全文获取类型
收费全文 | 1291篇 |
免费 | 110篇 |
国内免费 | 102篇 |
专业分类
测绘学 | 124篇 |
大气科学 | 43篇 |
地球物理 | 285篇 |
地质学 | 250篇 |
海洋学 | 35篇 |
天文学 | 572篇 |
综合类 | 73篇 |
自然地理 | 121篇 |
出版年
2024年 | 4篇 |
2023年 | 4篇 |
2022年 | 15篇 |
2021年 | 14篇 |
2020年 | 15篇 |
2019年 | 24篇 |
2018年 | 15篇 |
2017年 | 30篇 |
2016年 | 27篇 |
2015年 | 30篇 |
2014年 | 31篇 |
2013年 | 62篇 |
2012年 | 29篇 |
2011年 | 31篇 |
2010年 | 40篇 |
2009年 | 71篇 |
2008年 | 76篇 |
2007年 | 117篇 |
2006年 | 88篇 |
2005年 | 74篇 |
2004年 | 78篇 |
2003年 | 72篇 |
2002年 | 76篇 |
2001年 | 57篇 |
2000年 | 71篇 |
1999年 | 53篇 |
1998年 | 45篇 |
1997年 | 46篇 |
1996年 | 28篇 |
1995年 | 35篇 |
1994年 | 28篇 |
1993年 | 26篇 |
1992年 | 19篇 |
1991年 | 11篇 |
1990年 | 14篇 |
1989年 | 8篇 |
1988年 | 17篇 |
1987年 | 12篇 |
1986年 | 5篇 |
1985年 | 3篇 |
1982年 | 1篇 |
1981年 | 1篇 |
排序方式: 共有1503条查询结果,搜索用时 15 毫秒
81.
H. Greiner-Mai J. Hagedoorn L. Ballani I. Wardinski D. Stromeyer R. Hengst 《Studia Geophysica et Geodaetica》2007,51(4):491-513
We investigate the temporal behaviour of the axial component of the electromagnetic core-mantle coupling torque that is associated
with the poloidal part of the geomagnetic field observable at the Earth surface. For its computation, we use different models
of the geomagnetic field, expanded into spherical harmonics (Wardinski and Holme, 2006; Sabaka et al., 2004), and the mantle
conductivity. The geomagnetic field, which we have to know at the core-mantle boundary for the associated computations, will
be inferred from the field at the Earth surface by the non-harmonic field continuation through a conducting mantle shell.
The aims of this investigation are (i) to check how sensitive is the computation of the torque with respect to the different
geomagnetic field models, (ii) to check its dependence on the spherical harmonic degree n, and (iii) to determine the difference
between the mechanical torque derived from the observed length-of-day variations (atmospheric influence subtracted) and the
poloidal electromagnetic torque in dependence on the assumed conductivity. To use the non-harmonic field continuation for
the torque calculation and to obtain an insight into the influence of the different geomagnetic field models on the EM torques
are the major aspects of this paper.
grm@gfz-potsdam.de 相似文献
82.
We use the rotation curves of 13 galaxies to test the nonsymmetric gravitaional theory (NGT). If we follow Moffat's assumption of a constant mass-to-light for all galaxies then we shall find that the two supposedly universal constants r0, L0 to show a large scatter. By regarding the mass-to-light ratio as a free parameter for each galaxy, and adjusting the values of r0, L0, we find that NGT can well account for the observed rotation curves. Further, the mass-to-light ratios so found show the well-known trend along the Hubble morphological sequence. 相似文献
83.
A 29-year time-series of four-times-daily atmospheric effective angular momentum (EAM) estimates is used to study the atmospheric
influence on nutation. The most important atmospheric contributions are found for the prograde annual (77 μas), retrograde
annual (53 as), prograde semiannual (45 as), and for the constant offset of the pole (δψsinɛ0=−86 as, δɛ=77 as). Among them only the prograde semiannual component is driven mostly by the wind term of the EAM function,
while in all other cases the pressure term is dominant. These are nonnegligible quantities which should be taken into account
in the new theory of nutation. Comparison with the VLBI corrections to the IAU 1980 nutation model taking into account the
ocean tide contribution yields good agreement for the prograde annual and semiannual nutations. We also investigated time
variability of the atmospheric contribution to the nutation amplitudes by performing the sliding-window least-squares analysis
of both the atmospheric excitation and VLBI nutation data. Almost all detected variations of atmospheric origin can be attributed
to the pressure term, the biggest being the in-phase annual prograde component (about 30 as) and the retrograde one (as much
as 100200 as). These variations, if physical, limit the precision of classical modeling of nutation to the level of 0.1 mas.
Comparison with the VLBI data shows significant correlation for the retrograde annual nutation after 1989, while for the prograde
annual term there is a high correlation in shape but the size of the atmospherically driven variations is about three times
less than deduced from the VLBI data. This discrepancy in size can be attributed either to inaccuracy of the theoretical transfer
function or the frequency-dependent ocean response to the pressure variations. Our comparison also yields a considerably better
agreement with the VLBI nutation data when using the EAM function without the IB correction for ocean response, which indicates
that this correction is not adequate for nearly diurnal variations.
Received: 10 September 1997 / Accepted: 5 March 1998 相似文献
84.
基于三旋转自由度激光经纬仪的结构光工程测量原理与应用 总被引:4,自引:0,他引:4
围绕具有三旋转自由度的激光经纬仪,阐述它在封闭构筑物测量中应用的优越性,提出结构光工程测量中各种扫描关系式的解算式,并用实例证明所述理论的正确性与高效率。 相似文献
85.
Raymond Hide 《Geophysical Journal International》1998,135(3):1150-1152
Several dynamic agencies control differential rotation between various regions of a rotating gravitating body such as a planet, namely advection of angular momentum (within fluid regions) and torques due not only to (a) viscous forces, (b) dynamic pressure forces and (c) gravitational forces, but also to (d) Lorentz forces (involving the flow of electric currents in electrically conducting regions), (e) magnetostatic forces (when magnetized material is present) and (f) electrostatic forces (due to the presence of electric charges). Torques due to (a), (b), (c) and (d) have already been treated in the literature, some extensively. It is of general theoretical interest to derive from first principles mathematical expressions for torques due to (e) and (f), even though they turn out to be quantitatively insignificant in the case of the Earth. 相似文献
86.
87.
H. M. Antia Sarbani Basu & S. M. Chitre 《Monthly notices of the Royal Astronomical Society》1998,298(2):543-556
A new set of accurately measured frequencies of solar oscillations is used to infer the rotation rate inside the Sun, as a function of radial distance as well as latitude. We have adopted a regularized least-squares technique with iterative refinement for both 1.5D inversion, using the splitting coefficients, and 2D inversion using individual m splittings. The inferred rotation rate agrees well with earlier estimates showing a shear layer just below the surface and another one around the base of the convection zone. The tachocline or the transition layer where the rotation rate changes from differential rotation in the convection zone to an almost latitudinally independent rotation rate in the radiative interior is studied in detail. No compelling evidence for any latitudinal variation in the position and width of the tachocline is found, although it appears that the tachocline probably shifts to a slightly larger radial distance at higher latitudes and possibly also becomes thicker. However, these variations are within the estimated errors and more accurate data would be needed to make a definitive statement about latitudinal variations. 相似文献
88.
本世纪青藏高原气候的三次突变及与天文因素的相关 总被引:39,自引:9,他引:30
用给出了的划分气候阶段的标准对本世纪高原的气温,降水和季风的阶段性变化进行了分析,发现本世纪高原气候在20年代初,50-60年代和80年代初发生了三次突变,与北半球的气候变化一致。高原气温突长数年后我国和北半球温度突升,接着高原季节增强,高原“季风多雨区”变温,“季风少雨区”变干,反之则相反,进一步分析表明,地球自转速度和太阳黑子周期长度的变化对高原及北半球本世纪气候的突变和阶段性变化起着重要的作 相似文献
89.
P. Descamps T. Michalowski J. Berthier J.-P. Teng-Chuen-Yu B. Payet Y. Léonie H. Berrouachdi F. Benard 《Icarus》2007,189(2):362-369
We present a set of rotational lightcurve measurements of the small main belt Asteroid 3169 Ostro. Our observations reveal an unambiguous, double-peaked rotational lightcurve with a peak-to-peak variation up to 1.2±0.05 mag and a synodic period of 6.509±0.001 h. From the large flux variation and the overall shape of the lightcurves, we suggest that 3169 Ostro could be a tightly bound binary or a contact binary, similar to the Trojan Asteroid 624 Hektor. A shape model of this system is proposed on the assumption that 3169 Ostro is a Roche binary described by a pair of homogeneous elongated bodies, with a size ratio of 0.87, in hydrostatic equilibrium and in circular synchronous motion around each other. The direction of the spin axis is determined modulo 180° by its J2000 ecliptic coordinates λ0=50±10°, β0=±54±5°. The binary interpretation and the pole solution adequately fit the earlier photometric observations made in 1986 and 1988. However, additional supporting lightcurves are highly desirable especially in the next mutual events occurrence of 2008 and 2009 in order to remove the pole ambiguity and to confirm unambiguously the binary nature of 3169 Ostro. 相似文献
90.
F. De Luise D. Perna E. Dotto I.N. Belskaya G.B. Valsecchi A. Rossi P. Paolicchi 《Icarus》2007,191(2):628-635
In this paper we present the observational campaign carried out at ESO NTT and VLT in April and May 2006 to investigate the nature and the structure of the near-Earth object (144898) 2004 VD17. In spite of a great quantity of dynamical information, according to which it will have a close approach with the Earth in the next century, the physical properties of this asteroid are largely unknown. We performed visible and near-infrared photometry and spectroscopy, as well as polarimetric observations. Polarimetric and spectroscopic data allowed us to classify 2004 VD17 as an E-type asteroid. A good agreement was also found with the spectrum of the aubrite meteorite Mayo Belwa. On the basis of the polarimetric albedo (pv=0.45) and of photometric data, we estimated a diameter of about 320 m and a rotational period of about 2 h. The analysis of the results obtained by our complete survey have shown that (144898) 2004 VD17 is a peculiar NEO, since it is close to the breakup limits for fast rotator asteroids, as defined by Pravec and Harris [Pravec, P., Harris, A.W., 2000. Icarus 148, 12-20]. These results suggest that a more robust structure must be expected, as a fractured monolith or a rubble pile in a “strength regime” [Holsapple, K.A., 2002. Speed limits of rubble pile asteroids: Even fast rotators can be rubble piles. In: Workshop on Scientific Requirements for Mitigation of Hazardous Comets and Asteroids, Washington, September, 2002]. 相似文献