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991.
Matthew M. Hedman Joseph A. Burns Mark R. Showalter Philip D. Nicholson Matthew S. Tiscareno Bonnie J. Buratti Roger Clark 《Icarus》2007,188(1):89-107
The Cassini spacecraft has provided the first clear images of the D ring since the Voyager missions. These observations show that the structure of the D ring has undergone significant changes over the last 25 years. The brightest of the three ringlets seen in the Voyager images (named D72), has transformed from a narrow, <40-km wide ringlet to a much broader and more diffuse 250-km wide feature. In addition, its center of light has shifted inwards by over 200 km relative to other features in the D ring. Cassini also finds that the locations of other narrow features in the D ring and the structure of the diffuse material in the D ring differ from those measured by Voyager. Furthermore, Cassini has detected additional ringlets and structures in the D ring that were not observed by Voyager. These include a sheet of material just interior to the inner edge of the C ring that is only observable at phase angles below about 60°. New photometric and spectroscopic data from the ISS (Imaging Science Subsystem) and VIMS (Visual and Infrared Mapping Spectrometer) instruments onboard Cassini show the D ring contains a variety of different particle populations with typical particle sizes ranging from 1 to 100 microns. High-resolution images reveal fine-scale structures in the D ring that appear to be variable in time and/or longitude. Particularly interesting is a remarkably regular, periodic structure with a wavelength of ∼30 km extending between orbital radii of 73,200 and 74,000 km. A similar structure was previously observed in 1995 during the occultation of the star GSC5249-01240, at which time it had a wavelength of ∼60 km. We interpret this structure as a periodic vertical corrugation in the D ring produced by differential nodal regression of an initially inclined ring. We speculate that this structure may have formed in response to an impact with a comet or meteoroid in early 1984. 相似文献
992.
XIA Jiangjiang YAN Zhongwei JIA Gensuo ZENG Heqing Philip Douglas JONES ZHOU Wen ZHANG Anzhi 《大气科学进展》2015,32(6):831-838
It is well-known that global warming due to anthropogenic atmospheric greenhouse effects advanced the start of the vegetation growing season(SOS) across the globe during the 20 th century. Projections of further changes in the SOS for the 21 st century under certain emissions scenarios(Representative Concentration Pathways, RCPs) are useful for improving understanding of the consequences of global warming. In this study, we first evaluate a linear relationship between the SOS(defined using the normalized difference vegetation index) and the April temperature for most land areas of the Northern Hemisphere for 1982–2008. Based on this relationship and the ensemble projection of April temperature under RCPs from the latest state-of-the-art global coupled climate models, we show the possible changes in the SOS for most of the land areas of the Northern Hemisphere during the 21 st century. By around 2040–59, the SOS will have advanced by-4.7 days under RCP2.6,-8.4 days under RCP4.5, and-10.1 days under RCP8.5, relative to 1985–2004. By 2080–99, it will have advanced by-4.3 days under RCP2.6,-11.3 days under RCP4.5, and-21.6 days under RCP8.5. The geographic pattern of SOS advance is considerably dependent on that of the temperature sensitivity of the SOS. The larger the temperature sensitivity,the larger the date-shift-rate of the SOS. 相似文献
993.
994.
Kevin H. Baines Pierre Drossart Miguel A. Lopez-Valverde Sushil K. Atreya Christophe Sotin Thomas W. Momary Robert H. Brown Bonnie J. Buratti Roger N. Clark Philip D. Nicholson 《Planetary and Space Science》2006,54(15):1552-1562
We present a quantitative analysis of CO thermal emissions discovered on the nightside of Titan by Baines et al. [2005. The atmospheres of Saturn and Titan in the near-infrared: First results of Cassini/VIMS. Earth, Moon, and Planets, 96, 119–147]. in Cassini/VIMS spectral imagery. We identify these emission features as the P and R branches of the 1-0 vibrational band of carbon monoxide (CO) near 4.65 μm. For CH3D, the prominent Q branch of the ν2 fundamental band of CH3D near 4.55 μm is apparent. CO2 emissions from the strong v3 vibrational band are virtually absent, indicating a CO2 abundance several orders of magnitude less than CO, in agreement with previous investigations. Analysis of CO emission spectra obtained over a variety of altitudes on Titan's nightside limb indicates that the stratospheric abundance of CO is 32±15 ppm, and together with other recent determinations, suggests a vertical distribution of CO nearly constant at this value from the surface throughout the troposphere to at least the stratopause near 300 km altitude. The corresponding total atmospheric content of CO in Titan is 2.9±1.5×1014 kg. Given the long lifetime of CO in the oxygen-poor Titan atmosphere (0.5–1.0 Gyr), we find a mean CO atmospheric production rate of 6±3×105 kg yr−1. Given the lack of primordial heavy noble gases observed by Huygens [Niemann et al., 2005. The abundances of constituents of Titan's atmosphere from the GCMS on the Huygens probe. Nature, 438, 779–784], the primary source of atmospheric CO is likely surface emissions. The implied CO/CH4 mixing ratio of near-surface material is 1.8±0.9×10−4, based on an average methane surface emission rate over the past 0.5 Gyr of 1.3×10−13 gm cm−2 s−1 as required to balance hydrocarbon haze production via methane photolysis [Wilson and Atreya, 2004. Current state of modeling the photochemistry of Titan's mutually dependent atmosphere and ionosphere. J. Geophys. Res. 109, E06002 Doi:10.1029/2003JE002181]. This low CO/CH4 ratio is much lower than expected for the sub-nebular formation region of Titan and supports the hypothesis [e.g., Atreya et al., 2005. Methane on Titan: photochemical-meteorological-hydrogeochemical cycle. Bull. Am. Astron. Soc. 37, 735] that the conversion of primordial CO and other carbon-bearing materials into CH4-enriched clathrate-hydrates occurs within the deep interior of Titan via the release of hydrogen through the serpentinization process followed by Fischer–Tropsch catalysis. The time-averaged predicted emission rate of methane-rich surface materials is 0.02 km3 yr−1, a value significantly lower than the rate of silicate lava production for the Earth and Venus, but nonetheless indicative of significant active geological processes reshaping the surface of Titan. 相似文献
995.
996.
Elena M. Rossi Philip J. Armitage Tiziana Di Matteo 《Astrophysics and Space Science》2007,311(1-3):185-190
We discuss the physics of the power source for gamma-ray bursts (GRBs). There is a great variety of stellar systems proposed
as progenitors of long and short GRBs, but any current model for the engine ultimately involves the formation of a hyper-accreting
disk around a newly-formed black hole of a few solar masses. The study of such disks can shed light onto the burst composition
and energy content. We present preliminary results from disk vertical structure calculations. These include neutrino transport,
a height-dependent determination of the nuclear composition, and a simplified treatment of turbulent mixing. We find that
vertical mixing is rapid enough to largely erase compositional gradients, and as a consequence the upper layers of the disk
reflect the neutron-rich composition of the midplane close to the black hole. We review the implications of this for the nuclear
composition of outflows in GRBs. Our models suggest an increasing role for pairs in the upper regions of the disk, and we
speculate that a pair-driven wind could be a significant source of cooling.
Elena M. Rossi is a Chandra Fellow 相似文献
997.
The term Tertiary, subdivided into the Paleogene and Neogene, is traditionally used to represent the interval of geological time between the Cretaceous and Quaternary. In the 1990s, however, the Neogene and Paleogene were ratified by the International Union of Geological Sciences as periods/systems of the Cenozoic Era/Erathem, leaving the Tertiary officially undefined. The Tertiary nonetheless remains a formal term that has never been officially eliminated, and its widespread use today implies a long future. 相似文献
998.
Ray P. Norris Steven Tingay Chris Phillips Enno Middelberg Adam Deller Philip N. Appleton 《Monthly notices of the Royal Astronomical Society》2007,378(4):1434-1438
Infrared-Faint Radio Sources represent a new and unexpected class of object which is bright at radio wavelengths but unusually faint at infrared wavelengths. If, like most mJy radio sources, they were either conventional active or star-forming galaxies in the local Universe, we would expect them to be detectable at infrared wavelengths, and so their non-detection by the Spitzer Space Telescope is surprising. Here, we report the detection of one of these sources using very long baseline interferometry, from which we conclude that the sources are driven by active galactic nuclei. We suggest that these sources are either normal radio-loud quasars at high redshift or abnormally obscured radio galaxies. 相似文献
999.
Biodegradation of organic compounds in groundwater can be a significant source of methane in contaminated sites. Methane might accumulate in indoor spaces posing a hazard. The increasing use of ethanol as a gasoline additive is a concern with respect to methane production since it is easily biodegraded and has a high oxygen demand, favoring the development of anaerobic conditions. This study evaluated the use of stable carbon isotopes to distinguish the methane origin between gasoline and ethanol biodegradation, and assessed the occurrence of methane in ethanol fuel contaminated sites. Two microcosm tests were performed under anaerobic conditions: one test using ethanol and the other using toluene as the sole carbon source. The isotopic tool was then applied to seven field sites known to be impacted by ethanol fuels. In the microcosm tests, it was verified that methane from ethanol (δ13C = −11.1‰) is more enriched in 13C, with δ13C values ranging from −20‰ to −30‰, while the methane from toluene (δ13C = −28.5‰) had a carbon isotopic signature of −55‰. The field samples had δ13C values varying over a wide range (−10‰ to −80‰), and the δ13C values allowed the methane source to be clearly identified in five of the seven ethanol/gasoline sites. In the other two sites, methane appears to have been produced from both sources. Both gasoline and ethanol were sources of methane in potentially hazardous concentrations and methane could be produced from organic acids originating from ethanol along the groundwater flow system even after all the ethanol has been completed biodegraded. 相似文献
1000.
Philip E. Hardee 《Astrophysics and Space Science》2004,293(1-2):117-129
The basic theoretical stability properties and normal mode structures of astrophysical jets are reviewed. Simulations designed to examine the nonlinear development of instability and some results from comparison between simulations and theory are presented. The potential use of observed normal mode structures in jets is discussed. 相似文献