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411.
412.
M. Miceli A. Decourchelle J. Ballet F. Bocchino J. Hughes U. Hwang R. Petre 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(3):390-395
In the framework of the study of supernova remnants and their complex interaction with the interstellar medium and the circumstellar material, we focus on the galactic supernova remnant W49B. Its morphology exhibits an X-ray bright elongated nebula, terminated on its eastern end by a sharp perpendicular structure aligned with the radio shell. The X-ray spectrum of W49B is characterized by strong K emission lines from Si, S, Ar, Ca, and Fe. There is a variation of the temperature in the remnant with the highest temperature found in the eastern side and the lowest one in the western side. The analysis of the recent observations of W49B indicates that the remnant may be the result of an asymmetric bipolar explosion where the ejecta are collimated along a jet-like structure and the eastern jet is hotter and more Fe-rich than the western one. Another possible scenario associates the X-ray emission with a spherical explosion where parts of the ejecta are interacting with a dense belt of ambient material. To overcome this ambiguity we present new results of the analysis of an XMM-Newton observation and we perform estimates of the mass and energy of the remnant. We conclude that the scenario of an anisotropic jet-like explosion explains quite naturally our observation results, but the association of W49B with a hypernova and a γ-ray burst, although still possible, is not directly supported by any evidence. 相似文献
413.
Evolution and composition of baryonic matter is influenced by the evolution of other forms of matter and energy in the universe.
At the time of primordial nucleosynthesis the universal expansion and thus the decrease of the density and temperature of
baryonic matter were controlled by leptons and photons. Non-baryonic dark matter initiated the formation of clusters and galaxies,
and to this day, dark matter largely determines the dynamics and geometries of these baryonic structures and indirectly influences
their chemical evolution. Chemical analyses and isotopic abundance measurements in the solar system established the composition
in the protosolar cloud (PSC). The abundances of nuclear species in the PSC led to the discovery of the magic numbers and
the nuclear shell model, and they allowed the identification of nucleosynthetic sites and processes. To this day, we know
the abundances of the ∼300 stable and long-lived nuclides infinitely better in the PSC than in any other sample of matter
in the universe. Thus, we know the exact composition of a Galactic sample of intermediate age, allowing us to check on theories
of Galactic evolution before and after the formation of the solar system. This paper specifically discusses the nucleosynthesis
in the early universe and the Galactic evolution during the last 5 Gyr. 相似文献
414.
刘景旺 《华北航天工业学院学报》2007,(1)
本文报导了通过结合自行制备的掺铈钒酸钇晶体(Ce3 :YVO4)荧光粉与InGaN/GaN蓝光发光二极管(LED)结合而得的白光发光二极管(W-LED)。在室温、正向电压3.5V、正向电流20mA时W-LED的CIE色坐标为(0.32,0.37),接近纯白色(0.33,0.33)。 相似文献
415.
G. P. Chernov 《Space Science Reviews》2006,127(1-4):195-326
This review covers fairly comprehensively experimental and theoretical research on the fine structure of types zebra pattern
(ZP) and fiber bursts (FB) in solar type II + IV radio bursts. The basic attention is given to the latest experimental data.
A comparative analysis of several recent solar type IV radio outbursts with these fine structure in dynamical radio spectra
is carried out using available ground-based and satellite data (Yohkoh, SOHO, TRACE, RHESSI). New data on microwave zebra
structures and fiber bursts testifies that they are analogous to similar structures observed at meter wavelengths. The discovery
of the superfine structure, in the form of millisecond spikes is the most significant new effect in the cm range. All basic
theoretical models of the zebra pattern and fiber bursts are discussed critically. Two main models are studied for their interpretation:
(i) interactions between electrostatic plasma waves and whistlers, (ii) radio emission at double plasma resonance (DPR). The
relative significance of several possible mechanisms remains uncertain. 相似文献
416.
We present a preliminary analysis of two quiet Sun transition region areas observed with the SOHO/SUMER spectrometer, using
lines from oxygen, nitrogen and silicon. The average quiet Sun physical parameters are studied as a function of line intensity.
Systematic variations of line position and width with increasing intensity are found. A large number of small-scale active
points have been observed, and preliminary analysis of the physical properties and dynamics of these active features is presented.
A jet-like structure, found in an active point, is also investigated and its velocity along the line of sight determined.
This revised version was published online in June 2006 with corrections to the Cover Date. 相似文献
417.
Jeongwoo Lee 《Space Science Reviews》2007,133(1-4):73-102
Solar active region coronae are known for strong magnetic fields permeating tenuous plasma, which makes them an ideal astronomical
laboratory for magnetohydrodynamics research. It is, however, relatively less known that this physical condition also permits
a very efficient radiation mechanism, gyro-resonant emission, produced by hot electrons gyrating in the coronal magnetic field.
As a resonant mechanism, gyro-emission produces high enough opacity to fully reveal the coronal temperature, and is concentrated
at a few harmonics of the local gyrofrequency to serve as an excellent indicator of the magnetic field. In addition, the polarization
of the ubiquitous free–free emission and a phenomenon of depolarization due to mode coupling extend the magnetic field diagnostic
to a wide range of coronal heights. The ability to measure the coronal temperature and magnetic field without the complications
that arise in other radiative inversion problems is a particular advantage for the active region radio emissions available
only at these wavelengths. This article reviews the efforts to understand these radiative processes, and use them as diagnostic
tools to address a number of critical issues involved with active regions. 相似文献
418.
R. A. Mewaldt C. M. S. Cohen G. M. Mason A. C. Cummings M. I. Desai R. A. Leske J. Raines E. C. Stone M. E. Wiedenbeck T. T. von Rosenvinge T. H. Zurbuchen 《Space Science Reviews》2007,130(1-4):207-219
Although the average composition of solar energetic particles (SEPs) and the bulk solar wind are similar in a number of ways,
there are key differences which imply that solar wind is not the principal seed population for SEPs accelerated by coronal
mass ejection (CME) driven shocks. This paper reviews these composition differences and considers the composition of other
possible seed populations, including coronal material, impulsive flare material, and interplanetary CME material. 相似文献
419.
ATLAS是一种高级测试语言,它对测试需求的描述不局限于任何特殊测试系统.文中对ATLAS的语言元素、数据类型、语句结构、测试需求结构等进行了简要介绍. 相似文献
420.
We present relative carbon and oxygen abundances derived via an optically thin recombination line analysis for five WO stars, and compare the derived abundances to recent evolutionary models. New recombination coefficients for O4+, O5+ and O6+ ions have allowed total oxygen abundances to be derived. The final C/He values range between 0.4 and 0.8 by number, consistent with C/He ratios previously derived for WC stars. O/He values range between 0.1–0.4, with C/O ratios between 2.1–4.8.A comparison of the derived abundances with the evolutionary models of Maeder (1990) and Schaller et al. (1992) shows promising agreement. We find reasonably tight agreement between the abundances derived for the WO stars. The degree of enhancement for the oxygen abundances in regions of low metallicity predicted by Maeder (1990) is not corroborated by our results.Additionally we present a revised, quantified classification scheme for WO subtypes. We extend the class to lower excitation, WO5, and place MS 4 (=WR 30a) in this class. Equivalent widths of the strongest lines of MS 4 are also presented. Finally, we present new observations of DR 1, a WO3 star located in the dwarf irregular galaxy IC 1613. 相似文献