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451.
E. Pian P. Romano D. Maoz A. Cucchiara C. Pagani V. La Parola 《Monthly notices of the Royal Astronomical Society》2010,401(1):677-686
We have observed four low-luminosity active galactic nuclei (AGNs) classified as type 1 Low-Ionization Nuclear Emission-Line Regions (LINERs) with the X-Ray Telescope (XRT) and the Ultraviolet–Optical Telescope (UVOT) onboard Swift , in an attempt to clarify the main powering mechanism of this class of nearby sources. Among our targets, we detect X-ray variability in NGC 3998 for the first time. The light curves of this object reveal variations of up to 30 per cent amplitude in half a day, with no significant spectral variability on this time-scale. We also observe a decrease of ∼30 per cent over 9 d, with significant spectral softening. Moreover, the X-ray flux is ∼40 per cent lower than observed in previous years. Variability is detected in M81 as well, at levels comparable to those reported previously: a flux increase in the hard X-rays (1–10 keV) of 30 per cent in ∼3 h and variations by up to a factor of 2 within a few years. This X-ray behaviour is similar to that of higher luminosity, Seyfert-type objects. Using previous high-angular-resolution imaging data from the Hubble Space Telescope ( HST ), we evaluate the diffuse UV emission due to the host galaxy and isolate the nuclear flux in our UVOT observations. All sources are detected in the UV band, at levels similar to those of the previous observations with HST . The XRT (0.2–10 keV) spectra are well described by single power laws and the UV-to-X-ray flux ratios are again consistent with those of Seyferts and radio-loud AGNs of higher luminosity. The similarity in X-ray variability and broad-band energy distributions suggests the presence of similar accretion and radiation processes in low- and high-luminosity AGNs. 相似文献
452.
Abderrahim Samaouali Larbi Laânab Mohamed Boukalouch Yves Geraud 《Environmental Earth Sciences》2010,59(6):1171-1181
The objective of this work is to study the decay process involved in the historical Roman Chellah located in the Rabat city
(Morocco). This monument is made up of porous calcarenite stone. Several samples, taken from altered and unaltered blocks,
were analyzed by the water saturation, the mercury intrusion porosimetry techniques and using the scanning electron microscopy
coupled to energy dispersive X-ray spectrometer (SEM–EDX). To perform a reliable chemical analysis, some samples were also
analyzed by inductively coupled plasma-atomic emission spectroscopy (ICP-AES). The mercury porosimetry results show a bimodal
porous network for this porous material, the deterioration process of these stones involved an increase in porous volume of
about 2%. The lowest porosity observed in the unaltered block is connected to the presence of sparitic cement which causes
a partial inter-granular porosity clogging. The highest porosity of the deteriorated block without crust is due to the increase
in inter-granular space. SEM photographs of the unaltered sample show the presence of the porous primary grains, of ovoid
forms and millimeter-length sizes, and of the secondary grains, of rhombohedric forms and micro size. Porosity is essentially
located between the primary grains and can be completely clogged by secondary precipitations. Various forms of deterioration
are observed on the altered samples such as the dissolution of the secondary grains edges, wells of dissolution and also the
presence of argillaceous residues on the surface. This last was also detected by the ICP-AES and EDX analysis which show an
increase of the silicon and aluminum contents toward the surface. 相似文献
453.
Two measures of microbial activity were used to characterise a variety of sediment habitats in three intertidal inlets in the Nelson region, South Island, New Zealand. Rates of microbial mineralisation potential and epibenthic microalgal production were compared with sediment textures, concentrations of photosynthetic pigments, ATP concentrations, and organic and inorganic nutrients. Baseline ranges for these parameters were established for relatively undisturbed estuarine sites for assessing future environmental deterioration and for comparison with sites affected by organic enrichment. Sediment mineralisation rates were increased more than 1000‐fold by enrichment from a fruit processing plant and microalgal production was enhanced by more than 50‐fold at a site exposed to slaughterhouse wastes. The remaining variables, although often strongly correlated with activity measurements, were not as sensitive as measures of enrichment. Sediment microbial activity measurements are proposed as a means of detecting changes in nutrient status of estuarine environments. 相似文献
454.
T.E. Cravens I.P. Robertson R.V. Yelle A.J. Coates K. Agren V. De La Haye F.M. Neubauer 《Icarus》2009,199(1):174-188
Solar and X-ray radiation and energetic plasma from Saturn's magnetosphere interact with the upper atmosphere producing an ionosphere at Titan. The highly coupled ionosphere and upper atmosphere system mediates the interaction between Titan and the external environment. A model of Titan's nightside ionosphere will be described and the results compared with data from the Ion and Neutral Mass Spectrometer (INMS) and the Langmuir probe (LP) part of the Radio and Plasma Wave (RPWS) experiment for the T5 and T21 nightside encounters of the Cassini Orbiter with Titan. Electron impact ionization associated with the precipitation of magnetospheric electrons into the upper atmosphere is assumed to be the source of the nightside ionosphere, at least for altitudes above 1000 km. Magnetospheric electron fluxes measured by the Cassini electron spectrometer (CAPS ELS) are used as an input for the model. The model is used to interpret the observed composition and structure of the T5 and T21 ionospheres. The densities of many ion species (e.g., CH+5 and C2H+5) measured during T5 exhibit temporal and/or spatial variations apparently associated with variations in the fluxes of energetic electrons that precipitate into the atmosphere from Saturn's magnetosphere. 相似文献
455.
Multiple flaring activity in the supergiant fast X-ray transient IGR J08408−4503 observed with Swift
P. Romano L. Sidoli G. Cusumano P. A. Evans L. Ducci H. A. Krimm S. Vercellone K. L. Page A. P. Beardmore D. N. Burrows J. A. Kennea N. Gehrels V. La Parola V. Mangano 《Monthly notices of the Royal Astronomical Society》2009,392(1):45-51
IGR J08408−4503 is a supergiant fast X–ray transient discovered in 2006 with a confirmed association with a O8.5Ib(f) supergiant star, HD 74194. We report on the analysis of two outbursts caught by Swift /Burst Alert Telescope (BAT) on 2006 October 4 and 2008 July 5, and followed up at softer energies with Swift /X-ray Telescope (XRT). The 2008 XRT light curve shows a multiple-peaked structure with an initial bright flare that reached a flux of ∼10−9 erg cm−2 s−1 (2–10 keV), followed by two equally bright flares within 75 ks. The spectral characteristics of the flares differ dramatically, with most of the difference, as derived via time-resolved spectroscopy, being due to absorbing column variations. We observe a gradual decrease in the N H , derived with a fit using absorbed power-law model, as time passes. We interpret these N H variations as due to an ionization effect produced by the first flare, resulting in a significant decrease in the measured column density towards the source. The durations of the flares as well as the times of the outbursts suggest that the orbital period is ∼35 d, if the flaring activity is interpreted within the framework of the Sidoli et al. model with the outbursts triggered by the neutron star passage inside an equatorial wind inclined with respect to the orbital plane. 相似文献
456.
Dante S. LAURETTA Julia S. GOREVA Dolores H. HILL Marvin KILLGORE Alyssa R. La BLUE Andrew CAMPBELL R. C. GREENWOOD A. B. VERCHOVSKY Ian A. FRANCHI 《Meteoritics & planetary science》2009,44(6):823-838
Abstract— We report the results of an extensive study of the Fountain Hills chondritic meteorite. This meteorite is closely related to the CBa class. Mineral compositions and O‐isotopic ratios are indistinguishable from other members of this group. However, many features of Fountain Hills are distinct from the other CB chondrites. Fountain Hills contains 23 volume percent metal, significantly lower than other members of this class. In addition, Fountain Hills contains porphyritic chondrules, which are extremely rare in other CBa chondrites. Fountain Hills does not appear to have experienced the extensive shock seen in other CB chondrites. The chondrule textures and lack of fine‐grained matrix suggests that Fountain Hills formed in a dust‐poor region of the early solar system by melting of solid precursors. Refractory siderophiles and lithophile elements are present in near‐CI abundances (within a factor of two, related to the enhancement of metal). Moderately volatile and highly volatile elements are significantly depleted in Fountain Hills. The abundances of refractory siderophile trace elements in metal grains are consistent with condensation from a gas that is reduced relative to solar composition and at relatively high pressures (10?3bars). Fountain Hills experienced significant thermal metamorphism on its parent asteroid. Combining results from the chemical gradients in an isolated spinel grain with olivine‐spinel geothermometry suggests a peak temperature of metamorphism between 535 °C and 878 °C, similar to type‐4 ordinary chondrites. 相似文献
457.
458.
459.
Decametric storm radiation during the period July–August 1970 has been observed simultaneously with a high sensitivity spectrograph at Arecibo Observatory and with the log-periodic, swept-frequency array of the Clark Lake Radio Observatory. The observations complement each other; different types of fine structure emissions can be easily identified on the spectrograph records and their position can be determined from the swept-frequency recordings. We study the relative positions of the different emissions which have been observed during the storms. Four distinct sources appeared to be present. The continuum emission, the type I bursts and the flare-related type III's were all emitted at different locations. The storm type III bursts, type IIIb's and drift pairs overlapped in position, but appeared at different locations than the previously mentioned sources.On leave of absence from Instituto Argentino de Radioastronomia, Argentina. 相似文献
460.
J. I. García De La Rosa 《Solar physics》1987,112(1):49-58
A study of the observations made on the development and, in some cases, even the decay of 15 large active regions is presented. It is shown that the mature spots result from the subphotospherically controlled attraction of several large fragments of 1–2 × 1021 Mx, which are themselves made of smaller elements. The fragments are more stable structures than the spots they constitute; and usually survive after the spot decay. In the process of coalescence of fragments to form the spot, the fusion is never complete and properly exposed photographs reveal light bridges or saddle-like distributions of umbral dots in the interstices between fragments. These are also the regions along which the break up of the spot occurs. For us, these observations fit within the expectations of the penetrative convection mechanism for umbral dots proposed by Parker (1979b). 相似文献