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471.
Hildegard?WestphalEmail author Iris?Surholt Christian?Kiesl Holger F. ?Thern Thomas?Kruspe 《Pure and Applied Geophysics》2005,162(3):549-570
Carbonate rocks are well known for their complex petrophysical behavior where, in contrast to siliciclastic rocks, different parameters, including porosity and permeability, usually are not directly related. This behavior is the result of thorough reorganization of porosity during diagenesis, and it turns prediction of reservoir quality of carbonate rocks into a challenge. The study presented here deals with the problem of utilizing NMR techniques in prediction of petrophysical properties in carbonates.We employ a visual porosity classification as a priori knowledge for better interpreting NMR data for prediction purposes. This allows for choice of suitable T2 cutoff values to differentiate movable from bound fluids adapted for the specific carbonate rock, thus resulting in better interpretation of NMR data. The approach of using a genetic pore type classification for adapting the conventional method for T2 cutoff determination, which originally was developed for siliciclastic rocks, is promising. Similarly, for permeability determination on the basis of NMR measurements, the classification of carbonate rocks based on porosity types also shows potential. The approach implemented here has the promise to provide a basis of standardized interpretation of NMR data from carbonate rocks.Acknowledgment We are grateful to Baker Hughes INTEQ, Celle, for permission to publish the results of this work. This study was part of I.S.s Masters Thesis at Hannover University that was carried out in collaboration with Baker Hughes INTEQ, Celle, Germany. We appreciate comments of an anonymous referee and PAGEOPH editor Brian J. Mitchell. 相似文献
472.
Three-Dimensional Electromagnetic Modelling and Inversion from Theory to Application 总被引:12,自引:1,他引:11
Dmitry?B.?Avdeevdavdeev@cp.dias.ie" title="d.avdeev@mtu-net.ru davdeev@cp.dias.ie" itemprop="email" data-track="click" data-track-action="Email author" data-track-label="">Email author 《Surveys in Geophysics》2005,26(6):767-799
The whole subject of three-dimensional (3-D) electromagnetic (EM) modelling and inversion has experienced a tremendous progress
in the last decade. Accordingly there is an increased need for reviewing the recent, and not so recent, achievements in the
field. In the first part of this review paper I consider the finite-difference, finite-element and integral equation approaches
that are presently applied for the rigorous numerical solution of fully 3-D EM forward problems. I mention the merits and
drawbacks of these approaches, and focus on the most essential aspects of numerical implementations, such as preconditioning
and solving the resulting systems of linear equations. I refer to some of the most advanced, state-of-the-art, solvers that
are today available for such important geophysical applications as induction logging, airborne and controlled-source EM, magnetotellurics,
and global induction studies. Then, in the second part of the paper, I review some of the methods that are commonly used to
solve 3-D EM inverse problems and analyse current implementations of the methods available. In particular, I also address
the important aspects of nonlinear Newton-type optimisation techniques and computation of gradients and sensitivities associated
with these problems. 相似文献
473.
Franco?Braga Marco?Faggella Rosario?Gigliotti Michelangelo?LaterzaEmail author 《Bulletin of Earthquake Engineering》2005,3(3):333-353
The isolation systems are usually made of rubber bearings that are sometimes coupled in hybrid combination with frictional
devices; this is the case of an in-site experimental campaign, performed on a base isolated apartment building in Rapolla
(south of Italy). Several dropout tests at initial displacements up to 17cm allowed to obtain in-site information on the true
dynamic response of the isolation system (building and isolators). The tests carried out allow a comparison between the free
vibration responses of a building, isolated by using a 28 HDRB isolation system only, or an HDRB-Friction Sliders Hybrid one.
The paper highlights the main differences of the response in the superstructure (the structure over the isolation system)
obtained by using only HDRB isolation system, or the Hybrid one (HDRB and Friction Sliders in parallel system). Analysis and
comparisons of experimental data, show the influence of nonlinearities on structural higher modes amplification, especially
observed by using the higher nonlinear Hybrid isolation system. Tests results confirm that, in the case of a regular superstructure,
like the Rapolla building, the isolation system nonlinearities influence the structural response. 相似文献
474.
Antonio?VecchioEmail author Leonardo?Primavera Vincenzo?Carbone Luca?Sorriso-Valvo 《Solar physics》2005,229(2):359-372
We use the Proper Orthogonal Decomposition (POD) to investigate the spatiotemporal features of the solar activity. Daily observation
in the period 1949–1996 of the green coronal emission line at 530.3 nm are used as indicators of the activity behavior. We
show that few POD modes suffice in describing both the space and time main periodicities. In particular, being affected by
a strongly energetic stochastic behavior, daily data are described by five POD modes, while two POD modes are enough to describe
the butterfly diagram in monthly averaged data. Apart from the basic period T0 = 11 years, using daily data we found evidences for intercycle temporal periodicities. 相似文献
475.
A novel scenario for Maunder minimum-like grand minima epochs of reduced solar activity is proposed, based on diffusive coupling
between both solar hemispheres, each susceptible to stochastically-driven intermittent behavior. After introducing cross-hemispheric
coupling into a well-validated reduced model of the solar cycle based on the Babcock–Leighton mechanism for poloidal field
regeneration, simulations are presented demonstrating that even weak coupling can lead to a high degree of synchronicity between
the two hemispheres. This is in qualitative agreement with the similar onset and recovery times of sunspot activity at and
around the Maunder minimum. Moreover, even weak coupling manages to greatly reduce the frequency and duration of quiescent
episodes, again in qualitative agreement with the relative paucity of grand minima in the sunspot and radioisotope records. 相似文献
476.
Additional analysis of the behavior of the international sunspot number (R) series and the solar radio flux density (F10.7 cm) series during two long (250–500 days) and distinct episodes of persistent ≈13-day variations (Crane, Solar Phys. 1998, 253, 177) is reported. The conclusion is that while the center-to-limb behavior of R does not change between solar minimum and solar maximum, F10.7 cm exhibits significantly less limb brightening at solar maximum than at solar minimum. 相似文献
477.
Predicting the Arrival Time of Shock Passages at Earth 总被引:1,自引:0,他引:1
Chin-Chun?WuEmail author C.?D.?Fry D.?Berdichevsky M.?Dryer Z.?Smith T.?Detman 《Solar physics》2005,227(2):371-386
The purpose of this parametric study is to predict the arrival time at Earth of shocks due to disturbances observed on the Sun. A 3D magnetohydrodynamic (MHD) simulation code is used to simulate the evolution of these disturbances as they propagate out to 1 AU. The model in Han, Wu and Dryer (1988) uses solar data for input at 0.08 AU (18 solar radii). The initial shock speed (ISS) is assumed to be constant from the corona to 0.08 AU. We investigate how variations of this ISS affect the arrival times of the shock at Earth. This basic parametric study, however, does not consider inhomogeneous background solar wind structures such as corotating interaction regions and their precursor stream–stream interactions, nor interplanetary manifestations of complex coronal mass ejecta such as magnetic clouds. In the latter case, only their associated shocks are considered. Because the ambient (pre-existing background) solar wind speed is known to affect the shock arrival time at 1 AU, we also simulated events with various background solar wind speeds (BSWS) to investigate this effect. The results show that the shock arrival time at Earth depends on the BSWS, the speed of solar disturbances, their size, and their source location at the Sun. However, it is found that for a sufficiently large momentum input, the shock arrival time at Earth is not significantly affected by the pre-existing solar wind speed. 相似文献
478.
{We investigate the conversion of the 0.5–4 and 1–8 Å soft X-ray flux measurements made by detectors on the Geostationary Operational Environmental Satellites (GOES) into temperature and emission measures of coronal plasma using modern spectral models and modern understanding of coronal abundances. In particular, the original analysis by Thomas, Starr and Crannell (1985) is updated to take into account the realization that coronal abundances may be quite different from photospheric abundances. An important result of this analysis is that the derived temperatures and emission measures depend strongly on the assumed abundances even at high temperatures where continuum rather than spectral lines dominates the Sun’s X-ray spectrum. This occurs because the higher coronal abundances mean that most of the continuum is due to free–bound emission processes, not free–free emission, and thus is abundance-dependent. We find significant differences between modern calculations of the temperature response of the flux measurements and the versions currently in use: for a typical flare, emission measures may be up to a factor of 4 smaller than the current software suggests. Derived temperatures are similar for both photospheric and coronal abundances for cool flares (e.g., 15 MK), but for hot flares (e.g., 35 MK) coronal abundances can lead to significantly (~25%) lower temperatures being derived. 相似文献
479.
We have selected 104 active regions with a δ magnetic configuration from 1996 to 2002 to study how important a role the kink
instability plays in such active regions. In this study, we employ the systematic tilt angle of each active region as a proxy
for the writhe of a flux tube and the force-free parameter, αbest, as a proxy for the magnetic field twist in the flux tube. It is found that 65–67% of the active regions have the same sign
of twist and writhe. About 34% (32%) of the active regions violate (follow) the Hale-Nicholson and Joy's Laws (HNJL) but follow
(violate) the hemispheric helicity rule (HHR). Sixty-one (61) of the 104 active regions studied each produced more than five
large flares. Active regions violating HNJL, but following HHR, have a much stronger tendency to produce X-class flares and/or
strong proton events. Comparing with previous studies for active regions with well-defined (simpler) bipolar magnetic configuration,
it is found that the numbers following both HNJL and HHR are significantly lower in the δ-configuration case, while numbers
violating one of the laws and the rule significantly increase with the increase of the magnetic complexity of the active regions.
These results support the prediction for the presence of a kink instability, that the twist and writhe of the magnetic fields
exhibit the same sign for δ active regions (Linton et al., Astrophys. J. 507, 40, 1998, Astrophys. J. 522, 1205, 1999; Fan et al., Astrophys. J. 521, 460, 1999). Finally, we analyze possible origins of the twist and writhe of the magnetic fields for the active regions studied. 相似文献
480.
Kinetic Properties of CMEs Corrected for the Projection Effect 总被引:2,自引:0,他引:2
Observations of coronal mass ejections (CMEs) with coronagraphs are subject to a projection effect, which results in statistical
errors in many properties of CMEs, such as the eruption speed and the angular width. In this paper, we develop a method to
obtain the velocity and angular width distributions of CMEs corrected for the projection effect, and then re-examine the relationship
between CMEs and the associated flares. We find that (1) the mean eruption speed is 792 km s−1 and the mean angular width is 59∘, compared to the values of 549 km s−1 and 77∘, respectively before the correction; (2) after the correction, the weak correlation between CME speeds and the GOES X-ray
peak flux of the flares gets unexpectedly poorer; and (3) before correction, there is a weak correlation between the angular
width and the speed of CMEs, whereas the correlation is absent after the correction. 相似文献