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排序方式: 共有2069条查询结果,搜索用时 437 毫秒
961.
962.
C. Alcock R. A. Allsman D. R. Alves T. S. Axelrod A. C. Becker D. P. Bennett P. A. Charles K. H. Cook A. J. Drake K. C. Freeman M. Geha K. Griest M. J. Lehner S. L. Marshall K. E. McGowan † D. Minniti C. A. Nelson B. A. Peterson P. Popowski M. R. Pratt P. J. Quinn C. W. Stubbs W. Sutherland A.B. Tomaney T. Vandehei D. L. Welch 《Monthly notices of the Royal Astronomical Society》2001,321(4):678-684
We present a ∼5-yr optical light curve of the recurrent Be/X-ray transient A0538–66 obtained as a by-product of the MACHO Project. These data reveal both a long-term modulation at P =420.8±0.8 d and a short-term modulation at 16.6510±0.0022 d which, within errors, confirms the previously found orbital period. Furthermore, the orbital activity is only seen at certain phases of the 421-d cycle, suggesting that the long-term modulation is related to variations in the Be star envelope. 相似文献
963.
J. Casares G. Dubus T. Shahbaz C. Zurita P.A. Charles 《Monthly notices of the Royal Astronomical Society》2002,329(1):29-36
We present Very Large Telescope (VLT) low-resolution spectroscopy of the neutron star X-ray transient XTE J2123−058 during its quiescent state. Our data reveal the presence of a K7V companion which contributes 77 per cent to the total flux at λ 6300 and orbits the neutron star at . Contrary to other soft X-ray transients (SXTs), the H α emission is almost exactly in antiphase with the velocity curve of the optical companion. Using the light-centre technique we obtain and hence This, combined with a previous determination of the inclination angle yields and . M 2 agrees well with the observed spectral type. Doppler tomography of the H α emission shows a non-symmetric accretion disc distribution mimicking that seen in SW Sex stars. Although we find a large systemic velocity of − this value is consistent with the galactic rotation velocity at the position of J2123−058, and hence a halo origin. The formation scenario of J2123−058 is still unresolved. 相似文献
964.
Danuta Peryt Krystyna Wyrwicka Charles Orth Moses Attrep Jr Leonard R. Quintana 《地学学报》1994,6(2):158-165
Two sections of the Upper Cenomanian and Lower Turonian in central and south-east Poland were investigated for foraminifers, CaCO3 content, carbon content insoluble in HCl (Corg ) and in the carbonates (Ccarb ), carbon and oxygen isotopic composition of bulk-rock carbonates and elemental abundances. The Cenomanian/Turonian boundary interval is characterized by the appearance of more marly facies, a δ13 C and δ18 O stable isotope anomaly, a considerable increase in Corg content and decrease in Ccarb content and substantial changes in the foraminiferal assemblages. A major carbon stable isotope excursion with a shift of +2 (PDB) occurs in the lowermost Whiteinella archaeocretacea Zone. The late Cenomanian δ13 C anomaly is associated with heavy δ18 O values. The peak value of δ13 C corresponds to the minima in P/B ratio and in diversity of foraminiferal assemblages. A late Cenomanian anoxic event is thought to be responsible for changes in foraminiferal assemblages. However, elemental abundance analyses do not show changes in the concentrations of trace elements. This may be explained by the long distance between studied area and a source of enrichment which was probably located in the western hemisphere. 相似文献
965.
Lindsay P. Keller James C. Clark Charles F. Lewis Carleton B. Moore 《Meteoritics & planetary science》1992,27(1):87-91
Abstract— The Maralinga meteorite was found near the village of Maralinga, South Australia (30°18′S, 131°16′E) in 1974, but was not recognized as a meteorite until 1989. One weathered individual was recovered with a total mass of 3.38 kg. The bulk composition and petrography of Maralinga indicate that it is a metamorphosed (petrographic type 4) carbonaceous chondrite with major similarities to the Vigarano-subtype. However, recent trace element data from the literature suggest that Maralinga should be included with the CK (Karoonda-type) carbonaceous chondrites. We classify Maralinga as an anomalous CK4 chondrite because of its abundant chondrules and refractory inclusions relative to other known members of the CK group. Maralinga contains homogeneous silicates, including Ni-bearing olivines (Fa34), high-Ca clinopyroxene, and rare orthopyroxene. Plagioclase is chemically heterogeneous and falls into two distinct compositional groups one of ~ An20 and an ~ An80 group. Highly oxidizing conditions during metamorphism of Maralinga are indicated by the abundance of magnetite and the paucity of Fe-Ni metal. 相似文献
966.
967.
968.
Superhumps in low-mass X-ray binaries 总被引:1,自引:0,他引:1
C. A. Haswell A. R. King J. R. Murray P. A. Charles 《Monthly notices of the Royal Astronomical Society》2001,321(3):475-480
We propose a mechanism for the superhump modulations observed in optical photometry of at least two black-hole X-ray transients (SXTs). As in extreme mass-ratio cataclysmic variables (CVs), superhumps are assumed to result from the presence of the 3:1 orbital resonance in the accretion disc. This causes the disc to become non-axisymmetric and precess. However, the mechanism for superhump luminosity variations in low-mass X-ray binaries (LMXBs) must differ from that in CVs, where it is attributed to a tidally-driven modulation of the disc's viscous dissipation, varying on the beat between the orbital and disc precession period. By contrast in LMXBs, tidal dissipation in the outer accretion disc is negligible: the optical emission is overwhelmingly dominated by reprocessing of intercepted central X-rays. Thus a different origin for the superhump modulation is required. Recent observations and numerical simulations indicate that in an extreme mass-ratio system the disc area changes on the superhump period. We deduce that the superhumps observed in SXTs arise from a modulation of the reprocessed flux by the changing area. Therefore, unlike the situation in CVs, where the superhump amplitude is inclination-independent, superhumps should be best seen in low-inclination LMXBs, whereas an orbital modulation from the heated face of the secondary star should be more prominent at high inclinations. Modulation at the disc precession period (10 s of days) may indicate disc asymmetries such as warping. We comment on the orbital period determinations of LMXBs, and the possibility and significance of possible permanent superhump LMXBs. 相似文献
969.
Moody Rachel Schmidt Brian Alcock Charles Goldader Jeffrey Axelrod Tim Cook Kem H. Marshall Stuart 《Earth, Moon, and Planets》2003,92(1-4):125-130
We present preliminary results of the analysis of the first 500 squaredegrees of the Southern Edgeworth-Kuiper belt Survey, a large sky survey whichran from January 2000 to January 2003 and comprises 2900° in total. Early testspredict that we should discover ~10 bright TNOs in our data, doubling the currentknown population. 相似文献
970.