全文获取类型
收费全文 | 47678篇 |
免费 | 9458篇 |
国内免费 | 13721篇 |
专业分类
测绘学 | 3763篇 |
大气科学 | 9463篇 |
地球物理 | 11672篇 |
地质学 | 27417篇 |
海洋学 | 6012篇 |
天文学 | 1868篇 |
综合类 | 5037篇 |
自然地理 | 5625篇 |
出版年
2024年 | 301篇 |
2023年 | 1052篇 |
2022年 | 2294篇 |
2021年 | 2696篇 |
2020年 | 2267篇 |
2019年 | 2427篇 |
2018年 | 2823篇 |
2017年 | 2519篇 |
2016年 | 2863篇 |
2015年 | 2505篇 |
2014年 | 3066篇 |
2013年 | 2950篇 |
2012年 | 2977篇 |
2011年 | 3181篇 |
2010年 | 3231篇 |
2009年 | 3109篇 |
2008年 | 2638篇 |
2007年 | 2570篇 |
2006年 | 2291篇 |
2005年 | 2072篇 |
2004年 | 1895篇 |
2003年 | 1579篇 |
2002年 | 1552篇 |
2001年 | 1413篇 |
2000年 | 1495篇 |
1999年 | 1861篇 |
1998年 | 1513篇 |
1997年 | 1590篇 |
1996年 | 1323篇 |
1995年 | 1174篇 |
1994年 | 1092篇 |
1993年 | 986篇 |
1992年 | 786篇 |
1991年 | 548篇 |
1990年 | 379篇 |
1989年 | 400篇 |
1988年 | 336篇 |
1987年 | 236篇 |
1986年 | 184篇 |
1985年 | 143篇 |
1984年 | 104篇 |
1983年 | 85篇 |
1982年 | 87篇 |
1981年 | 60篇 |
1980年 | 58篇 |
1979年 | 46篇 |
1978年 | 17篇 |
1976年 | 9篇 |
1958年 | 32篇 |
1957年 | 9篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
991.
992.
T.H. McConnochie J.F. Bell III D. Savransky M.J. Wolff A.D. Toigo H. Wang M.I. Richardson P.R. Christensen 《Icarus》2010,210(2):545-565
We present measurements of the altitude and eastward velocity component of mesospheric clouds in 35 imaging sequences acquired by the Mars Odyssey (ODY) spacecraft’s Thermal Emission Imaging System visible imaging subsystem (THEMIS-VIS). We measure altitude by using the parallax drift of high-altitude features, and the velocity by exploiting the time delay in the THEMIS-VIS imaging sequence.We observe two distinct classes of mesospheric clouds: equatorial mesospheric clouds observed between 0° and 180° Ls; and northern mid-latitude clouds observed only in twilight in the 200–300° Ls period. The equatorial mesospheric clouds are quite rare in the THEMIS-VIS data set. We have detected them in only five imaging sequences, out of a total of 2048 multi-band equatorial imaging sequences. All five fall between 20° south and 0° latitude, and between 260° and 295° east longitude. The mid-latitude mesospheric clouds are apparently much more common; for these we find 30 examples out of 210 northern winter mid-latitude twilight imaging sequences. The observed mid-latitude clouds are found, with only one exception, in the Acidalia region, but this is quite likely an artifact of the pattern of THEMIS-VIS image targeting. Comparing our THEMIS-VIS images with daily global maps generated from Mars Orbiter Camera Wide Angle (MOC-WA) images, we find some evidence that some mid-latitude mesospheric cloud features correspond to cloud features commonly observed by MOC-WA. Comparing the velocity of our mesospheric clouds with a GCM, we find good agreement for the northern mid-latitude class, but also find that the GCM fails to match the strong easterly winds measured for the equatorial clouds.Applying a simple radiative transfer model to some of the equatorial mesospheric clouds, we find good model fits in two different imaging sequences. By using the observed radiance contrast between cloud and cloud-free regions at multiple visible-band wavelengths, these fits simultaneously constrain the optical depths and particles sizes of the clouds. The particle sizes are constrained primarily by the relative contrasts at the available wavelengths, and are found to be quite different in the two imaging sequences: reff = 0.1 μm and reff = 1.5 μm. The optical depths (constrained by the absolute contrasts) are substantial: 0.22 and 0.5, respectively. These optical depths imply a mass density that greatly exceeds the saturated mass density of water vapor at mesospheric temperatures, and so the aerosol particles are probably composed mainly of CO2 ice. Our simple radiative transfer model is not applicable to twilight, when the mid-latitude mesospheric clouds were observed, and so we leave the properties of these clouds as a question for further work. 相似文献
993.
Using 141 CME-interplanetary shock (CME-IPS) events and foF2 from eight ionosonde stations from January 2000 to September 2005, from the statistical results we find that there is a “same side?–?opposite side effect” in ionospheric negative storms, i.e., a large portion of ionospheric negative disturbances are induced by the same-side events (referring to the CMEs whose source located on the same side of the heliospheric current sheet (HCS) as the Earth), while only a small portion is associated with the opposite-side events (the CMEs source located on the opposite side of the HCS as the Earth); the ratio is 128 vs. 46, and it reaches 41 vs. 14 for the intense ionospheric negative storms. In addition, the ionospheric negative storms associated with the same-side events are often more intense. A comparison of the same-side event (4 April 2000) and the opposite-side event (2 April 2001) shows that the intensity of the ionospheric negative storm caused by the same-side event is higher than that by the opposite-side event, although their initial conditions are quite similar. Our preliminary results show that the HCS has an “impeding” effect to CME-IPS, which results in a shortage of energy injection in the auroral zone and restraining the development of ionospheric negative perturbations. 相似文献
994.
Hu Xiong Wu Xiao-cheng Gong Xiao-yan Wang Xin Xu Qin-chen 《Chinese Astronomy and Astrophysics》2010,34(1):100-112
The technical system of the Sino-Russian joint satellite-to-satellite Mars ionosphere occultation is analyzed and introduced. The analogue computation of the observed values of the radio waves of the ionosphere occultation event is carried out by adopting the three-dimensional ray tracking method and the electron density profile inversion is conducted by means of the simulated occultation observational data, with the result showing that the emulation algorithm is reliable. By taking advantage of the emulation method the case computation and analysis of the inversion errors caused by the observational error of the occultation radio wave phase and the satellite orbital error are respectively carried out, and it is obtained from the result that the effect of the phase measuring error of the 5% circle on the result of the daytime ionosphere occultation exploration may be neglected, while the absolute error of the night electron density measurement is less than 4 × 108 m?3, and the main effect of the satellite orbital error on the occultation leads to the lifting or falling of the ionospheric height. The result shows that the technical system of the Sino-Russian joint Mars ionosphere occultation exploration is advanced. It can be expected that the high accuracy electron density profile is obtained and the technical system can be applied to the exploration of the lunar ionospheric environment. 相似文献
995.
The distribution of black hole spins in consideration of only the effect of merges is discussed. The angular momentum after merging is treated via the post-Newtonian approximation, and the effects of merges under different conditions are simulated by adopting the Monte Carlo method. The obtained results indicate that the major merge cannot make the distribution of black hole spins stable, but the minor merge can make the black hole spin smoothly slow down. The distribution of black hole spins can stay at a stable level with the overwhelming proportion of small spins, when the mass ratio of merging black holes takes the form of power-law function. In addition, based on the simulated results, the possible relationship between radio-loud active galactic nuclei (AGNs) and black hole spins is also discussed. Finally, the distribution of radio loudness is calculated and presented. 相似文献
996.
This article describes a novel algorithm for cosmic‐ray rejection in single spectroscopic CCD images. This algorithm is based on a variation of template matching. It focuses on identifying those pixels belong to spectra, while other conventional algorithms tried to locate the cosmic‐ray hits directly. The main principle is applying template matching to find suspicious blocks, which is followed by surface patching to locate the legitimate pixels accurately. Therefore, the rest pixels are the ones corrupted by cosmic‐ray hits. Meanwhile, almost all the parameters are automatically extracted from the images. Examples of its performance are given for both simulated and observed images. It shows an advantage of significantly low false alarm rate with relatively high detection rate (© 2009 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
997.
998.
水超脉泽辐射( 各向同性光度超过 10 个太阳光度) 通常在星系中心最内部的核区( 小于几个秒差距) 被发现,因而活动星系核被认为是其唯一的能量源。同其它没有检测到水脉泽辐射的活动星系核相比,水脉泽寄主活动星系核可能隐含着某种或某些特殊性质。基于此我们调研了已经公开发表的所有水脉泽源的 X 射线观测情况,得到了一个有 X 射线观测研究结果的子样本( 39 个源) 。由它们的 X 射线光度以及估算的黑洞质量,导出了它们的无量纲吸积率( logL2-10keV /LEdd,其中 L2-10keV和 LEdd分别是 2 - 10keV 的固有光度和爱丁顿光度) ; 与距离范围相当的、没有检测到水脉泽的活动星系核样本相比,发现脉泽寄主活动星系核有较高的吸积率。进一步分析比较这两个活动星系核样本的质量吸积率,也发现类似的趋势。此外,为了探索吸积率和水脉泽辐射间可能的内在联系,我们对它们的脉泽光度和吸积率进行了统计分析,然而结果显示二者之间没有明显的相关性。 相似文献
999.
Wang Shujuan Yan Yihua Zhao Ruizhen Fu Qijun Tan Chengming Xu Long Wang Shijin Lin Huaan 《Solar physics》2001,204(1-2):153-164
25 MHz–7.6 GHz global and detailed (fine structure – FS) radio spectra are presented, which were observed in the NOAA 9077
active region for the Bastille Day (14 July 2000) flare at 10:10–11:00 UT. Besides broadband radio bursts, high-resolution
dynamic spectra reveal metric type II burst, decimetric type IV burst and various decimetric and microwave FSs, such as type III
bursts, type U bursts, reverse-slope (RS)-drifting burst, fiber bursts, patch and drifting pulsation structure (DPS). The
peak-flux-density spectrum of the radio bursts over the range 1.0–7.6 GHz globally appears as a U-shaped signature. Analyzing
the features of backbone and herringbones of the type II burst, the speeds of shock and relevant energetic electron beams
were estimated to be 1100 km s−1 and 58 500 km s−1, respectively. Also the time sequence of the radio emission is analyzed by comparing with the hard X-rays (HXRs) and the
soft X-rays (SXRs) in this flare. After the maxima of the X-rays, the radio emission in the range 1.0–7.6 GHz reached maxima
first at the higher frequency, then drifted to the lower frequency. This comparison suggested that the flare included three
successive processes: firstly the X-rays rose and reached maxima at 10:10–10:23 UT, accompanied by fine structures only in
the range 2.6–7.6 GHz; secondly the microwave radio emission reached maxima accompanied by many fine structures over the range
1.0–7.6 GHz at 10:23–10:34 UT; then a decimetric type IV burst and its associated FSs (fibers) in the range 1.0–2.0 GHz appeared
after 10:40 UT. 相似文献
1000.
五个短蛸群体等位基因酶的遗传变异 总被引:11,自引:1,他引:11
采用水平淀粉凝胶电泳技术研究了山东沿海莱州(LZ),烟台(YT)、青岛(QD),日照(RZ)和大连(DL)五地短蛸自然群体的等位基因酶遗传变异。分析了AAT,ALP,EST,GRS,G6PD,SDH,CAT,SOD,IDH,GPI,PGM,G3PD,MPI,ME,MDH,CK,AK等同工酶在短蛸外套肌和肝脏组织中的表达情况,并对同工酶进行了生化遗传分析,LZ,YT,QD,RZ,DL五个群体的多态位点比例分别为15%,5%,10%,10%,10%(P0.99),群体平均杂合度观测值分别为0.024,0.001,0.009,0.007,0.006,平均位点有效等位基因数分别为1.200,1.022,1.061,1.103,1.077。结果表明,LZ群体的遗传多样性较高,同时,各群体中普遍存在杂合子缺失现象,对五个群体的遗传距离进行聚类分析,构建了系统树图。 相似文献