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1.
Chromospheric lines, including Ha, Lyα, Lyβand CaⅡK, CaⅡ8542, are systemically and quantitatively investigated with respect to the non-thermal excitation and ionization due to particle beam bombardment for a series of solar semi-empirical atmospheric models. As a result we propose to use the contrast in the integrated intensity of hydrogen lines to estimate the total energy flux of the bombarding beam during the solar flare impulsive phase. Partial frequency redistribution is considered in the Lyαline calculation and a smaller intensity enhancement in the Ha line-centers is found than in the previous results of Fang et al.  相似文献   
2.
Super-active region NOAA 6555 was highly flare productive during the period March 21st–27th, 1991 of its disk passage. We have st udied its chromospheric activity using high spatial resolution Hα filtergrams taken at Udaipur along with MSFC vector magnetograms. A possible relationship of flare productivity and the variation in shear has been explored. Flares were generally seen in those subareas of the active region which possessed closed magnetic field configuration, whereas only minor flares and/or surges occurred in subareas showing open magnetic field configuration. Physical mechanisms responsible for the observed surges are also discussed.  相似文献   
3.
本文分析了云南天文台10m射电望远镜在2lcm波段上观测到的一次尖峰辐射事件,这次事件发生在5629活动区(S16W109),它伴随了X2·9/SF耀斑及边缘耀斑环,并且有质子流量的上升和一次罕见的地磁场突然反相脉冲与之对应.我们从耀斑环的Hβ照片可以看出,在尖峰辐射发生前,原先存在的耀斑环的顶部开始变亮,而尖峰开始后环顶亮度达到极大,说明这次尖峰辐射与耀斑环顶部增亮有关,辐射很可能来自环顶.从尖峰事件的时间轮廓得到的FFT功率谱表明存在150ms的准周期脉动.按照Mclean等人的模型,即脉动是由俘获在磁通管内的电子的径向振荡引起,可以推断,这次尖峰辐射与Fermi机制激发快速电子有关,且尖峰的发生需要被俘获的电子.此外,我们将这次尖峰事件分解为几百个元耀斑爆发(EFB),并且讨论了这些EFB的性质.  相似文献   
4.
We present radio interferometric observations of the Algol-type binary system RZ Cassiopeiae made with the VLA and MERLIN arrays at 6 cm over an incomplete orbital cycle of the system (1.195 d). We detected RZ Cas with both instruments. The images were unresolved in both cases, with angular extents comparable to the synthesized beams. The peak flux density in the VLA image was 1.14 mJy beam−1 and in the MERLIN image it was 0.93 mJy beam−1. The derived brightness temperatures are  4.02 × 108  and  4.35 × 108 K  and the effective electron energies are 0.347 and 0.346 MeV for the MERLIN and VLA data respectively. The radio light curve shows an interesting modulation centred close to the primary eclipse which seems to correlate with ASCA SIS observations of the system. The results can be interpreted as an emitting region on the outer hemisphere of the cool component aligned along the centroid axis of the binary system.  相似文献   
5.
Summary From the early discovery in 1948 of X-rays from the Solar corona, X-ray spectroscopy has proven to be an invaluable tool in studying hot astrophysical and laboratory plasmas. Because the emission line spectra and continua from optically thin plasmas are fairly well known, high-resolution X-ray spectroscopy has its most obvious application in the measurement of optically thin sources such as the coronae of stars. In particular X-ray observations with theEINSTEIN observatory have demonstrated that soft X-ray emitting coronae are a common feature among stars on the cool side of the Hertzsprung-Russell diagram, with the probable exception of single very cool giant and supergiant stars and A-type dwarfs. Observations with the spectrometers aboardEINSTEIN andEXOSAT have shown that data of even modest spectral resolution (/ = 10–100) permit the identification of coronal material at different temperatures whose existence may relate to a range of possible magnetic loop structures in the hot outer atmospheres of these stars. The higher spectral resolution of the next generation of spectrometers aboard NASA'sAXAF and ESA'sXMM will allow to fully resolve the coronal temperature structure and to enable velocity diagnostics and the determination of coronal densities, from which the loop geometry (i.e. surface filling factors and loop lengths) can be derived. In this paper various diagnostic techniques are reviewed and the spectral results fromEINSTEIN andEXOSAT are discussed. A number of spectral simulations forAXAF andXMM, especially high-resolution iron K-shell, L-shell, and2s-2p spectra in the wavelength regions around 1.9 Å, 10 Å, and 100 Å, respectively, are shown to demonstrate the capabilities for temperature, density, and velocity diagnostics. Finally, iron K-shell spectra are simulated for various types of detectors such as microcalorimeter, Nb-junction, and CCD.  相似文献   
6.
理学3080E3型X射线荧光光谱仪维修实例   总被引:2,自引:0,他引:2  
唐晓慧 《岩矿测试》2005,24(3):237-238
介绍理学3080E3型X射线荧光光谱仪样品驱动单元及高压发生器部分的故障现象及维修实例。  相似文献   
7.
太阳耀斑的GPS监测方法及实例分析   总被引:3,自引:1,他引:3  
利用GPS伪距与载波相位联合数据处理的方法,分析了2000年7月14日太阳耀斑爆发期间,武汉、北京、乌鲁木齐GPS观测数据得到的电离层TEC,提出了利用多项式拟合计算由耀斑引起的电离层TEC增加量的方法。  相似文献   
8.
气球携带碘化银焰弹技术研究   总被引:1,自引:1,他引:1       下载免费PDF全文
秦长学 《气象》1997,23(11):11-13
主要介绍在北京地区开展气球携带碘化银焰弹雨雪作业的作业技术,经济效益等问题。通过各种增雨雪技术比较,认敢球携带碘化银焰弹增雨雪作业在北方干旱地区的抗旱工作中或作为收音机增雨雪作业的补充手段具有应用价值  相似文献   
9.
冯桂力  陈文选  刘文 《气象》1997,23(12):3-8
利用二维雹云模拟济南地区1996年7月24日出现的一次冰雹过程,模拟结果表明对雹云26个主要微物理过程双参数化较细致地描述对流过程的热,动力反馈和微物理特点2。根据计算结果,对该次冰雹过程进行了AgI催化试验,结果得出在云发展初期对暖底雹云实施高浓度的冰晶催化,可起到减少地面冰雹和增加地面降水的作用。  相似文献   
10.
Based on the dynamic framework of WRF and Morrison 2-moment explicit cloud scheme, a salt-seeding scheme was developed and used to simulate the dissipation of a warm fog event during 6–7 November 2009 in the Beijing and Tianjin area. The seeding effect and its physical mechanism were studied. The results indicate that when seeding fog with salt particles sized 80 μm and at a quantity of 6 gm~(-2) at the fog top, the seeding effect near the ground surface layer is negative in the beginning period, and then a positive seeding effect begins to appear at 18 min, with the best effect appearing at 21 min after seeding operation. The positive effect can last about 35 min. The microphysical mechanism of the warm fog dissipation is because of the evaporation due to the water vapor condensation on the salt particles and coalescence with salt particles.The process of fog water coalescence with salt particles contributed mostly to this warm fog dissipation. Furthermore, two series of sensitivity experiments were performed to study the seeding effect under different seeding amounts and salt particles sizes. The results show that seeding fog with salt particles sized of 80 μm can have the best seeding effect, and the seeding effect is negative when the salt particle size is less than 10 μm. For salt particles sized 80 μm, the best seeding effect, with corresponding visibility of 380 m, can be achieved when the seeding amount is 30 g m~(-2).  相似文献   
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