全文获取类型
收费全文 | 2951篇 |
免费 | 395篇 |
国内免费 | 486篇 |
专业分类
测绘学 | 262篇 |
大气科学 | 883篇 |
地球物理 | 452篇 |
地质学 | 408篇 |
海洋学 | 363篇 |
天文学 | 929篇 |
综合类 | 144篇 |
自然地理 | 391篇 |
出版年
2024年 | 13篇 |
2023年 | 25篇 |
2022年 | 61篇 |
2021年 | 85篇 |
2020年 | 72篇 |
2019年 | 75篇 |
2018年 | 72篇 |
2017年 | 76篇 |
2016年 | 79篇 |
2015年 | 108篇 |
2014年 | 131篇 |
2013年 | 140篇 |
2012年 | 131篇 |
2011年 | 141篇 |
2010年 | 118篇 |
2009年 | 248篇 |
2008年 | 206篇 |
2007年 | 247篇 |
2006年 | 209篇 |
2005年 | 203篇 |
2004年 | 183篇 |
2003年 | 168篇 |
2002年 | 156篇 |
2001年 | 130篇 |
2000年 | 98篇 |
1999年 | 93篇 |
1998年 | 98篇 |
1997年 | 76篇 |
1996年 | 67篇 |
1995年 | 69篇 |
1994年 | 55篇 |
1993年 | 48篇 |
1992年 | 30篇 |
1991年 | 34篇 |
1990年 | 19篇 |
1989年 | 19篇 |
1988年 | 17篇 |
1987年 | 9篇 |
1986年 | 5篇 |
1985年 | 1篇 |
1984年 | 3篇 |
1983年 | 2篇 |
1982年 | 1篇 |
1981年 | 1篇 |
1980年 | 5篇 |
1979年 | 1篇 |
1978年 | 2篇 |
1977年 | 1篇 |
1954年 | 1篇 |
排序方式: 共有3832条查询结果,搜索用时 15 毫秒
401.
丘陵区土壤热通量遥感估算模型适应性分析 总被引:1,自引:0,他引:1
利用具有丘陵区典型特征的四川省乐至县气象站的土壤热通量和净辐射观测数据,分析了二者的变化特征,并验证了土壤热通量遥感估算模型的适用性。分析结果表明:晴空土壤热通量G与净辐射Rn存在明显日变化,最大值出现13时左右;其比值G/Rn受土壤湿润程度和地表覆盖的影响,地表湿润、覆盖率高,比值小。在干旱时,瞬时比值可高达0.7,而湿润情况,可低至0.05。对目前广泛使用的G/Rn卫星遥感模型估算结果与实测值的对比分析表明,不同的G/Rn卫星遥感估算模型估算结果存在明显的差异,仅依靠植被指数的模型不适合南方丘陵区。本研究认为Bastiaanssen等的模型较适合丘陵区的土壤热通量遥感估算模型。 相似文献
402.
403.
Climatic characteristics of broadband solar radiation (Rs) in Chinese arid and semi-arid areas are reported in this study. The annual average daily Rs in the arid and semi-arid areas is 16.3 ±5.77 and 15.3 ± 5.16 MJ m^-2 d^-1, respectively. The highest value (17.2 ± 5.84 MJ m^-2 d^-1) appears in an arid area at Linze. The lowest value appears in the semi-arid area of Ansai. Pronounced seasonal variation of Rs is observed with the highest value in summer and the lowest in winter. The clearness index showed similar seasonal pattern at most sites, with the minimum observed in the summer and the highest values in winter at both arid and semi-arid areas. The seasonal variation of the ratio of Rs to its extraterrestrial value Kt in the arid area is more significant than that observed in the semi-arid region, and it is caused by the different range of variation of water vapor between arid and semi-arid areas. The seasonal fluctuations in Rs and Kt are mainly controlled by the water vapor content in these areas. The aerosol particles have significant influence on Rs and Kt at stations with higher aerosol burden. 相似文献
404.
Arbab I. Arbab 《Astrophysics and Space Science》2009,323(2):181-184
In the framework of unifying gravity and electromagnetism, we have shown that accelerating objects emit gravitational wave
as those determined by Larmor formula for the accelerating charged particle. We have found new formulae for the power of Gravitational
waves radiated by spinning and orbiting objects. The minimum wavelength of the gravitational wave emitted by an object of
mass m and radius R is
. 相似文献
405.
Geraint J. A. Harker Saleem Zaroubi Rajat M. Thomas Vibor Jeli Panagiotis Labropoulos Garrelt Mellema Ilian T. Iliev Gianni Bernardi Michiel A. Brentjens A. G. de Bruyn Benedetta Ciardi Leon V. E. Koopmans V. N. Pandey reas H. Pawlik Joop Schaye Sarod Yatawatta 《Monthly notices of the Royal Astronomical Society》2009,393(4):1449-1458
Detecting redshifted 21-cm emission from neutral hydrogen in the early Universe promises to give direct constraints on the epoch of reionization (EoR). It will, though, be very challenging to extract the cosmological signal (CS) from foregrounds and noise which are orders of magnitude larger. Fortunately, the signal has some characteristics which differentiate it from the foregrounds and noise, and we suggest that using the correct statistics may tease out signatures of reionization. We generate mock data cubes simulating the output of the Low Frequency Array (LOFAR) EoR experiment. These cubes combine realistic models for Galactic and extragalactic foregrounds and the noise with three different simulations of the CS. We fit out the foregrounds, which are smooth in the frequency direction, to produce residual images in each frequency band. We denoise these images and study the skewness of the one-point distribution in the images as a function of frequency. We find that, under sufficiently optimistic assumptions, we can recover the main features of the redshift evolution of the skewness in the 21-cm signal. We argue that some of these features – such as a dip at the onset of reionization, followed by a rise towards its later stages – may be generic, and give us a promising route to a statistical detection of reionization. 相似文献
406.
Kirsty J. Rhook Paul M. Geil J. Stuart B. Wyithe 《Monthly notices of the Royal Astronomical Society》2009,392(4):1388-1396
It has recently been suggested that the power spectrum of redshifted 21 cm fluctuations could be used to measure the scale of baryonic acoustic oscillations (BAOs) during the reionization era. The resulting measurements are potentially as precise as those offered by the next generation of galaxy redshift surveys at lower redshift. However, unlike galaxy redshift surveys, which in the linear regime are subject to a scale-independent galaxy bias, the growth of ionized regions during reionization is thought to introduce a strongly scale-dependent relationship between the 21 cm and mass power spectra. We use a seminumerical model for reionization to assess the impact of ionized regions on the precision and accuracy with which the BAO scale could be measured using redshifted 21 cm observations. For a model in which reionization is completed at z ∼ 6 , we find that the constraints on the BAO scale are not systematically biased at z ≳ 6.5 . In this scenario, and assuming the sensitivity attainable with a low-frequency array comprising 10 times the collecting area of the Murchison Widefield Array, the BAO scale could be measured to within 1.5 per cent in the range 6.5 ≲ z ≲ 7.5 . 相似文献
407.
Brian J. Morsony Jared C. Workman Davide Lazzati Mikhail V. Medvedev 《Monthly notices of the Royal Astronomical Society》2009,392(4):1397-1402
We consider radiation emitted by the jitter mechanism in a Blandford–McKee self-similar blastwave. We assume the magnetic field configuration throughout the whole blastwave meets the condition for the emission of jitter radiation and we compute the ensuing images, light curves and spectra. The calculations are performed for both a uniform and a wind environment. We compare our jitter results to synchrotron results. We show that jitter radiation produces slightly different spectra than synchrotron, in particular between the self-absorption and the peak frequency, where the jitter spectrum is flat, while the synchrotron spectrum grows as ν1/3 . The spectral difference is reflected in the early decay slope of the light curves. We conclude that jitter and synchrotron afterglows can be distinguished from each other with good quality observations. However, it is unlikely that the difference can explain the peculiar behaviour of several recent observations, such as flat X-ray slopes and uncorrelated optical and X-ray behaviour. 相似文献
408.
Patrick Weltevrede Geoff Wright 《Monthly notices of the Royal Astronomical Society》2009,395(4):2117-2126
We present a geometric study of the radio and γ-ray pulsar B1055−52 based on recent observations at the Parkes radio telescope. We conclude that the pulsar's magnetic axis is inclined at an angle of 75° to its rotation axis and that both its radio main pulse and interpulse are emitted at the same height above their respective poles. This height is unlikely to be higher or much lower than 700 km, a typical value for radio pulsars.
It is argued that the radio interpulse arises from emission formed on open fieldlines close to the magnetic axis which do not pass through the magnetosphere's null (zero-charge) surface. However, the main pulse emission must originate from fieldlines lying well outside the polar cap boundary beyond the null surface, and farther away from the magnetic axis than those of the outer gap region where the single γ-ray peak is generated. This casts doubt on the common assumption that all pulsars have closed, quiescent, corotating regions stretching to the light cylinder. 相似文献
It is argued that the radio interpulse arises from emission formed on open fieldlines close to the magnetic axis which do not pass through the magnetosphere's null (zero-charge) surface. However, the main pulse emission must originate from fieldlines lying well outside the polar cap boundary beyond the null surface, and farther away from the magnetic axis than those of the outer gap region where the single γ-ray peak is generated. This casts doubt on the common assumption that all pulsars have closed, quiescent, corotating regions stretching to the light cylinder. 相似文献
409.
We constrain the distance of the gamma-ray burst (GRB) prompt emission site from the explosion centre R , by determining the location of the electron's self-absorption frequency in the GRB prompt optical-to-X/γ-ray spectral energy distribution, assuming that the optical and the γ-ray emissions are among the same synchrotron radiation continuum of a group of hot electrons. All possible spectral regimes are considered in our analysis. The method has only two assumed parameters, namely the bulk Lorentz factor of the emitting source Γ and the magnetic field strength B in the emission region (with a weak dependence). We identify a small sample of four bursts that satisfy the following three criteria: (1) they all have simultaneous optical and γ-ray detections in multiple observational time intervals, (2) they all show temporal correlations between the optical and γ-ray light curves and (3) the optical emission is consistent with belonging to the same spectral component as the γ-ray emission. For all the time intervals of these four bursts, it is inferred that R ≥ 1014 (Γ/300)3/4 ( B /105 G)1/4 cm. For a small fraction of the sample, the constraint can be pinned down to R ≈ 1014 –1015 cm for Γ∼ 300 . For a second sample of bursts with prompt optical non-detections, only upper limits on R can be obtained. We find no inconsistency between the R -constraints for this non-detection sample and those for the detection sample. 相似文献
410.
During the few days centered about new Moon, the lunar surface is optically hidden from Earth-based observers. However, the Moon still offers an observable: an extended sodium tail. The lunar sodium tail is the escaping “hot” component of a coma-like exosphere of sodium generated by photon-stimulated desorption, solar wind sputtering and meteoroid impact. Neutral sodium atoms escaping lunar gravity experience solar radiation pressure that drives them into the anti-solar direction forming a comet-like tail. During new Moon time, the geometry of the Sun, Moon and Earth is such that the anti-sunward sodium flux is perturbed by the terrestrial gravitational field resulting in its focusing into a dense core that extends beyond the Earth. An all-sky camera situated at the El Leoncito Observatory (CASLEO) in Argentina has been successfully imaging this tail through a sodium filter at each lunation since April 2006. This paper reports on the results of the brightness of the lunar sodium tail spanning 31 lunations between April 2006 and September 2008. Brightness variability trends are compared with both sporadic and shower meteor activity, solar wind proton energy flux and solar near ultra violet (NUV) patterns for possible correlations. Results suggest minimal variability in the brightness of the observed lunar sodium tail, generally uncorrelated with any single source, yet consistent with a multi-year period of minimal solar activity and non-intense meteoric fluxes. 相似文献