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891.
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896.
物态方程一直是恒星模型理论研究中的最重要的物理方程之一,对于日震学等高精度要求的研究领域来讲,只包含理想效应的物态方程并不能满足研究需要,而要更细致、包含非理想效应的物态方程对系统作更精确和完善的描述,在弱耦合及弱电子简并的系统中,为研究各种带电粒子之间的库仑耦合效应,以化学图像为基础,分别用具有硬核改正的Debye—Hueckel扩展理论来处理离子-电子作用、多体作用的经典点粒子相互作用理论描述离子-离子作用和量子统计方法处理电子-电子作用,并把此3种作用对物态方程自由能的贡献用半解析的数学公式给出,为适应日震学研究的要求,特别选取一组类太阳的恒星模型作为研究对象,从实际模型计算出发,对库仑耦合中的各种效应进行了比较分析,讨论并检验了所作的理论改进。 相似文献
897.
It is well known that asteroid families have steeper absolute magnitude (H) distributions for H < 12-13 values than the background population. Beyond this threshold, the shapes of the absolute magnitude distributions in the family/background populations are difficult to determine, primarily because both populations are not yet observationally complete. Using a recently generated catalog containing the proper elements of 106,284 main belt asteroids and an innovative approach, we debiased the absolute magnitude distribution of the major asteroid families relative to the local background populations. Our results indicate that the magnitude distributions of asteroid families are generally not steeper than those of the local background populations for H > 13 (i.e., roughly for diameters smaller than 10 km). In particular, most families have shallower magnitude distributions than the background in the range 15-17 mag. Thus, we conclude that, contrary to previous speculations, the population of kilometer-size asteroids in the main belt is dominated by background bodies rather than by members of the most prominent asteroid families. We believe this result explains why the Spacewatch, Sloan Digital Sky Survey, and Subaru asteroid surveys all derived a shallow magnitude distribution for the dimmer members of the main belt population.We speculate on a few dynamical and collisional scenarios that can explain this shallow distribution. One possibility is that the original magnitude distributions of the families (i.e., at the moment of the formation event) were very shallow for H larger than ∼ 13, and that most families have not yet had the time to collisionally evolve to the equilibrium magnitude distribution that presumably characterizes the background population. A second possibility is that family members smaller than about 10 km, eroded over time by collisional and dynamical processes, have not yet been repopulated by the break-up of larger family members. For this same reason, the older (and possibly characterized by a weaker impact strength) background population shows a shallow distribution in the range 15-60 km. 相似文献
898.
A simple mechanical model is formulated to study the dynamics of rubble-pile asteroids, formed by the gravitational re-accumulation of fragments after the collisional breakup of a parent body. In this model, a rubble-pile consists of N interacting fragments represented by rigid ellipsoids, and the equations of motion explicitly incorporate the minimal degrees of freedom necessary to describe the attitude and rotational state of each fragment. In spite of its simplicity, our numerical examples indicate that the overall behavior of our model is in line with several known properties of collisional events, like the energy and angular momentum partition during high velocity impacts. Therefore, it may be considered as a well defined minimal model. 相似文献
899.
M. A. Nowak J. Wilms W. A. Heindl K. Pottschmidt J. B. Dove M. C. Begelman 《Monthly notices of the Royal Astronomical Society》2001,320(3):316-326
LMC X-1 and LMC X-3 are the only known persistent stellar-mass black-hole candidates that have almost always shown spectra that are dominated by a soft, thermal component. We present here results from 170-ks-long Rossi X-ray Timing Explorer ( RXTE ) observations of these objects, taken in 1996 December, where their spectra can be described by a disc blackbody plus an additional soft high-energy power law (detected up to energies of 50 keV in LMC X-3). These observations, as well as archival Advanced Satellite for Cosmology and Astrophysics ( ASCA ) observations, constrain any narrow Fe line present in the spectra to have an equivalent width ≲90 eV. Stronger, broad lines (≈150 eV EW, are permitted. We also study the variability of LMC X-1. Its X-ray power spectral density (PSD) is approximately proportional to between 10−3 and 0.3 Hz with a root-mean-square (rms) variability of ≈7 per cent. At energies >5 keV, the PSD shows evidence of a break at possibly indicating an outer disc radius of ≲1000 GM c 2 in this likely wind-fed system. Furthermore, the coherence function a measure of the degree of linear correlation between variability in the >5 keV band and variability in the lower energy bands, is extremely low (≲50 per cent). We discuss the implications of these observations for the mechanisms that might be producing the soft and hard X-rays in these systems. 相似文献
900.
We present the results of a detailed analysis of RXTE observations of classω (Klein-Woltet al. 2002) which show an unusual state transition between high-soft and low-soft states in the Galactic microquasar GRS 1915 +
105. Out of about 600 pointed RXTE observations, the source was found to exhibit such state transition only on 16 occasions.
An examination of the RXTE/ASM data in conjunction with the pointed observations reveals that these events appeared as a series
of quasi-regular dips in two stretches of long duration (about 20 days during each occasion) when hard X-ray and radio flux
were very low. The X-ray light curve and colour-colour diagram of the source during these observations are found to be different
from any reported so far. The duration of these dips is found to be of the order of a few tens of seconds with a repetition
time of a few hundred seconds. The transition between these dips and non-dips which differ in intensity by a factor of ∼ 3.5,
is observed to be very fast (∼ a few seconds). It is observed that the low-frequency narrow QPOs are absent in the power density
spectrum (PDS) of the dip and non-dip regions of classω and the PDS is a power law in the 0.1–10 Hz frequency range. There is a remarkable similarity in the spectral and timing
properties of the source during the dip and non-dip regions in this set of observations. These properties of the source are
distinctly different from those seen in the observations of other classes. This indicates that the basic accretion disk structure
during both dip and non-dip regions of classω is similar, but differ only in intensity. To explain these observations, we invoke a model in which the viscosity is very
close to critical viscosity and the shock wave is weak or absent. 相似文献