全文获取类型
收费全文 | 30999篇 |
免费 | 453篇 |
国内免费 | 338篇 |
专业分类
测绘学 | 649篇 |
大气科学 | 1988篇 |
地球物理 | 5659篇 |
地质学 | 11787篇 |
海洋学 | 3117篇 |
天文学 | 7164篇 |
综合类 | 69篇 |
自然地理 | 1357篇 |
出版年
2022年 | 308篇 |
2021年 | 479篇 |
2020年 | 537篇 |
2019年 | 577篇 |
2018年 | 1134篇 |
2017年 | 1082篇 |
2016年 | 1199篇 |
2015年 | 582篇 |
2014年 | 1100篇 |
2013年 | 1773篇 |
2012年 | 1199篇 |
2011年 | 1528篇 |
2010年 | 1348篇 |
2009年 | 1657篇 |
2008年 | 1407篇 |
2007年 | 1475篇 |
2006年 | 1369篇 |
2005年 | 820篇 |
2004年 | 759篇 |
2003年 | 729篇 |
2002年 | 730篇 |
2001年 | 660篇 |
2000年 | 608篇 |
1999年 | 495篇 |
1998年 | 500篇 |
1997年 | 475篇 |
1996年 | 414篇 |
1995年 | 369篇 |
1994年 | 398篇 |
1993年 | 312篇 |
1992年 | 316篇 |
1991年 | 302篇 |
1990年 | 333篇 |
1989年 | 231篇 |
1988年 | 236篇 |
1987年 | 281篇 |
1986年 | 224篇 |
1985年 | 342篇 |
1984年 | 310篇 |
1983年 | 285篇 |
1982年 | 307篇 |
1981年 | 222篇 |
1980年 | 265篇 |
1979年 | 209篇 |
1978年 | 221篇 |
1977年 | 174篇 |
1976年 | 168篇 |
1975年 | 179篇 |
1974年 | 175篇 |
1973年 | 177篇 |
排序方式: 共有10000条查询结果,搜索用时 9 毫秒
991.
This study investigates how the choice of the planetary boundary layer (PBL) parameterization and dust emission scheme affects the prediction of dust entrainment simulated with a regional mesoscale model. For this analysis we consider a representative dust episode which occurred on April 2001 in the Aral Sea region. The meteorological fields were simulated using the PSU/NCAR MM5 modeling system considering two different boundary layer parameterizations. In each case, emitted dust fluxes were computed off-line by incorporating MM5 meteorological fields into the dust module DuMo. Several dust emission schemes with a prescribed erodible fraction and fixed threshold wind speed were the subject of our analysis. Implications to assessment of the anthropogenic fraction of dust emitted in the Aral region were investigated by conducting the full, half, and no lake modeling experiments.Our results show that the discrepancies in dust fluxes between the two different PBLs are much higher compared to the discrepancy associated with the use of considered dust production schemes. Furthermore, the choice of the PBL affects the timing and duration of a modeled dust event. We demonstrate that different combinations of the PBL parameterization and wind- or friction velocity-driven dust emission schemes can result in up to about a 50% difference in predicted dust mass caused by the Aral Sea desiccation. We found that the drying-up of the Aral cannot only affect the dust emission by expanding the source area, but also by affecting atmospheric characteristics, especially winds. These competitive factors add further complexity to quantification of the anthropogenic dust fraction in the region. 相似文献
992.
Michael W. Busch Steven J. Ostro Jon D. Giorgini Ellen S. Howell Alice A. Hine Irwin I. Shapiro 《Icarus》2007,186(2):581-584
In November 2005, we observed the moons of Mars using the Arecibo 2380-MHz (13-cm) radar, obtaining a result for the OC radar albedo of Phobos (0.056±0.014) consistent with its previously reported radar albedo and implying an upper bound on its near-surface bulk density of . We detected Deimos by radar for the first time, finding its OC radar albedo to be 0.021±0.006, implying an upper bound on its near-surface density of , consistent with a high-porosity regolith. We briefly discuss reasons for these low radar albedos, Deimos' being possibly the lowest of any Solar System body yet observed by radar. 相似文献
993.
The results of the high-resolution long-term spectral monitoring of the Herbig Ae star HD 31648 in the regions of emission
Hα line, Na I D resonance lines and OI 7774 lines are presented.
We confirmed the conclusion, made in previous papers, that the spectral variability of the star in the region of Hα line have
a cyclic character. It is manifested itself as the changing of the equivalent width and intensity of Hα line of the time scale
of about 1200d.
It is shown, that the stellar wind is non-homogeneous and consists of several components, which are differed each other by
their velocities. They are observed as in the H line as in Na I D resonance lines. The component’s parameters are changed
during the cycle of stellar activity (in the maximum of activity the velocity and density of the wind are taken the largest
values and then they are gradually decreased).
The investigation of rapid variability of the He I 5876 line on the time scale of a few hours allows find the correlation
between the variability of the blue and the red wings of the line. It points at the connection between the accretion and the
outflows. Such connection, in particularly, is predicted by the modeling of the wind from young stars made in the frame of
the magneto-centrifugal model, the accordance of which for the HD 31648 was shown in the previous papers. In the present work
we confirmed this conclusion on the basis of the new data.
We found the weak variability of the stellar brightness (about 0.2m), which is agree with the spectral variability (the brightness
of the star becomes lower in the maximum of the activity). These changes are well explained by the process of the dust transfer
from CS disk by the stellar wind. This process is likely to be more effective in the maximum of activity.
An analysis of the variability of other spectral lines shows the agreement between the changing of the Hα line, the Na I D
resonance doublet lines and KI 7698 line. The weak connection between the He I 5876 and the Na I D lines is also found. Since
the formation regions of He I 5876 and Na I D lines are essentially different, we can conclude that the phenomena, responsible
for the observed cyclic variability, take place in a spacious region of the CS envelope.
We believe that the most plausible reason of found cyclic variability is the reconstruction of the inner structure of the
CS gas envelope, caused by the presence around the star a low mass companion or planet.
__________
Translated from Astrofizika, Vol. 50, No. 4, pp. 565–588 (November 2007). 相似文献
994.
Taeyoung Lee Melvin Leok N. Harris McClamroch 《Celestial Mechanics and Dynamical Astronomy》2007,98(2):121-144
Equations of motion, referred to as full body models, are developed to describe the dynamics of rigid bodies acting under
their mutual gravitational potential. Continuous equations of motion and discrete equations of motion are derived using Hamilton’s
principle. These equations are expressed in an inertial frame and in relative coordinates. The discrete equations of motion,
referred to as a Lie group variational integrator, provide a geometrically exact and numerically efficient computational method
for simulating full body dynamics in orbital mechanics; they are symplectic and momentum preserving, and they exhibit good
energy behavior for exponentially long time periods. They are also efficient in only requiring a single evaluation of the
gravity forces and moments per time step. The Lie group variational integrator also preserves the group structure without
the use of local charts, reprojection, or constraints. Computational results are given for the dynamics of two rigid dumbbell
bodies acting under their mutual gravity; these computational results demonstrate the superiority of the Lie group variational
integrator compared with integrators that are not symplectic or do not preserve the Lie group structure. 相似文献
995.
I. I. Romanyuk V. E. Panchuk N. E. Piskunov D. O. Kudryavtsev 《Astrophysical Bulletin》2007,62(1):26-35
The possibility of investigating the vertical structure of the magnetic field in chemically peculiar main-sequence stars is discussed. The nonuniform distribution of chemical elements over the surface complicates the problem substantially. The most efficient measurements are shown to be those of the longitudinal field components based on spectral lines with wavelengths longer and shorter than 3646 Å (shortward and longward of the Balmer jump), which form at different optical depths in the atmosphere. Various methodological problems are addressed that must be overcome in order to accomplish the task. The brightest magnetic star α 2 CVn is observed with the echelle spectrometer equipped with an Uppsala CCD chip. New observations corroborate our previous result: the longitudinal component of the magnetic field B e of the α 2 CVn star increases with depth by about 30% over the atmosphere thickness scale. 相似文献
996.
N. F. Vojkhanskaja 《Astrophysics》2007,50(3):351-361
Cataclysmic variables (CV) and pre-cataclysmic binaries (PCB) are discussed. The main difference between them (accretion or
its absence) is shown to be a consequence of the evolutionary process and the properties of their progenitors. Both types
of system have a bimodal distribution of their periods, but the extrema are in counterphase. Luminosity-effective temperature
diagrams for the primary components are used to show that both systems have approximately the same age, which conflicts with
the notion of PCBs as precursors of CVs. Calculations of the maximum distance between components for which the system remains
stable show that CVs have passed this limit, while PCBs maintain their stability during this evolution. It is suggested that,
after ejecting a common shell, future CVs immediately become semi-detached systems. It this is so, then there must be cataclysmic
variables which are the central stars of planetary nebulae.
__________
Translated from Astrofizika, Vol. 50, No. 3, pp. 427–439 (August 2007). 相似文献
997.
We present the characteristics, operations history, performance, and calibration of the Grazing Incidence Spectrometer (GIS)
of the Coronal Diagnostic Spectrometer onboard SOHO. The GIS sensitivity has been monitored in a direct manner by examining
the quiet Sun count rates during 1996 – 2006, nearly a whole solar cycle of observations. Overall, the instrument, with its
grazing-incidence optics and microchannel plates, has performed exceptionally well. For most spectral regions, changes in
the instrument sensitivity have been very small over a 10-year period. The trends in sensitivities support the use of the
radiometric calibration of Del Zanna et al. (Astron. Astrophys.
379, 708, 2001) throughout the mission. The verification of the detector performance over such a long period allows us to point out the
spectral lines that can reliably be used for scientific analysis. 相似文献
998.
We investigate the quantum field theory of a Lorentz non-invariant model with a massive nonlinear dispersion relation in Minkowski
space. The model involves some non-causal signals in the form of wave packets propagating with super-luminal group velocities.
To avoid the problems with causality we characterize the causal sector of the theory by a cutoff condition excluding all super-luminal
group velocities. It is argued that in the causal theory satisfying the energy positivity condition an Unruh’s detector moving
with a constant velocity with respect to the preferred frame does not detect any particle. But in a causal theory violating
energy positivity, detection of a field quanta occurs. We comment on the origin of this particle creation. 相似文献
999.
Many lens surveys have hitherto used observations of large samples of background sources to select the small minority which are multiply imaged by lensing galaxies along the line of sight. Recently surveys such as SLACS and OLS have improved the efficiency of surveys by pre-selecting double-redshift systems from SDSS. We explore other ways to improve survey efficiency by optimum use of astrometric and morphological information in existing large-scale optical and radio surveys. The method exploits the small position differences between FIRST radio positions of lensed images and the SDSS lens galaxy positions, together with the marginal resolution of some larger gravitational lens systems by the FIRST beam. We present results of a small pilot study with the VLA and MERLIN, and discuss the desirable criteria for future surveys. 相似文献
1000.
M. Fellhauer N. W. Evans V. Belokurov D. B. Zucker B. Yanny M. I. Wilkinson G. Gilmore M. J. Irwin D. M. Bramich S. Vidrih P. Hewett T. Beers 《Monthly notices of the Royal Astronomical Society》2007,375(4):1171-1179
Prominent in the 'Field of Streams'– the Sloan Digital Sky Survey map of substructure in the Galactic halo – is an 'Orphan Stream' without obvious progenitor. In this numerical study, we show a possible connection between the newly found dwarf satellite Ursa Major II (UMa II) and the Orphan Stream. We provide numerical simulations of the disruption of UMa II that match the observational data on the position, distance and morphology of the Orphan Stream. We predict the radial velocity of UMa II as −100 km s−1 , as well as the existence of strong velocity gradients along the Orphan Stream. The velocity dispersion of UMa II is expected to be high, though this can be caused both by a high dark matter content or by the presence of unbound stars in a disrupted remnant. However, the existence of a gradient in the mean radial velocity across UMa II provides a clear-cut distinction between these possibilities. The simulations support the idea that some of the anomalous, young halo globular clusters like Palomar 1 or Arp 2 or Ruprecht 106 may be physically associated with the Orphan Stream. 相似文献