全文获取类型
收费全文 | 270篇 |
免费 | 31篇 |
专业分类
测绘学 | 2篇 |
地球物理 | 10篇 |
海洋学 | 1篇 |
天文学 | 287篇 |
综合类 | 1篇 |
出版年
2024年 | 5篇 |
2023年 | 5篇 |
2022年 | 7篇 |
2021年 | 5篇 |
2020年 | 5篇 |
2019年 | 5篇 |
2018年 | 3篇 |
2017年 | 2篇 |
2016年 | 4篇 |
2015年 | 8篇 |
2014年 | 8篇 |
2013年 | 7篇 |
2012年 | 20篇 |
2011年 | 10篇 |
2010年 | 17篇 |
2009年 | 19篇 |
2008年 | 22篇 |
2007年 | 20篇 |
2006年 | 29篇 |
2005年 | 22篇 |
2004年 | 13篇 |
2003年 | 17篇 |
2002年 | 7篇 |
2001年 | 8篇 |
2000年 | 6篇 |
1999年 | 7篇 |
1998年 | 7篇 |
1997年 | 1篇 |
1995年 | 2篇 |
1994年 | 4篇 |
1993年 | 2篇 |
1992年 | 1篇 |
1991年 | 1篇 |
1987年 | 1篇 |
1984年 | 1篇 |
排序方式: 共有301条查询结果,搜索用时 203 毫秒
201.
202.
203.
204.
205.
Site testing results indicate that Antarctic Dome A is an excellent ground-based astronomical site suitable for observations ranging from visible to infrared wavelengths. However, the harsh environment in Antarctica, especially the very low temperature and atmospheric pressure, always produces frost on the telescopes' mirrors, which are exposed to the air. Since the Dome A site is still unattended, the Antarctic telescope tubes are always designed to be filled with dry nitrogen, and the outer surfaces of the optical system are heated by an indium-tin oxide thin film. These precautions can prevent the optical surfaces from frosting over, but they degrade the image quality by introducing additional mirror seeing. Based on testing observations of the second Antarctic Survey Telescope (AST3-2) in the Mohe site in China, mirror seeing resulting from the heated aspheric plate has been measured using micro-thermal sensors. Results comparing the real-time atmospheric seeing monitored by the Differential Image Motion Monitor and real-time examinations of image quality agree well. 相似文献
206.
W. Schmidt O. von der Lühe R. Volkmer C. Denker S.K. Solanki H. Balthasar N. Bello Gonzlez Th. Berkefeld M. Collados A. Fischer C. Halbgewachs F. Heidecke A. Hofmann F. Kneer A. Lagg H. Nicklas E. Popow K.G. Puschmann D. Schmidt M. Sigwarth M. Sobotka D. Soltau J. Staude K.G. Strassmeier T.A. Waldmann 《Astronomische Nachrichten》2012,333(9):796-809
The 1.5 m telescope GREGOR opens a new window to the understanding of solar small‐scale magnetism. The first light instrumentation includes the Gregor Fabry Pérot Interferometer (GFPI), a filter spectro‐polarimeter for the visible wavelength range, the GRating Infrared Spectro‐polarimeter (GRIS) and the Broad‐Band Imager (BBI). The excellent performance of the first two instruments has already been demonstrated at the Vacuum Tower Telescope. GREGOR is Europe’s largest solar telescope and number 3 in the world. Its all‐reflective Gregory design provides a large wavelength coverage from the near UV up to at least 5 microns. The field of view has a diameter of 150″. GREGOR is equipped with a high‐order adaptive optics system, with a subaperture size of 10 cm, and a deformable mirror with 256 actuators. The science goals are focused on, but not limited to, solar magnetism. GREGOR allows us to measure the emergence and disappearance of magnetic flux at the solar surface at spatial scales well below 100 km. Thanks to its spectro‐polarimetric capabilities, GREGOR will measure the interaction between the plasma flows, different kinds of waves, and the magnetic field. This will foster our understanding of the processes that heat the chromosphere and the outer layers of the solar atmosphere. Observations of the surface magnetic field at very small spatial scales will shed light on the variability of the solar brightness (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
207.
We report on the results of a dedicated campaign to derive a pointing model for the GREGOR solar telescope which took place in December 2011. Two main goals were in the focus of this campaign: first to prove the aptness of the GREGOR solar telescope for night‐time, unattended operations and second to derive some qualitative measure of the amount of misalignment in the optical and mechanical parts of the telescope. In the final version, a root‐mean‐square deviation (RMSD) of 1.6″ for the azimuth model and an RMSD of 2.3″ in the elevation model could be achieved (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
208.
O. von der Lühe R. Volkmer T.J. Kentischer R. Geißler 《Astronomische Nachrichten》2012,333(9):894-900
The design and characteristics of the Broad‐Band Imager (BBI) of GREGOR are described. BBI covers the visible spectral range with two cameras simultaneously for a large field and with critical sampling at 390 nm, and it includes a mode for observing the pupil in a Foucault configuration. Samples of first‐light observations are shown (© 2012 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
209.
The hard X-ray imaging telescope of the modulation collimator type is widely used in current solar observations. The spatial modulation telescope is the telescope which keeps its central axis not rotate, suitable for the satellite of 3-axis attitude stabilization. For the possible Chinese solar mission in the near future, we make a design of hard X-ray imaging telescope, and simulate the photon counting using the common simulation software GEANT4. Then we implement the image reconstruction with MATLAB, and compare the reconstructed image of the photons simulated by GEANT4 with that of the photons calculated by the geometric algorithm. The results show that the simulated one by GEANT4 is more closer to the reality than that obtained by the geometric algorithm. An executable design is also proposed at last. 相似文献
210.
《Astroparticle Physics》2012,35(7):435-448
MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located in the Canary island of La Palma. Since autumn 2009 both telescopes have been working together in stereoscopic mode, providing a significant improvement with respect to the previous single-telescope observations. We use observations of the Crab Nebula taken at low zenith angles to assess the performance of the MAGIC stereo system. The trigger threshold of the MAGIC telescopes is 50 − 60 GeV. Advanced stereo analysis techniques allow MAGIC to achieve a sensitivity as good as (0.76 ± 0.03)% of the Crab Nebula flux in 50 h of observations above 290 GeV. The angular resolution at those energies is better than ∼0.07°. We also perform a detailed study of possible systematic effects which may influence the analysis of the data taken with the MAGIC telescopes. 相似文献