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991.
The possible cosmological variation of the proton-to-electron mass ratio μ = m p/m e was estimated by measuring the H2 wavelengths in the spectra of distant quasars. We analyze high-resolution (FWHM≈7 km s?1) spectra of the two damped Lyman-α systems at redshifts z abs=2.3377 and 3.0249 observed in the spectra of the quasars Q 1232+082 and Q 0347?382, respectively. Our analysis yielded the most conservative estimate for the possible variation of μ in the past ~ 10 Gyr, Δμ/μ = (5.7 ± 3.8) × 10?5. Since the significance of this result does not exceed 1.5σ, further observations are needed to increase the statistical significance. This is the most stringent limit on the possible cosmological variation of μ to date. 相似文献
992.
本法以硫酸、硝酸和高氯酸为氧化剂,加热氧化破坏试样中存在的品质和非晶质炭。一般10g试样需用8—10ml H_2SO_4、0.2ml HNO_3和1ml高氯酸。将试样与混合酸共热20min,即可达到破坏试样中炭的目的。然后用王水分解样品,聚醚型聚氨酯泡沫塑料富集,硫脲解脱,原子吸收测定金。 相似文献
993.
麦阔里岛和戴维斯站分别位于极光带中心和极光带极向边缘区内.这两处的极光吸收次数在晚间多些,其中突然性吸收主要出现在午夜(当地地磁时间)前,缓变性吸收在午夜后.极光吸收与太阳的活动性密切相关.太阳风高能粒子主要沉降在极光中心带磁午夜区,然后向东西与南北方向扩散,以向西的电射流为主,向东的为辅.但向西的弱些、速度慢些;向东的强些、速度快些.太阳活动增强后,尤其是强的X耀斑事件后,向西的电射流增多增强.另外,在较高磁纬地区的戴维斯站,冬季时极光吸收增多增强.但在极光中心区的麦阔里岛观测站,基本上无此种季节效应.这可能是由于冬季(对南半球而言)极光卵向南偏移造成的. 相似文献
994.
P.J. Outram R.J. Smith T. Shanks B.J. Boyle S.M. Croom N.S. Loaring L. Miller 《Monthly notices of the Royal Astronomical Society》2001,328(3):805-809
We examine the highest signal-to-noise ratio spectra from the 2dF QSO Redshift Survey (2QZ) 10k release and identify over 100 new low-ionization heavy-element absorbers: damped Lyman α (DLA) candidates suitable for higher-resolution follow-up observations. These absorption systems map the spatial distribution of high- z metals in exactly the same volumes as the foreground 2QZ QSOs themselves sample and hence the 2QZ gives us the unique opportunity to compare directly the two tracers of large-scale structure. We examine the cross-correlation of the two populations to see how they are relatively clustered, and, by considering the colour of the QSOs, detect a small amount of dust in these metal systems. 相似文献
995.
Poonam Chandra Govind Swarup Vasant K. Kulkarni Nimisha G. Kantharia 《Journal of Astrophysics and Astronomy》2004,25(1-2):57-65
We have made observations of the as sociated HI absorption of a high redshift radio galaxy 0902+34 atz = 3.395 with the Giant Meterwave Radio Telescope in the 323 ± 1 MHz band. We find a narrow absorption line with a flux density
of 11.5 mJy at a redshift of 3.397 consistent with that observed by Usonet al. (1991), Briggset al. (1993) and de Bruyn (1996). A weak broad absorption feature reported by de Bruyn (1996) has not been detected in our observations.
We also place an upper limit of 4mJy(2σ) on emission line strength at the position where Usonet al. (1991) claimed to have found a narrow emission line. 相似文献
996.
Semih Küçükarslan 《国际地质力学数值与分析法杂志》2004,28(9):963-980
In this paper, time-domain dynamic analysis of dam–reservoir–foundation interaction is presented by coupling the dual reciprocity boundary element method (DRBEM) in the infinite reservoir and foundation domain and the finite element method in the finite dam domain. An efficient coupling procedure is formulated by using the sub-structuring method. The effects of the reservoir bottom absorption are included in the formulations. Sharan's boundary condition for the far-end of the infinite fluid domain is implemented. To verify the proposed scheme, numerical examples are carried out by comparing with the available exact solutions and finite–finite element coupling results for the dam–reservoir interaction. A complete dam–reservoir–foundation interaction is also studied by including the bottom absorption effects. Copyright © 2004 John Wiley & Sons, Ltd. 相似文献
997.
A. Skopal M. F. Bode M. Bryce J. Meaburn S. Tamura 《Astrophysics and Space Science》1995,224(1-2):559-560
We present optical high-resolution spectroscopy and UBV photometry of the symbiotic binary CH Cyg during the current outburst which began in 1992 February. 相似文献
998.
999.
C. Camy-Peyret B. Bergovist B. Galle M. Carleer C. Clerbaux R. Colin C. Fayt F. Goutail M. Nunes-Pinharanda J. P. Pommereau M. Hausmann U. Platt I. Pundt T. Rudolph C. Hermans P. C. Simon A. C. Vandaele J. M. C. Plane N. Smith 《Journal of Atmospheric Chemistry》1996,23(1):51-80
The results of an intercomparison campaign of eight different long path UV-visible DOAS instruments measuring NO2, O3 and SO2 concentrations in a moderately polluted urban site are presented. For effective optical path lengths of 230 and 780 m the overall spread of these measurements (±1) are 5×1010, 6×1010 and 1×1010 molec·cm-3 (2.0, 2.4, and 0.4 ppb) for these molecules respectively when all instruments used a common set of absorption cross sections. The remaining differences are not completely random and the systematic differences are attributed to the different retrieval methods used for each instrument. 相似文献
1000.
Naphthalene (C10H8), several other hydrocarbons, mostly derivates of naphthalene, and bromine oxide (BrO) were analyzed for narrow band (0.01 nm) absorption lines in the wavelength range between 307.7 and 308.3 nm to study their potential impact on OH radical measurements by differential absorption spectroscopy.Only naphthalene showed narrow band absorption lines in this wavelength region. From nine naphthalene lines the differential absorption cross-section was determined.The strongest naphthalene line at 308.002 nm is close to the Q
1(2) OH line, but about a factor of 200 weaker (=(65.2±15.3)×10-20 cm2/molec). The corresponding detection limit for naphthalene is about 15 ppt. We re-evaluated some spectra of our OH measurement campaign in July 1987 with respect to naphthalene and obtained an upper limit of 30 ppt for its concentration.BrO was recorded in the larger wavelength interval between 307.7 and 308.7 nm. Structured absorptions were only observed at wavelengths above 308.2 nm and no significant structures were found in the vicinity of the Q
1(2) and Q
1(3) OH lines. 相似文献