic data for type-S spherules. However spherules with barred olivine textures that are thought to have experienced a more intense heating than the porphyritic ones might have undergone some distillation. Two cosmic spherules, one classified as a radial pyroxene type and the other showing a glassy texture, show unfractionated oxygen isotopic abundances. They are probably chondrule fragments that survived atmospheric entry unmelted.Possible reasons type-I spherules show larger degrees of isotopic fractionation than type-S spherules include: a) the short duration of the heating pulse associated with the high volatile content of the type-S spherule precursors compared to type-I spherules; b) higher evaporation temperatures for at least a refractory portion of the silicates compared to that of iron metal or oxide; c) lower duration of heating of type-S spherules compared to type-I spherules as a consequence of their lower densities.  相似文献   

南美洲鳗鲡(Anguilla rostrata)的耗氧率(ROC)、窒息点(AP)和适温范围(RT)及对非离子氨(NIA)、NO2-的LC50和SC的研究     

杨小东  江兴龙  乐普敏  龚铭杰 《海洋与湖沼》2019,50(2):455-464

为研究南美洲鳗鲡(Anguillarostrata)的耗氧率及其对水温、低溶氧、非离子氨和亚硝酸盐耐受性,本研究采用自制的鱼类呼吸装置测定其耗氧率和窒息点,以黑仔鳗为试验材料,探索其对水温、非离子氨、亚硝酸盐耐受性。结果表明,南美洲鳗鲡耗氧率存在昼夜变化,其昼间耗氧率为(86.46±37.77)mg/(kgh),夜间耗氧率为(123.58±22.56)mg/(kgh),二者存在显著性差异(P0.05);在15—30°C范围内,耗氧率随温度升高逐渐增大,耗氧率和水温的回归方程y=–0.1316x2+9.4507x–13.712(R2=0.9993);南美洲鳗鲡的耗氧率随体质量增大而降低,耗氧量随体质量增加而增大,耗氧量和体重的回归方程为y=0.2321x0.8334(R2=0.9979);在水温25°C时其窒息点随鱼体质量的增大而降低,均重10g、40g和160g的鳗鲡窒息点溶解氧浓度分别为(0.98±0.25)、(0.46±0.06)和(0.32±0.02)mg/L;13—29°C为南美洲鳗鲡的适温范围,25—29°C为其生长适宜水温,在一定范围内的短时低水温或高水温环境对其损伤是可逆的;水中非离子氨对南美洲鳗鲡的LC50和SC分别为12.22mg/L和1.22mg/L,亚硝酸盐氮对南美洲鳗鲡的LC50和SC分别为61.68mg/L和6.17mg/L。  相似文献   

云南永善县茂林铜矿铜元素赋存状态研究     

慕敏  乐智广  张淼  李佳成 《云南地质》2021,(1):30-36

云南永善县茂林铜矿属于玄武岩型铜矿,品位较低。通过电子探针、化学多元素分析以及光、薄片镜下观察等研究,对矿石的结构、构造,铜矿物在矿石中的赋存状态都有了清楚认识。研究结果显示约68%的铜以独立矿物的形式赋存在赤铜矿和自然铜中,另有32%的铜则以类质同像的形式赋存在绿泥石中。  相似文献   

Integration of remote sensing data into hydrological models for reservoir management     

C. LOUMAGNE  M. NORMAND  M. RIFFARD  A. WEISSE  A. QUESNEY  S. LE HÉGARAT-MASCLE 《水文科学杂志》2013,58(1):89-102

Abstract

The purpose of this paper is to present the methodology set up to derive catchment soil moisture from Earth Observation (EO) data using microwave spaceborne Synthetic Aperture Radar (SAR) images from ERS satellites and to study the improvements brought about by an assimilation of this information into hydrological models. The methodology used to derive EO data is based on the appropriate selection of land cover types for which the radar signal is mainly sensitive to soil moisture variations. Then a hydrological model is chosen, which can take advantage of the new information brought by remote sensing. The assimilation of soil moisture deduced from EO data into hydrological models is based principally on model parameter updating. The main assumption of this method is that the better the model simulates the current hydrological system, the better the following forecast will be. Another methodology used is a sequential one based on Kalman filtering. These methods have been put forward for use in the European AIMWATER project on the Seine catchment upstream of Paris (France) where dams are operated to alleviate floods in the Paris area.  相似文献   

Petrology and Geochemistry of MORB from 25?E to 46?E along the Southwest Indian Ridge: Evidence for Contrasting Styles of Mantle Enrichment     

LE ROEX  ANTON P.; DICK  HENRY J. B.; FISHER  ROBERT L. 《Journal of Petrology》1989,30(4):947-986

The 1984 PROTEA expedition, leg 5, to the central SouthwestIndian Ridge recovered basaltic lavas from fracture zones andridge segments between 25?E and 48?E. In terms of petrographyand major element variations the samples are unremarkable forocean ridge basalts and range from aphyric to highly plagioclasephyric and from primitive (mg-number = 70) to moderately evolved(mg-number = 40) in composition. Multiply saturated (i.e., olivine,plagioclase, and clinopyroxene) basalts are common within thisregion. There is no systematic difference in compositional characteristicsbetween basalts dredged from fracture zone walls and those dredgedfrom ridge segments, and fractional crystallization has playedan important role in controlling the overall range in lava compositionin both tectonic environments. Incompatible element abundance ratios in the basalts are morenotable and distinguish between geochemically depleted (N-type)MORB with high Zr/Nb (1668) and Y/Nb (4?723) ratios and low(La/Sm)^m, ratios (0-?76–1?00), and geochemically enriched(E-type) MORB with low Zr/Nb (3?4–15?8) and Y/Nb (0?5–8?8)and high (La/Sm). ratios (1?07–3?8). N-type MORB appearsto be absent in the immediate vicinity of Marion Island, butoccurs further along the ridge to the northeast and southwest.Geochemically enriched MORB occurs at scattered localities alongthe ridge but is particularly abundant along the section ofthe ridge closest to the Marion hotspot. In detail, two distinct varieties of E-type MORB can be recognized.The one type has incompatible element and isotopic ratios similarto, although slightly less enriched than, those characteristicof the Marion hotspot (Zr/Nb=5?8–8?6; Y/Nb=0?5–0?8;Ba/Nb=5?1–9?0). The second type can be distinguished byhaving high Ba/Nb ratios (9–22), unlike any lavas directlyassociated with the Marion hotspot, but similar to those characteristicof DUPAL ocean island basalts (OIB). A single sample from thisgroup for which there are isotopic data indicates derivationfrom an isotopically anomalous source region. A model is proposed whereby the sub-oceanic mantle below thisportion of the southwest Indian Ocean has experienced at leasttwo distinct enrichment events. The one is associated with theupwelling of the Marion mantle plume (geochemically characterizedby having low Ba/Nb ratios and normal OIB isotopic ratios).The other is associated with upwelling from a DUPAL source (characterizedby having high Ba/Nb ratio and unusual isotopic ratios) whichhas been proposed to exist beneath this portion of the southwestIndian Ocean (Hart, 1984). On the basis of Ba/Nb and Nb/U ratios,recycled oceanic lithosphere is favoured as a source for theMarion hotspot, while recycled oceanic lithosphere plus ancientpelagic sediment appears to be the most likely source for theDUPAL anomaly and the DUPAL E-type MORB in this region.  相似文献   

Noble gas contents of shergottites and implications for the Martian origin of SNC meteorites     

D.D. Bogard  L.E. Nyquist  P. Johnson 《Geochimica et cosmochimica acta》1984,48(9):1723-1739

Isotopic concentrations of the noble gases have been measured in several different phases of Elephant Moraine A79001 and in whole rock samples of Zagami and Allan Hills A77005, three meteorites which belong to the rare group of SNC achondrites that may have originated from the planet Mars. Shocked phases of EETA79001 contain a trapped Ar, Kr, and Xe component characterized by ${}^{84}\text{Kr}{}^{132}\text{Xe}$ ～15, ${}^{40}\text{Ar}{}^{36}\text{Ar}\text{> 2000}$, ${}^{129}\text{Xe}{}^{132}\text{Xe ≥ 2}$, and ${}^4\text{He}{}^{40}\text{Ar}\text{≤ 0.1}$. These elemental and isotopic ratios are unlike those for any other noble gas component except analyses of the Martian atmosphere made by Viking spacecraft. The isotopic composition of the trapped Kr shows an approximate 1% per mass unit enrichment of lighter isotopes compared to terrestrial Kr, and the traped Xe may show either a fission component or a fractionated enrichment of heavier isotopes compared to terrestrial Xe. It is hypothesized that these gases represent a portion of the Martian atmosphere which was shock-implanted into EETA79001, and that they constitute direct evidence of a Martian origin for the shergottite meteorites. Cosmic ray-produced gases in the eight known SNC meteorites form three distinct groups with exposure ages of ～11 MY (Chassigny and the nakhlites), ～2.6 MY (Shergotty, Zagami, and ALHA77005), and ～0.5 MY (EETA79001). These ages suggest three distinct events and cannot have been produced by irradiation for a common time under greatly different shielding. Comparison of cosmogenic ${}^3\text{He}{}^{21}\text{Ne}$ measured in EETA79001 with two independent models for the production of this ratio as a function of shielding indicates that this meteorite was irradiated in space as a relatively small object. If the SNC meteorites were ejected from Mars ～ 180 My ago, the shock age of the shergottites, they must have been relatively large objects (>6 meters diameter) which experienced at least three space collisions to initiate cosmic ray exposure. Ejection from Mars by three events at the times of initiation of cosmic ray exposure would permit the ejected objects to have been much smaller (<1 meter diameter), but would require three such events on 1.3 Gy Martian terraine in the past ～10 MY and would not explain the common 180 MY shock age seen in all four shergottites.  相似文献