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141.
The observations of X-ray Type II bursts from the low-mass X-ray binary MXB 1730-335 can be explained by a particular form of magnetic gating in the presence of steady external accretion. The requirements are a strong magnetic field of the neutron star (7×1011–2×1012 gauss at the surface), rotational symmetry and alignment of the field axis with the axis of a steadily accreting disk to within 6°. 相似文献
142.
本文利用GOES-7卫星的1分钟记录资料研究了1991年3月和6月期间6个大X耀斑伴随的软X射线爆发特性和源强度的关系。结果指出:对X射线耀斑,其射线辐射流量上升快的在日冕中激起的激波速度也较快.数值模拟研究指出,这可能反映爆发能量释放速率是源强度的主要指标. 相似文献
143.
144.
145.
T. G. Tsuru T. Tanimori A. Bamba K. Imanishi K. Koyama H. Kubo H. Matsumoto K. Miuchi M. Nagayoshi R. Orito A. Takada S. Takagi M. Tsujimoto M. Ueno H. Tsunemi K. Hayashida E. Miyata 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2688-2690
We propose a new type of wide band X-ray imaging spectrometer as a focal plane detector of the super mirror onboard on future X-ray missions including post Astro-E2. This camera is realized by the hybrid of back illumination CCDs and a back supportless CCD for 0.05–10 keV band, and a Micro Pixel Gas Chamber detecting X-rays at 10–80 keV. 相似文献
146.
R.L.C. Starling E.M. Puchnarewicz E. Romero-Colmenero K.O. Mason 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2004,34(12):2588-2593
We present a series of monitoring observations of the ultrasoft broad-line Seyfert galaxy RE J2248-511 with XMM-Newton. Previous X-ray observations showed a transition from a very soft state to a harder state five years later. We find that the ultrasoft X-ray excess has re-emerged, yet there is no change in the hard power-law. Reflection models with a reflection fraction of 15, and Comptonisation models with two components of different temperatures and optical depths (kT1 = 83 keV, T1 = 30 eV, τ1 = 0.8; KT2 = 3.5 keV, T2 = 60 eV, τ2 = 2.8) can be fit to the spectrum, but cannot be constrained. The best representation of the spectrum is a model consisting of two blackbodies (kT1 = 0.09 ± 0.01 keV, kT2 = 0.21 ± 0.03 keV) plus a power-law (Γ = 1.8 ± 0.08). We also present simultaneous optical and infrared data showing that the optical spectral slope also changes dramatically on timescales of years. If the optical to X-ray flux comes primarily from a Comptonised accretion disk we obtain estimates for the black hole mass , accretion rate and inclination cos(i) 0.8 of the disk. 相似文献
147.
M. Nakajima T. Mihara K. Makishima H. Niko 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2006,38(12):2756-2758
We report on the luminosity dependent change of the cyclotron resonance energy obtained from a transient X-ray pulsar, 4U 0115+63. Using RXTE data observed on 1999 March, we found that the fundamental resonance energy stayed constant (11 keV) when the source luminosity was above 5 × 1037 erg s−1. As the luminosity decreased below 5 × 1037 erg s−1, the fundamental resonance energy gradually increased up to 16 keV at 0.16 × 1037 erg s−1. The luminosity dependence of the resonance energy can be understood by the change of the accretion column height. 相似文献
148.
F. Frontera D. Dal Fiume W. Dusi E. Morelli G. Spada G. Ventura 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
The transient X-ray pulsar A0535+26 was observed on October 4, 1980 during a high level intensity outburst with a balloon borne hard X-ray detector. High statistical quality source spectra were determined up to 100 keV. Both blackbody and Wien laws fit well the data. Pulse phase spectroscopy shows variation of temperature index between 7.5 and 8.5 keV in the off source spectra and between 7.4 and 10.5 keV in the off pulse spectra. The time averaged luminosity above 30 keV is 8×1036 erg/s. 相似文献
149.
The X-ray Nova GRO J0422+32 in its low brightness has been identified with a B 21
m
, R20
m
star on Palomar Sky Survey glass copies. The scans obtained with an automatical microdensitometer along with our special PC program were used. The resulting outburst amplitude 8
m
is one of similarity features for the class of the low mass X-ray Novae, black hole candidates. 相似文献
150.
Peter W. A. Roming Thomas E. Kennedy Keith O. Mason John A. Nousek Lindy Ahr Richard E. Bingham Patrick S. Broos Mary J. Carter Barry K. Hancock Howard E. Huckle S D. Hunsberger Hajime Kawakami Ronnie Killough T Scott Koch Michael K. Mclelland Kelly Smith Philip J. Smith Juan Carlos Soto Patricia T. Boyd Alice A. Breeveld Stephen T. Holland Mariya Ivanushkina Michael S. Pryzby Martin D. Still Joseph Stock 《Space Science Reviews》2005,120(3-4):95-142
The Ultra-Violet/Optical Telescope (UVOT) is one of three instruments flying aboard the Swift Gamma-ray Observatory. It is designed to capture the early (∼1 min) UV and optical photons from the afterglow of gamma-ray
bursts in the 170–600 nm band as well as long term observations of these afterglows. This is accomplished through the use
of UV and optical broadband filters and grisms. The UVOT has a modified Ritchey–Chrétien design with micro-channel plate intensified
charged-coupled device detectors that record the arrival time of individual photons and provide sub-arcsecond positioning
of sources. We discuss some of the science to be pursued by the UVOT and the overall design of the instrument. 相似文献