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61.
东川铜矿床同位素地球化学研究:I.地层年代与铅同位素化探应用 总被引:7,自引:0,他引:7
采用Pb-Pb等时线法测定了昆阳群中亚群落雪组白云岩、黑山组碳质板岩和上亚群大营盘组碳质板岩样品,获得了(1716±56)Ma、(1607±128)Ma和(1258±70)Ma的年龄,确定了昆阳群中亚群时代约为1600—1800Ma,属晚古元古代,上亚群大营盘组约为1200—1300Ma,属中元古代。还应用铅同位素化探技术系统研究了汤丹铜矿1号硐中段西14穿脉岩石-矿石的铅同位素组成,结果表明铅同位素V1值与铜含量呈反相关系。这是运用系统剖面方法开展铅同位素化探的首次尝试。 相似文献
62.
C.J. Clayton 《Organic Geochemistry》1991,17(6)
For modelling isotopic variations in oils it is convenient to differentiate the effects of oil generation ( 100–150°C) from the effects of oil to gas cracking ( 150–180°C). During generation, δ13C of kerogen may increase by up to 1% due to release of isotopically light oil and gas, although most kerogens show little or no chan δ13C of the generated oil increases by between 0 and 1% (av. 0.5%) due to mixing of isotopically heavy oil with an initial isotopically light unbound fraction, possibly of bacterial origin. The change occurs mostly over the first 20% of generation. During oil to gas cracking, kinetic isotope effects become important and the effect on δ13C of the remaining oil can be modelled as a Rayleigh process. δ13C increases by 1.5% by 50% cracking. Insufficient data are available to calibrate the effects at higher levels of cracking, and modelling these variations is hindered by a lack of understanding of the mechanism of pyrobitumen formation. However, increases greater than about 4% are unlikely to be observed. With increasing maturity, the low molecular weight fractions become isotopically heavy faster than the high molecular weight fractions. As a result, any separation of the low molecular weight fraction into a gas phase (“condensate formation”) will produce an isotopic difference between oil and condensate that depends on maturity. In the early stages of generation the condensate may be up to 1% lighter than the remaining oil. With increasing maturity, this difference at first decreases and then increases in the opposite sense. By half way through oil to gas cracking the condensate may be 1.5% heavier than the residual liquid. More subtle rearrangement reactions may result in small, but significant, changes to the shape of the isotope “type-curves” when different oil fractions are compared. 相似文献
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64.
胶南榴辉岩矿物氧同位素平衡及其Sm-Nd年代学制约 总被引:2,自引:4,他引:2
对苏鲁地体中的胶南榴辉岩进行了矿物氧同位素分析,并与同一手标本矿物的Sm-Nd内部等时线定年和Nd-Sr同位素分布进行了对比。研究表明,石榴子石与绿辉石之间的氧同位素平衡与否能够对矿物Sm-Nd同位素体系的平衡状况和内部等时线定年结果的有效性给予直接制约。合理的石榴子石+绿辉石Sm-Nd内部等时线年龄产于两矿物之间达到并在峰变质条件下保持氧同位素平衡的样品中,而两矿物之间处于氧同位素不平衡的样品不能给出正确的Sm-Nd内部等时线年龄。同一矿物在手标本尺度出现显著的O-Nd-Sr同位素不均一性,据此对这些元素在石榴子石和绿辉石中的扩散速率顺序进行了估计,不仅得到了与实验扩散系数相吻合的结果,而且由此估计出在峰变质条件下达到矿物内部同位素均一化所需要的时间应大于10Ma。 相似文献
65.
Early Miocene (ca.?21–18 Ma) volcanism in the Karacada? area comprises three groups of volcanic rocks: (1) calcalkaline suite (andesitic to rhyolitic lavas and their pyroclastics), (2) mildly-alkaline suite (alkali basalt, hawaiite, mugearite, benmoreite and trachydacite), and (3) a single trachyandesitic flow unit. Field observations, 40Ar/39Ar ages and geochemical data show that there was a progressive temporal transition from group 1 to 3 in a post-collisional tectonic setting. The calcalkaline suite rocks with medium-K in composition resemble those of subduction-related lavas, whereas the mildly-alkaline suite rocks having a sodic tendency (Na2O/K2O=1.5–3.2) resemble those of within-plate lavas. Incompatible element and Sr-Nd isotopic characteristics of the suites suggest that the lithospheric mantle beneath the Karacada? area was heterogeneously enriched by two processes before collision: (1) enrichment by subduction-related processes, which is important in the genesis of the calcalkaline volcanism, (2) enrichment by small degree melts from the astenosphere, which dominates the mildly alkaline volcanism. Perturbation of the enriched lithosphere by either delamination following collision and uplift or removal of the subducted slab following subduction and collision (i.e., slab breakoff) is the likely mechanism for the initiation of the post-collision volcanism. 相似文献
66.
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68.
Since 1994, the Rumuruti (R) chondrites have been recognized as a new, well-established chondrite group differing from carbonaceous, ordinary, and enstatite chondrites. The first R chondrite, Carlisle Lakes, was found in Australia in 1977. Meanwhile, the number has increased to 107 (December, 2010). This group is named after the Rumuruti meteorite, the first and so far the only R chondrite fall. Most of the R chondrites are breccias containing a variety of different clasts embedded in a clastic matrix. Some textural and mineralogical characteristics can be summarized as follows: (a) the chondrule abundance in large fragments and in unbrecciated rocks is ∼35–50 vol%; (b) Ca,Al-rich inclusions are rare; (c) the olivine abundance is typically 65–78 vol%; (d) the mean chondrule diameter is ∼400 μm; (e) in unequilibrated R chondrites, low-Ca pyroxene is dominating, whereas in equilibrated R chondrites it is Ca-rich pyroxene; (f) the typical olivine in a metamorphosed lithology is ∼Fa38–40; (g) matrix olivine in unequilibrated, type 3 fragments and rocks has much higher Fa (∼45–60 mol%) compared to matrix olivines in type 4–6 lithologies (∼Fa38–41); (h) spinels have a high TiO2 of ∼5 wt%; (i) abundant different noble metal-bearing phases (metals, sulfides, tellurides, arsenides) occur. The exception is the metamorphosed, type 5/6 R chondrite La Paz Icefield 04840 which contains hornblende, phlogopite, and Ca-poor pyroxene, the latter phase typically occurring in low-grade metamorphosed R chondrites only.In bulk composition, R chondrites have some affinity to ordinary chondrites: (a) the absence of significant depletions in Mn and Na in R chondrites and ordinary chondrites is an important feature to distinguish these groups from carbonaceous chondrites; (b) total Fe (∼24 wt%) of R chondrites is between those of H and L chondrites (27.1 and 21.6 wt%, respectively); (c) the average CI/Mg-normalized lithophile element abundances are ∼0.95 × CI, which is lower than those for carbonaceous chondrites (≥1.0 × CI) and slightly higher than those for ordinary chondrites (∼0.9 × CI); (d) trace element concentrations such as Zn (∼150 ppm) and Se (∼15 ppm) are much higher than in ordinary chondrites; (e) the whole rock Δ17O of ∼2.7 for R chondrites is the highest among all meteorite groups, and the mean oxygen isotope composition is δ17O = 5.36 ± 0.43, δ18O = 5.07 ± 0.86, Δ17O = +2.72 ± 0.31; (f) noble gas cosmic ray exposure ages of R chondrites range between ∼0.1 and ∼70 Ma. More than half of the R chondrites analyzed for noble gases contain implanted solar wind and, thus, are regolith breccias. The 43 R chondrites from Northern Africa analyzed so far for noble gases seem to represent at least 16 falls. Although the data base is still scarce, the data hint at a major collision event on the R chondrite parent body between 15 and 25 Ma ago. 相似文献
69.
70.
广东北部早白垩世粗面岩的成因:Sr-Nd-Pb同位素制约 总被引:2,自引:0,他引:2
广东北部大长沙盆地粗面岩锆石SHRIMP U-Pb年龄为(135.3±1.5) Ma,形成于早白垩世早期,其Sr-Nd-Pb同位素组成为:富放射性成因铅,(206pb/204Pb)i=18.23~18.39,(207pb/204pb )i=15.78~ 15.88,(208Pb/204Pb)i=38.83~39.14,... 相似文献