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131.
为提高连续小波变换识别位场场源准确度,研究噪声对场源识别结果的影响和尺度因子优选方法问题。根据连续小波变换识别位场场源的基本原理,用该方法对不同噪声水平的合成数据进行场源识别,分析噪声对于场源识别结果的影响,研究小波变换的尺度因子对噪声压制的效果,讨论连续小波变换进行场源识别时尺度因子的选取方法。理论模型和实测资料场源识别结果表明,噪声会降低连续小波变换场源识别结果的准确度,笔者提出的尺度因子优选方法能有效压制噪声干扰,提高场源识别结果的准确度。 相似文献
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Equilibrium models of differentially rotating nascent neutron stars are constructed, which represent the result of the accretion-induced collapse of rapidly rotating white dwarfs. The models are built in a two-step procedure: (1) a rapidly rotating pre-collapse white dwarf model is constructed; (2) a stationary axisymmetric neutron star having the same total mass and angular momentum distribution as the white dwarf is constructed. The resulting collapsed objects consist of a high-density central core of size roughly 20 km, surrounded by a massive accretion torus extending over 1000 km from the rotation axis. The ratio of the rotational kinetic energy to the gravitational potential energy of these neutron stars ranges from 0.13 to 0.26, suggesting that some of these objects may have a non-axisymmetric dynamical instability that could emit a significant amount of gravitational radiation. 相似文献
135.
C.M. Lisse K. Dennerl S.J. Wolk T.H. Zurbuchen R. Hoekstra C.D. Fry T. Mäkinen 《Icarus》2007,190(2):391-405
We present results from the Chandra X-ray Observatory's extensive campaign studying Comet 9P/Tempel 1 (T1) in support of NASA's Deep Impact (DI) mission. T1 was observed for ∼295 ks between 30th June and 24th July 2005, and continuously for ∼64 ks on July 4th during the impact event. X-ray emission qualitatively similar to that observed for the collisionally thin Comet 2P/Encke system [Lisse, C.M., Christian, D.J., Dennerl, K., Wolk, S.J., Bodewits, D., Hoekstra, R., Combi, M.R., Mäkinen, T., Dryer, M., Fry, C.D., Weaver, H., 2005b. Astrophys. J. 635 (2005) 1329-1347] was found, with emission morphology centered on the nucleus and emission lines due to C, N, O, and Ne solar wind minor ions. The comet was relatively faint on July 4th, and the total increase in X-ray flux due to the Deep Impact event was small, ∼20% of the immediate pre-impact value, consistent with estimates that the total coma neutral gas release due to the impact was 5×106 kg (∼10 h of normal emission). No obvious prompt X-ray flash due to the impact was seen. Extension of the emission in the direction of outflow of the ejecta was observed, suggesting the presence of continued outgassing of this material. Variable spectral features due to changing solar wind flux densities and charge states were clearly seen. Two peaks, much stronger than the man-made increase due to Deep Impact, were found in the observed X-rays on June 30th and July 8th, 2005, and are coincident with increases in the solar wind flux arriving at the comet. Modeling of the Chandra data using observed gas production rates and ACE solar wind ion fluxes with a CXE mechanism for the emission is consistent, overall, with the temporal and spectral behavior expected for a slow, hot wind typical of low latitude emission from the solar corona interacting with the comet's neutral coma, with intermittent impulsive events due to solar flares and coronal mass ejections. 相似文献
136.
We calculate the direction of the rotational angular momentum vector,M, of comet 19P/Borrelly based on rotational lightcurve data from 2000, groundbased imaging of the coma during the Deep Space
1encounter, and the basic near-nucleus coma morphology as revealed by the Deep Space 1 spacecraft. For the most likely direction,
we derivea family of solutions (with center at RA = 221°, Dec = -7°) if the direction of M is towards the sunward hemisphere during the Deep Space 1 encounter, whereas if the rotation is of opposite sense, the diametrically
opposite family of solutions (with center at RA = 41°, Dec = 7°) would result. We argue that the coma morphology in September
2001 is consistent with the nucleus being a principal axis rotator or one observationally indistinguishable from it. Therefore,
for all practical purposes, the direction of the rotational angular momentum vector coincides with the spin axis. We also
discuss why the determination of the spin axis direction based on observations from the last apparition is in disagreement
with the current result. 相似文献
137.
H. M. Antia 《Journal of Astrophysics and Astronomy》2002,23(1-2):3-8
The interior of the Sun is not directly observable to us. Nevertheless, it is possible to infer the physical conditions prevailing
in the solar interior with the help of theoretical models coupled with observational input provided by measured frequencies
of solar oscillations. The frequencies of these solar oscillations depend on the internal structure and dynamics of the Sun
and from the knowledge of these frequencies it is possible to infer the internal structure as well as the large scale flows
inside the Sun, in the same way as the observations of seismic waves on the surface of Earth help us in the study of its interior.
With the accumulation of seismic data over the last six years it has also become possible to study temporal variations in
the solar interior. Some of these seismic inferences would be described. 相似文献
138.
Igor M. Volkov 《Astrophysics and Space Science》2005,296(1-4):105-108
We present a new photoelectric light curve of α Coronae Borealis. The derived rate of apsidal motion differs from the theoretical
prediction. A possible solution of the problem is suggested. 相似文献
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