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191.
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H. Arp 《Astrophysics and Space Science》2006,301(1-4):117-126
The association of low redshift, active galaxies with high redshift quasars is here tested in two regions uniformly surveyed
for quasars to faint limits. Three active galaxies in these regions all show significant association with nearby quasars.
Radio, optical and X-ray data available for these galaxies give new information on the processes which accompany the proposed
ejection of the quasars. It is concluded that the quasars are originally relatively compact compared to the galactic medium
through which they exit but can be slowed. It is argued that effects of ejection can be seen on the galaxies and may be connected
with spiral structure. Evidence for periodicity of the redshifts is discussed. 相似文献
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Judith A. Irwin J.M. Stil T.J. Bridges 《Monthly notices of the Royal Astronomical Society》2001,328(2):359-369
Deep SCUBA observations of NGC 1275 at 450 and 850 μm along with the application of deconvolution algorithms have permitted us to separate the strong core emission in this galaxy from the fainter extended emission around it. The core has a steep spectral index and is likely caused primarily by the active galactic nucleus. The faint emission has a positive spectral index and is clearly caused by extended dust in a patchy distribution out to a radius of ∼20 kpc from the nucleus. These observations have now revealed that a large quantity of dust, ∼ (two orders of magnitude larger than that inferred from previous optical absorption measurements), exists in this galaxy. We estimate the temperature of this dust to be ∼20 K (using an emissivity index of and the gas/dust ratio to be 360. These values are typical of spiral galaxies. The dust emission correlates spatially with the hot X-ray emitting gas, which may be a result of collisional heating of broadly distributed dust by electrons. As the destruction time-scale is short, the dust cannot be replenished by stellar mass loss and must be externally supplied, via either the infalling galaxy or the cooling flow itself. 相似文献
195.
塞佛特星系NGC1 0 6 8是一个非常令人注目的特殊天体 ,它是Seyfert[1]发现的第一批此类星系中离我们最近 (1 9Mpc,取H0 =6 0kms- 1Mpc- 1)和最亮的一个塞佛特星系 ,因此天文学家从射电到X 射线整个电磁波段对它进行了详尽的观测和研究。NGC1 0 6 8最初被归类为塞佛特II型天体 ,但是通过对其偏振光的光谱观测 ,发现了认为被遮挡住的塞佛特I型核发出的± 432 0km/s的宽Hβ发射线 ,因此被认为是活动星系核统一模型的一个范例 (见文 [2 ] )。射电与光学的观测资料都表明NGC1 0 6 8的中心部分有激烈的喷射活动… 相似文献
196.
P. Lira M. J. Ward A. Zezas S. S. Murray 《Monthly notices of the Royal Astronomical Society》2002,333(3):709-714
We present high spatial resolution X-ray Chandra HRC and HST WFPC2 H α observations of the prototypical infrared-luminous galaxy NGC 6240. The central region of this system shows a remarkably complex morphology, with filaments and loops observed in the optical and X-rays. The total X-ray luminosity is dominated by the extended emission. Both nuclei are clearly detected in the HRC image and both appear to be extended. The energetics of the nuclei imply that the southern nucleus is the more plausible counterpart to the obscured active galactic nucleus. The overall spectral energy distribution of the galaxy is in good agreement with a blend of starburst and AGN components that have similar bolometric luminosities, L bol ∼5×1045 erg s-1 , with the starburst dominating the observed continuum in the near-infrared ( K band), optical and soft X-ray bands. 相似文献
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