Keywords: Astrophysics; X-ray binaries; Neutron stars; Black holes 相似文献
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811.
In a paper submitted to A&A we present the first line blanketed hydrodynamic models of spherically expanding atmospheres of hot stars. This paper is complementary to the submitted paper. Here, we emphasize the advantages and the weak points of our approach and we present additional technical aspects.The models are characterised by a simultaneous solution of the equation of motion, the non-LTE populations of H and He, and radiation transfer in a line blanketed atmosphere. The entire domain from the optically thick photosphere out to the terminal velocity of the wind is treated. The radiative forces are evaluated consistently with the depth-dependent radiation field, taking into account multiple scattering by metal lines and line overlap. 相似文献
812.
Solar magnetic field is believed to play a central role in solar activities and flares, filament eruptions as well as CMEs
are due to the magnetic field re-organization and the interaction between the plasma and the field. At present the reliable
magnetic field measurements are still confined to a few lower levels like in photosphere and chromosphere. Although IR technique
may be applied to observe the coronal field but the technique is not well-established yet. Radio techniques may be applied
to diagnose the coronal field but assumptions on radiation mechanisms and propagations are needed. Therefore extrapolation
from photospheric data upwards is still the primary method to reconstruction coronal field. Potential field has minimum energy
content and a force-free field can provide the required excess energy for energy release like flares, etc. Linear models have
undesirable properties and it is expected to consider non-constant-alpha force-free field model. As the recent result indicates
that the plasma beta is sandwich-ed distributed above the solar surface (Gary, 2001), care must be taken in modeling the coronal
field correctly. As the reconstruction of solar coronal magnetic fields is an open boundary problem, it is desired to apply
some technique that can incorporate this property. The boundary element method is a well-established numerical techniques
that has been applied to many fields including open-space problems. It has also been applied to solar magnetic field problems
for potential, linear force-free field and non-constant-alpha force-free field problems. It may also be extended to consider
the non-force-free field problem. Here we introduce the procedure of the boundary element method and show its applications
in reconstruction of solar magnetic field problems.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
813.
814.
石磊 《中国民航学院学报》1996,(6):31-38
介绍了国航货运计算机系统的网络拓朴结构、网络需求和网络设计思想.如何使SITA网络和本地局域网连接,解决SNA/LAN的互联方案. 相似文献
815.
对称矩阵反问题解的稳定性 总被引:1,自引:0,他引:1
戴华 《南京航空航天大学学报》1994,26(1):133-139
考虑如下对称矩阵反问题:问题Ⅰ:给定X,B∈R(n×n),求A∈SR(n×n)使得AX=B,其中SR(n×n)={{A|A∈R(n×n),AT=A}。问题Ⅱ:给定,求使得其中是矩阵的Frobenius范数,SA表示问题Ⅰ的解集合。本文讨论问题Ⅰ解的稳定性,给出问题Ⅱ解的扰动界。 相似文献
816.
利用具有紧文集的Datubechies正交小波基函数,构造出了一种新的计算一维波动方程的数值方法——小波解法。由于该方法充分利用了Daubechies小波函数良好的局部性质,并且巧妙地运用了Fourier变换,数值试验表明该方法不但精度高,而且计算量小。 相似文献
817.
E.P.J. van den Heuvel 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2006,38(12):2667-2672
Three recent developments in the field of formation and evolution of neutron stars and black holes in binaries are addressed:
- • The finding that there is a class of neutron stars, formed in interacting binaries, that do not receive kick velocities in their birth events. This finding is particularly important for our understanding of the formation – and formation rates – of double neutron stars. It is argued that these low-kick neutron stars, which tend to have low masses, are formed by a different physical mechanism than the neutron stars that receive large kick velocities at birth.
• The occurrence of velocity kicks in the formation events of stellar black holes.
• The nature of the companions of millisecond X-ray pulsars.
818.
中心频率为175MHz复合布拉格声光器件的设计 总被引:2,自引:1,他引:2
介绍以钼酸铅为声光介质、中心频率为175MHz复合声光器件的设计,计算了以铟为粘合层时换能器带宽并确定了镀层厚度,该器件带宽为120MHz,时间带宽积达1207.5,初步满足声光信号处理的需要。 相似文献
819.
From solar nanoflares to stellar giant flares: Scaling laws and non-implications for coronal heating
Markus J. Aschwanden 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2007,39(12):1867-1875
In this study we explore physical scaling laws applied to solar nanoflares, microflares, and large flares, as well as to stellar giant flares. Solar flare phenomena exhibit a fractal volume scaling, V(L) L1.9, with L being the flare loop length scale, which explains the observed correlation between the total emission measure EMp and flare peak temperature Tp in both solar and stellar flares. However, the detected stellar flares have higher emission measures EMp than solar flares at the same flare peak temperature Tp, which can be explained by a higher electron density that is caused by shorter heating scale height ratios sH/L ≈ 0.04–0.1. Using these scaling laws we calculate the total radiated flare energies EX and thermal flare energies ET and find that the total counts C are a good proxy for both parameters. Comparing the energies of solar and stellar flares we find that even the smallest observed stellar flares exceed the largest solar flares, and thus their observed frequency distributions are hypothetically affected by an upper cutoff caused by the maximum active region size limit. The powerlaw slopes fitted near the upper cutoff can then not reliably be extrapolated to the microflare regime to evaluate their contribution to coronal heating. 相似文献
820.
波束扫描合成孔径雷达是为了满足星载合成孔径雷达宽测绘的要求而提出的,本文主要研究SCANSAR成象处理。SCANSAR的工作原理、信号格式、信号结构和信号参数限制的深入分析是成象处理研究的基础,成象处理算法包括块数据成象算法和块图象拼接算法两部分,频谱分析法和时域频域混合相关法被用于块数据成象,块图象的拼接是利用时间关系剪裁块图象再顺次拼接,完整的计算机仿真验证了本文提出的SCANSAR信号格式和 相似文献