全文获取类型
收费全文 | 12438篇 |
免费 | 187篇 |
国内免费 | 116篇 |
专业分类
测绘学 | 266篇 |
大气科学 | 878篇 |
地球物理 | 2389篇 |
地质学 | 4783篇 |
海洋学 | 1247篇 |
天文学 | 2578篇 |
综合类 | 50篇 |
自然地理 | 550篇 |
出版年
2022年 | 150篇 |
2021年 | 233篇 |
2020年 | 222篇 |
2019年 | 248篇 |
2018年 | 547篇 |
2017年 | 457篇 |
2016年 | 511篇 |
2015年 | 220篇 |
2014年 | 445篇 |
2013年 | 654篇 |
2012年 | 488篇 |
2011年 | 603篇 |
2010年 | 598篇 |
2009年 | 689篇 |
2008年 | 617篇 |
2007年 | 612篇 |
2006年 | 535篇 |
2005年 | 358篇 |
2004年 | 343篇 |
2003年 | 301篇 |
2002年 | 295篇 |
2001年 | 260篇 |
2000年 | 268篇 |
1999年 | 174篇 |
1998年 | 192篇 |
1997年 | 178篇 |
1996年 | 115篇 |
1995年 | 138篇 |
1994年 | 122篇 |
1993年 | 102篇 |
1992年 | 80篇 |
1991年 | 101篇 |
1990年 | 102篇 |
1989年 | 70篇 |
1988年 | 79篇 |
1987年 | 100篇 |
1986年 | 80篇 |
1985年 | 111篇 |
1984年 | 97篇 |
1983年 | 106篇 |
1982年 | 87篇 |
1981年 | 82篇 |
1980年 | 98篇 |
1979年 | 88篇 |
1978年 | 87篇 |
1977年 | 77篇 |
1976年 | 59篇 |
1975年 | 64篇 |
1974年 | 72篇 |
1973年 | 64篇 |
排序方式: 共有10000条查询结果,搜索用时 15 毫秒
641.
R. Krivonos A. Tkachenko R. Burenin E. Filippova I. Lapshov I. Mereminskiy S. Molkov M. Pavlinsky S. Sazonov M. Gubarev J. Kolodziejczak S. L. O’Dell D. Swartz Vyacheslav E. Zavlin B. D. Ramsey 《Experimental Astronomy》2017,44(1):147-164
The Astronomical Röntgen Telescope X-ray Concentrator (ART-XC) is a hard X-ray telescope with energy response up to 30 keV, to be launched on board the Spectrum Röntgen Gamma (SRG) spacecraft in 2018. ART-XC consists of seven identical co-aligned mirror modules. Each mirror assembly is coupled with a CdTe double-sided strip (DSS) focal-plane detector. Eight X-ray mirror modules (seven flight and one spare units) for ART-XC were developed and fabricated at the Marshall Space Flight Center (MSFC), NASA, USA. We present results of testing procedures performed with an X-ray beam facility at MSFC to calibrate the point spread function (PSF) of the mirror modules. The shape of the PSF was measured with a high-resolution CCD camera installed in the focal plane with defocusing of 7 mm, as required by the ART-XC design. For each module, we performed a parametrization of the PSF at various angular distances Θ. We used a King function to approximate the radial profile of the near on-axis PSF (Θ < 9 arcmin) and an ellipse fitting procedure to describe the morphology of the far off-axis angular response (9 < Θ < 24 arcmin). We found a good agreement between the seven ART-XC flight mirror modules at the level of 10%. The on-axis angular resolution of the ART-XC optics varies between 27 and 33 arcsec (half-power diameter), except for the spare module. 相似文献
642.
Tongjiang Wang Nelson L. Reginald Joseph M. Davila O. Chris St. Cyr William T. Thompson 《Solar physics》2017,292(8):97
Three-dimensional electron density distributions in the solar corona are reconstructed for 100 Carrington rotations (CR 2054?–?2153) during 2007/03?–?2014/08 using the spherically symmetric method from polarized white-light observations with the inner coronagraph (COR1) onboard the twin Solar Terrestrial Relations Observatory (STEREO). These three-dimensional electron density distributions are validated by comparison with similar density models derived using other methods such as tomography and a magnetohydrodynamics (MHD) model as well as using data from the Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronagraph (LASCO)-C2. Uncertainties in the estimated total mass of the global corona are analyzed based on differences between the density distributions for COR1-A and -B. Long-term variations of coronal activity in terms of the global and hemispheric average electron densities (equivalent to the total coronal mass) reveal a hemispheric asymmetry during the rising phase of Solar Cycle 24, with the northern hemisphere leading the southern hemisphere by a phase shift of 7?–?9 months. Using 14 CR (\(\approx13\)-month) running averages, the amplitudes of the variation in average electron density between Cycle 24 maximum and Cycle 23/24 minimum (called the modulation factors) are found to be in the range of 1.6?–?4.3. These modulation factors are latitudinally dependent, being largest in polar regions and smallest in the equatorial region. These modulation factors also show a hemispheric asymmetry: they are somewhat larger in the southern hemisphere. The wavelet analysis shows that the short-term quasi-periodic oscillations during the rising and maximum phases of Cycle 24 have a dominant period of 7?–?8 months. In addition, it is found that the radial distribution of the mean electron density for streamers at Cycle 24 maximum is only slightly larger (by \(\approx30\%\)) than at cycle minimum. 相似文献
643.
L. O. T. Fernandes P. Kaufmann E. Correia C. G. Giménez de Castro A. S. Kudaka A. Marun P. Pereyra J.-P. Raulin A. B. M. Valio 《Solar physics》2017,292(1):21
Previous sub-THz studies were derived from single-event observations. We here analyze for the first time spectral trends for a larger collection of sub-THz bursts. The collection consists of a set of 16 moderate to small impulsive solar radio bursts observed at 0.2 and 0.4 THz by the Solar Submillimeter-wave Telescope (SST) in 2012?–?2014 at El Leoncito, in the Argentinean Andes. The peak burst spectra included data from new solar patrol radio telescopes (45 and 90 GHz), and were completed with microwave data obtained by the Radio Solar Telescope Network, when available. We critically evaluate errors and uncertainties in sub-THz flux estimates caused by calibration techniques and the corrections for atmospheric transmission, and introduce a new method to obtain a uniform flux scale criterion for all events. The sub-THz bursts were searched during reported GOES soft X-ray events of class C or larger, for periods common to SST observations. Seven out of 16 events exhibit spectral maxima in the range 5?–?40 GHz with fluxes decaying at sub-THz frequencies (three of them associated to GOES class X, and four to class M). Nine out of 16 events exhibited the sub-THz spectral component. In five of these events, the sub-THz emission fluxes increased with a separate frequency from that of the microwave spectral component (two classified as X and three as M), and four events have only been detected at sub-THz frequencies (three classified as M and one as C). The results suggest that the THz component might be present throughout, with the minimum turnover frequency increasing as a function of the energy of the emitting electrons. The peculiar nature of many sub-THz burst events requires further investigations of bursts that are examined from SST observations alone to better understand these phenomena. 相似文献
644.
D. O. Gough 《Solar physics》2017,292(5):70
It has been argued (Gough and McIntyre in Nature 394, 755, 1998) that the only way for the radiative interior of the Sun to be rotating uniformly in the face of the differentially rotating convection zone is for it to be pervaded by a large-scale magnetic field, a field which is responsible also for the thinness of the tachocline. It is most likely that this field is the predominantly dipolar residual component of a tangled primordial field that was present in the interstellar medium from which the Sun condensed (Braithwaite and Spruit in Nature 431, 819, 2004), and that advection by the meridional flow in the tachocline has caused the dipole axis to be inclined from the axis of rotation by about \(60^{\circ}\) (Gough in Geophys. Astrophys. Fluid Dyn., 106, 429, 2012). It is suggested here that, notwithstanding its turbulent passage through the convection zone, a vestige of that field is transmitted by the solar wind to Earth, where it modulates the geomagnetic field in a periodic way. The field variation reflects the inner rotation of the Sun, and, unlike turbulent-dynamo-generated fields, must maintain phase. I report here a new look at an earlier analysis of the geomagnetic field by Svalgaard and Wilcox (Solar Phys. 41, 461, 1975), which reveals evidence for appropriate phase coherence, thereby adding support to the tachocline theory. 相似文献
645.
The preflare phase of the flare SOL2011-08-09T03:52 is unique in its long duration, in that it was covered by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Nobeyama Radioheliograph, and because it showed three well-developed soft X-ray (SXR) peaks. No hard X-rays (HXR) are observed in the preflare phase. Here we report that no associated radio emission at 17 GHz was found either, despite the higher sensitivity of the radio instrument. The ratio between the SXR peaks and the upper limit of the radio peaks is higher by more than one order of magnitude than the ratio in regular flares. The result suggests that the ratio between acceleration and heating in the preflare phase was different than in regular flares. Acceleration to relativistic energies, if any, occurred with lower efficiency. 相似文献
646.
We suggest a method and build a model of radio galaxy distribution over the sphere using data from the WENSS catalogs and standard radio count models by Condon. We calculate the angular power spectrum of the contribution of extended radio galaxies into the microwave background and show that it can be a distorting factor for correct estimation of the angular spectrum from the signal determined by the Sunyaev–Zeldovich effect. 相似文献
647.
A. N. Sarkisyan A. S. Vinokurov Yu. N. Solovieva O. N. Sholukhova A. E. Kostenkov S. N. Fabrika 《Astrophysical Bulletin》2017,72(4):486-501
We present a code for the optimal extraction of long-slit 2D spectra in crowded stellar fields. Its main advantage and difference from the existing spectrum extraction codes is the presence of a graphical user interface (GUI) and a convenient visualization system of data and extraction parameters. On the whole, the package is designed to study stars in crowded fields of nearby galaxies and star clusters in galaxies. Apart from the spectrum extraction for several stars which are closely located or superimposed, it allows the spectra of objects to be extracted with subtraction of superimposed nebulae of different shapes and different degrees of ionization. The package can also be used to study single stars in the case of a strong background. In the current version, the optimal extraction of 2D spectra with an aperture and the Gaussian function as PSF (point spread function) is proposed. In the future, the package will be supplemented with the possibility to build a PSF based on a Moffat function. We present the details of GUI, illustrate main features of the package, and show results of extraction of the several interesting spectra of objects from different telescopes. 相似文献
648.
S. N. Kulichkov I. P. Chunchuzov O. I. Popov 《Izvestiya Atmospheric and Oceanic Physics》2010,46(1):60-68
The results of simulating the influence of an atmospheric fine structure on the characteristics of acoustic signals propagating
throughout the atmosphere for long distances from their sources are presented. A numerical model of an atmospheric fine inhomogeneous
structure within the height range z = 20…120 km is proposed to perform calculations. This model and its numerical parameters are based on the current notions
of the formation of an atmospheric fine structure due to internal gravity waves. The numerical calculations were performed
using the parabolic-equation method. A spatial structure of the acoustic field and the structure of an acoustic signal at
long distances from a pulsed source were calculated. It is shown that the presence of an atmospheric fine structure results
in a scattering of acoustic signals and their recording in the geometric shadow region. The results of calculations of signal
forms are in a satisfactory agreement with data on signals recorded in the geometric shadow region which is formed at a distance
of about 300 km from an experimental explosion. 相似文献
649.
S. I. Prokopiev T. E. Ovchinnikova O. F. Vasiliev 《Izvestiya Atmospheric and Oceanic Physics》2010,46(2):256-260
To adequately describe the hydrophysical processes in water bodies with a high mineralization, it is necessary to take into
account the dependence that the thermodynamic characteristics of water have on the amount of salts contained in it. This work
investigates some widely known formulas for calculating a number of thermodynamic parameters of mineralized water. The density,
freezing temperature, specific heat of evaporation, and relative pressure of saturated vapor over the surface are considered.
The possibilities of using these formulas when modeling hydrophysical processes in water bodies with salinity in the range
of 0–250 pro mille are analyzed. It is shown that the formulas under consideration should be used when the salinity does not
exceed 100 pro mille. If the mineralization is higher, it is necessary to elaborate more suitable formulas on the basis of
an approximation of in situ data or data from handbooks. 相似文献
650.
M. D. Kravchishina V. P. Shevchenko A. S. Filippov A. N. Novigatskii O. M. Dara T. N. Alekseeva V. A. Bobrov 《Oceanology》2010,50(3):365-385
The grain-size and mineral composition of the suspended particulate matter (SPM) of the Severnaya Dvina River mouth is studied,
as well as the content of several lithogenic elements in the SPM during the spring flood in May 2004. The data published on
the composition of the riverine SPM in the White Sea basin are very poor. The spring flood period when more than half of the
annual runoff is supplied from the river to the sea in a short time is understood more poorly. The report considers the comparison
results for the grain-size compositions of the SPM and the bottom sediments. The data of laser and hydraulic techniques of
the grain-size analysis are compared. The short-period variations of the SPM concentration and composition representing two
diurnal peaks of the tide level are studied. It is found that the SPM is mainly transferred during the spring flood as mineral
aggregates up to 40 μm diameter. The sandysilty fraction of the riverine SPM settles in the delta branches and channels, and
the bulk of the fine pelitic matter is supplied to the sea. The mineral and chemical composition of the Severnaya Dvina River
SPM is determined by the supply of substances from the drainage basin. This substance is subjected to intense mechanic separation
during the transfer to the sea. The key regularities of the formation of the mineral composition of the SPM during the flood
time are revealed. The effect of the grain-size composition of the SPM on the distribution of the minerals and elements studied
in the dynamic system of the river mouth are characterized. 相似文献