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991.
Rob Cavallo Keith A. Arnaud Virginia Trimble 《Journal of Astrophysics and Astronomy》1993,14(3-4):141-143
Pointed ROSAT PSPC exposures of 9277 and 6992 sec, directed toward the nearby, single, cool, magnetic white dwarfs GR 290
and EG 250 yielded no counts significantly above the expected background rate. The corresponding flux limits (for an assumed
source temperature of l keV) are 1.0 and 1.7 × 10−14erg cm−2 s−1, within the 0.1–2.5 keV bandpass of the instrument (99% confidence limits). This is more than an order of magnitude below
the tentative detection level (for GR 290) and limits (for four other similar stars) obtained from archival Einstein data
in 1991. The corresponding limits on coronal electron density are comparable with those implied if cyclotron emission is not
responsible for any of the features observed in the optical spectra of magnetic white dwarfs. X-ray data currently provide
no evidence for the existence of coronae around these stars. A final long observation (25,000 sec of GD 356) is scheduled
for later this year on ROSAT, along with coordinated EUVE observations. 相似文献
992.
刘允芬 《中国地理科学(英文版)》1995,(1)
THEIMPACTOFTHECONTEMPORARYCLIMATICCHANGEONCHINASTHERMALRESOURCES¥LiuYunfen(刘允芬)(CommissionforIntegratedSurveyofNaturalResourc... 相似文献
993.
994.
It has been known that material anisotropy and thermal stresses affect borehole stability significantly. Aiming at the experimental studies associated with borehole stability in anisotropic (transversely isotropic) poroelastic materials subject to non‐isothermal conditions, this paper details and applies an anisotropic porothermoelastic solution to an unjacketed hollow cylinder in a triaxial set‐up. Numerical analyses are presented to demonstrate thermal and material anisotropy effects on the pore pressure and the stress concentrations in and around the geometry of a hollow cylinder subjected to thermal and stress perturbations. Copyright © 2004 John Wiley & Sons, Ltd. 相似文献
995.
Based on a comprehensive analysis of the October 25, 1994 event, we consider the balance of energetic particles in a type-IV solar radio emission source with a zebra-type fine structure (in a coronal magnetic loop). The zebra pattern is formed through the injection of fast electrons into a trap and the formation of a ring-type nonequilibrium electron distribution function. We estimated the characteristic zebra-pattern lifetime, which is determined by the escape of fast particles from the trap into the loss cone. In addition, we determined the number of fast particles that must be injected into the trap to provide the observed radio brightness temperature in zebra-pattern stripes by analyzing the plasma emission mechanism responsible for the zebra-pattern generation. As a result, we estimated the efficiency of the electron acceleration mechanism in coronal magnetic loops at the post-flare evolutionary phase of an active region. 相似文献
996.
Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses and synoptic maps from Kitt Peak are used to analyze the polar coronal holes of solar activity cycles 22 and 23 (from 1990 to end of 2003). In the beginning of the declining phase of solar cycles 22 and 23, the north polar coronal holes (PCHs) appear about one year earlier than the ones in the south polar region. The solar wind velocity and the solar wind ionic charge composition exhibit a characteristic dependence on the solar wind source position within a PCH. From the center toward the boundary of a young PCH, the solar wind velocity decreases, coinciding with a shift of the ionic charge composition toward higher charge states. However, for an old PCH, the ionic charge composition does not show any obvious change, although the latitude evolution of the velocity is similar to that of a young PCH. 相似文献
997.
Hari Om Vats M. R. Deshpande O. P. N. Calla N. M. Vadher B. M. Darji V. Sukumaran 《Earth, Moon, and Planets》1996,75(2):127-133
In this article we report the peculiar oscillations in the intensity of microwave (4.15 GHz) emission seen during the impact of K fragment of comet Shoemaker-Levy 9 on July 19, 1994. The oscillations begin at 10h 13m 25s UT suddenly with a frequency of ~0.3 Hz and gradually the frequency of these oscillations increases to ~ 1 Hz. The oscillations are not due to local atmosphere or the radio interference from signals of geostationary satellite. They are intrinsic to the microwave emission from Jupiter during the impact of K fragment. Peak-to-peak amplitude of the oscillations is about 34% of the total microwave emission from Jupiter. If we assume that only 50% of the microwave emission is non-thermal and only the non-thermal emission suffered oscillations, then the oscillations are about 68% of the non-thermal emission from Jupiter. The observations also indicate that there are three continuum enhancements during this event and periodic oscillations almost all through. The third enhancement was the largest and during this enhancement there were some additional aperiodic variations. The aperiodic variations were of the order of few minutes and were possibly generated by the gravity waves. The periodic oscillations could be synchrotron emission modulated by the plasma oscillation in the outer magnetosphere. kg]Key words 相似文献
998.
郑州市区的地下热水来自增温地层,在使用电法勘探确定热水层位和埋深时,用五极纵轴测深法与对称四极测深法相结合,取得了良好的地质效果。 相似文献
999.
从理论N体模拟、射电辐射、红外辐射以及统计比较等几个方面,概述了棒在星系恒星形成中的作用,并讨论了在这一问题研究中出现的互相予盾的一些结果。 相似文献
1000.
Rakesh K. Malik Pradeep Gothoskar P. K. Manohran G. Swarup K. Subramanian V. Balasubramanian 《Journal of Astrophysics and Astronomy》1995,16(3-4):393-398
Jupiter flux at 327 MHz was monitored using the Ooty radio telescope from July 12th to July 29th during the collision of comet
Shoemaker-Levi 9 with Jupiter. Flux was found to increase steadily from July 17th to July 26th by ∼ 2–5 Jy, after which it
declined to its pre-event value. The comparison of 327 MHz observations with those at 840 MHz and 2240 MHz indicates that
the enhancement was mainly due to the increased synchrotron emission and the contribution of thermal emission was very small
at metric-decimetric frequencies. The enhancement in radio emission was found to be more at 840 MHz than at 327 or 2240 MHz.
The steepening of the spectrum between 327 and 840 MHz as well as between 2240 and 840 MHz was also noted. 相似文献