全文获取类型
收费全文 | 523篇 |
免费 | 31篇 |
国内免费 | 2篇 |
专业分类
测绘学 | 36篇 |
大气科学 | 44篇 |
地球物理 | 155篇 |
地质学 | 161篇 |
海洋学 | 31篇 |
天文学 | 86篇 |
综合类 | 3篇 |
自然地理 | 40篇 |
出版年
2023年 | 3篇 |
2022年 | 7篇 |
2021年 | 18篇 |
2020年 | 9篇 |
2019年 | 14篇 |
2018年 | 26篇 |
2017年 | 23篇 |
2016年 | 22篇 |
2015年 | 25篇 |
2014年 | 25篇 |
2013年 | 32篇 |
2012年 | 20篇 |
2011年 | 26篇 |
2010年 | 22篇 |
2009年 | 31篇 |
2008年 | 25篇 |
2007年 | 27篇 |
2006年 | 30篇 |
2005年 | 17篇 |
2004年 | 18篇 |
2003年 | 8篇 |
2002年 | 19篇 |
2001年 | 11篇 |
2000年 | 5篇 |
1999年 | 6篇 |
1998年 | 4篇 |
1996年 | 3篇 |
1995年 | 2篇 |
1994年 | 4篇 |
1993年 | 2篇 |
1986年 | 3篇 |
1984年 | 3篇 |
1983年 | 2篇 |
1982年 | 3篇 |
1981年 | 4篇 |
1980年 | 5篇 |
1979年 | 3篇 |
1978年 | 4篇 |
1976年 | 4篇 |
1975年 | 4篇 |
1974年 | 2篇 |
1971年 | 4篇 |
1967年 | 3篇 |
1966年 | 2篇 |
1965年 | 2篇 |
1963年 | 3篇 |
1962年 | 3篇 |
1959年 | 2篇 |
1958年 | 2篇 |
1957年 | 2篇 |
排序方式: 共有556条查询结果,搜索用时 31 毫秒
71.
72.
Compared to other phytoplankton groups, nitrogen-fixing cyanobacteria generally prefer high water temperatures for growth and are therefore expected to benefit from global warming. We use a coupled biological-physical model with an advanced cyanobacteria life cycle model to compare the abundance of cyanobacteria in the Baltic Sea during two different time periods (1969–1998; 2069–2098). For the latter, we find prolonged growth and a more than twofold increase in the climatologically (30 years) averaged cyanobacteria biomass and nitrogen fixation. Additional sensitivity experiments indicate that the biological-physical feedback mechanism through light absorption becomes more important with global warming. In general, we find a nonlinear response of cyanobacteria to changes in the atmospheric forcing fields as a result of life-cycle related feedback mechanisms. Overall, the sensitivity of the cyanobacteria-driven system suggests that biological-physical and life-cycle related feedback mechanisms are important and must therefore be included in future projection studies. 相似文献
73.
Daniel F. Ryan Aidan M. O’Flannagain Markus J. Aschwanden Peter T. Gallagher 《Solar physics》2014,289(7):2547-2563
We test the compatibility and biases of multi-thermal flare DEM (differential emission measure) peak temperatures determined with AIA with those determined by GOES and RHESSI using the isothermal assumption. In a set of 149 M- and X-class flares observed during the first two years of the SDO mission, AIA finds DEM peak temperatures at the time of the peak GOES 1?–?8 Å flux to have an average of T p=12.0±2.9 MK and Gaussian DEM widths of log10(σ T )=0.50±0.13. From GOES observations of the same 149 events, a mean temperature of T p=15.6±2.4 MK is inferred, which is systematically higher by a factor of T GOES/T AIA=1.4±0.4. We demonstrate that this discrepancy results from the isothermal assumption in the inversion of the GOES filter ratio. From isothermal fits to photon spectra at energies of ?≈6?–?12 keV of 61 of these events, RHESSI finds the temperature to be higher still by a factor of T RHESSI/T AIA=1.9±1.0. We find that this is partly a consequence of the isothermal assumption. However, RHESSI is not sensitive to the low-temperature range of the DEM peak, and thus RHESSI samples only the high-temperature tail of the DEM function. This can also contribute to the discrepancy between AIA and RHESSI temperatures. The higher flare temperatures found by GOES and RHESSI imply correspondingly lower emission measures. We conclude that self-consistent flare DEM temperatures and emission measures require simultaneous fitting of EUV (AIA) and soft X-ray (GOES and RHESSI) fluxes. 相似文献
74.
75.
We describe a forward-fitting method that has been developed to reconstruct hard X-ray images of solar flares from the Ramaty
High-Energy Solar Spectroscopic Imager (RHESSI), a Fourier imager with rotation-modulated collimators that was launched on
5 February 2002. The forward-fitting method is based on geometric models that represent a spatial map by a superposition of
multiple source structures, which are quantified by circular gaussians (4 parameters per source), elliptical gaussians (6
parameters), or curved ellipticals (7 parameters), designed to characterize real solar flare hard X-ray maps with a minimum
number of geometric elements. We describe and demonstrate the use of the forward-fitting algorithm. We perform some 500 simulations
of rotation-modulated time profiles of the 9 RHESSI detectors, based on single and multiple source structures, and perform
their image reconstruction. We quantify the fidelity of the image reconstruction, as function of photon statistics, and the
accuracy of retrieved source positions, widths, and fluxes. We outline applications for which the forward-fitting code is
most suitable, such as measurements of the energy-dependent altitude of energy loss near the limb, or footpoint separation
during flares.
Supplementary material to this paper is available in electronic form at http://dx.doi.org/10.1023/A:1022469811115 相似文献
76.
The recent detection of very-high-energy (GeV – TeV) γ-ray emission from the Galactic black-hole candidate and microquasar LS 5039 has sparked renewed interest in jet models for
the high-energy emission in those objects. In this work, we have focused on models in which the high-energy emission results
from synchrotron and Compton emission by relativistic electrons in the jet (leptonic jet models). Particular attention has
been paid to a possible orbital modulation of the high-energy emission due to azimuthal asymmetries caused by the presence
of the companion star. Both orbital-phase dependentγγ absorption and Compton scattering of optical/UV photons from the companion star may lead to an orbital modulation of the
gamma-ray emission. We make specific predictions which should be testable with refined data from HESS and the upcoming GLAST
mission. 相似文献
77.
Markus Kissler-Patig 《Astrophysics and Space Science》2002,281(1-2):487-491
Old, metal-poor globular clusters trace the formation and evolution of early-type galaxies. Their are the best probes, at
low redshift, of the building-up of galaxy halos at high redshift. Their properties constrain the characteristics of their
progenitors. Recent results suggest that DLAs atz > 3 are the likely hosts for their formation. Finally, they shed light on the old, metal-poor halos probably present around
all early-type galaxies.
This revised version was published online in September 2006 with corrections to the Cover Date. 相似文献
78.
79.
Wolfgang?StinnesbeckEmail author Gerta?Keller Thierry?Adatte Markus?Harting Doris?Stüben Georg?Istrate Utz?Kramar 《International Journal of Earth Sciences》2004,93(6):1042-1065
CSDP core Yaxcopoil-1 was drilled to a depth of 1,511 m within the Chicxulub crater. An organic-rich marly limestone near the base of the hole (1,495 to 1,452 m) was deposited in an open marine shelf environment during the latest Cenomanian (uppermost Rotalipora cushmani zone). The overlying sequence of limestones, dolomites and anhydrites (1,495 to 894 m) indicates deposition in various carbonate platform environments (e.g., sabkhas, lagoons). A 100-m-thick suevite breccia (894–794 m) identifies the Chicxulub impact event. Above the suevite breccia is a dolomitic limestone with planktic foraminiferal assemblages indicative of Plummerita hantkeninoides zone CF1, which spans the last 300 ky of the Maastrichtian. An erosional surface 50 cm above the breccia/dolomite contact marks the K/T boundary and a hiatus. Limestones above this contact contain the first Tertiary planktic foraminifera indicative of an upper P. eugubina zone P1a(2) age. Another hiatus 7 cm upsection separates zone P1a(2) and hemipelagic limestones of planktic foraminiferal Zone P1c. Planktic foraminiferal assemblages of Zone Plc to P3b age are present from a depth of 794.04 up to 775 m. The Cretaceous carbonate sequence appears to be autochthonous, with a stratigraphic sequence comparable to late Cretaceous sediments known from outside the Chicxulub crater in northern and southern Yucatan, including the late Cenomanian organic-rich marly limestone. There is no evidence that these sediments represent crater infill due to megablocks sliding into the crater, such as major disruption of sediments, chaotic changes in lithology, overturned or deep dipping megablocks, major mechanical fragmentation, shock or thermal alteration, or ductile deformation. Breccia units that are intercalated in the carbonate platform sequence are intraformational in origin (e.g., dissolution of evaporites) and dykes are rare. Major disturbances of strata by the impact therefore appear to have been confined to within less than 60 km from the proposed impact center. Yaxcopoil-1 may be located outside the collapsed transient crater cavity, either on the upper end of an elevated and tilted horst of the terrace zone, or even outside the annular crater cavity. The Chicxulub site thus records a large impact that predates the K/T boundary impact and mass extinction. 相似文献
80.
Rainer Kaltenbaek Gerald Hechenblaikner Nikolai Kiesel Oriol Romero-Isart Keith C. Schwab Ulrich Johann Markus Aspelmeyer 《Experimental Astronomy》2012,34(2):123-164
Quantum physics challenges our understanding of the nature of physical reality and of space-time and suggests the necessity of radical revisions of their underlying concepts. Experimental tests of quantum phenomena involving massive macroscopic objects would provide novel insights into these fundamental questions. Making use of the unique environment provided by space, MAQRO aims at investigating this largely unexplored realm of macroscopic quantum physics. MAQRO has originally been proposed as a medium-sized fundamental-science space mission for the 2010 call of Cosmic Vision. MAQRO unites two experiments: DECIDE (DECoherence In Double-Slit Experiments) and CASE (Comparative Acceleration Sensing Experiment). The main scientific objective of MAQRO, which is addressed by the experiment DECIDE, is to test the predictions of quantum theory for quantum superpositions of macroscopic objects containing more than 108 atoms. Under these conditions, deviations due to various suggested alternative models to quantum theory would become visible. These models have been suggested to harmonize the paradoxical quantum phenomena both with the classical macroscopic world and with our notion of Minkowski space-time. The second scientific objective of MAQRO, which is addressed by the experiment CASE, is to demonstrate the performance of a novel type of inertial sensor based on optically trapped microspheres. CASE is a technology demonstrator that shows how the modular design of DECIDE allows to easily incorporate it with other missions that have compatible requirements in terms of spacecraft and orbit. CASE can, at the same time, serve as a test bench for the weak equivalence principle, i.e., the universality of free fall with test-masses differing in their mass by 7 orders of magnitude. 相似文献