全文获取类型
收费全文 | 547篇 |
免费 | 14篇 |
国内免费 | 13篇 |
专业分类
测绘学 | 52篇 |
大气科学 | 10篇 |
地球物理 | 21篇 |
地质学 | 57篇 |
海洋学 | 9篇 |
天文学 | 382篇 |
综合类 | 31篇 |
自然地理 | 12篇 |
出版年
2024年 | 1篇 |
2023年 | 1篇 |
2022年 | 7篇 |
2021年 | 5篇 |
2020年 | 1篇 |
2019年 | 6篇 |
2018年 | 5篇 |
2017年 | 5篇 |
2016年 | 5篇 |
2015年 | 7篇 |
2014年 | 11篇 |
2013年 | 11篇 |
2012年 | 10篇 |
2011年 | 15篇 |
2010年 | 13篇 |
2009年 | 57篇 |
2008年 | 26篇 |
2007年 | 66篇 |
2006年 | 55篇 |
2005年 | 58篇 |
2004年 | 44篇 |
2003年 | 33篇 |
2002年 | 29篇 |
2001年 | 16篇 |
2000年 | 22篇 |
1999年 | 13篇 |
1998年 | 27篇 |
1997年 | 1篇 |
1996年 | 1篇 |
1995年 | 3篇 |
1993年 | 2篇 |
1991年 | 1篇 |
1990年 | 1篇 |
1987年 | 2篇 |
1980年 | 1篇 |
1977年 | 1篇 |
1919年 | 1篇 |
1900年 | 1篇 |
1897年 | 5篇 |
1882年 | 1篇 |
1880年 | 1篇 |
1877年 | 3篇 |
排序方式: 共有574条查询结果,搜索用时 15 毫秒
91.
92.
93.
Nino Chkheidze 《New Astronomy》2012,17(2):227-231
A plasma emission model is presented interpreting the observational properties of RX J1856.5-3754. In particular, on the basis of the Vlasov’s kinetic equation we study the process of the quasi-linear diffusion (QLD) developed by means of the cyclotron instability. This mechanism provides simultaneous generation of optical and X-ray emission on the light cylinder scales, in one location of the pulsar magnetosphere. It is assumed that the observed X-ray spectrum of this source is generated via the synchrotron mechanism. A different approach of the synchrotron theory is considered, giving a spectral energy distribution that is in a good agreement with the observational data. 相似文献
94.
95.
96.
97.
98.
Gavin Ramsay S. B. Potter David A. H. Buckley Peter J. Wheatley 《Monthly notices of the Royal Astronomical Society》1999,306(4):809-814
CP Tuc (AX J2315–592) shows a dip in X-rays which lasts for approximately half the binary orbit and is deeper in soft X-rays compared with hard X-rays. It has been proposed that this dip is due to the accretion stream obscuring the accretion region from view. If CP Tuc were a polar, as has been suggested, then the length of such a dip would make it unique amongst polars since in those polars in which a dip is seen in hard X-rays the dip lasts for only 0.1 of the orbit. We present optical polarimetry and RXTE observations of CP Tuc which show circular polarization levels of ∼10 per cent and find evidence for only one photometric period. These data confirm CP Tuc as a polar. Our modelling of the polarization data implies that the X-ray dip is due to the bulk of the primary accretion region being self-eclipsed by the white dwarf. The energy dependence of the dip is due to a combination of this self-eclipse and also the presence of an X-ray temperature gradient over the primary accretion region. 相似文献
99.
Roberto Soria Kinwah Wu Duncan K. Galloway 《Monthly notices of the Royal Astronomical Society》1999,309(2):528-532
We carried out I , R , V and B photometric observations of the neutron star X-ray binary RXTE J2123−058 shortly after the end of the X-ray outburst in mid-1998. We adopt the low-mass binary model to interpret our observations. After folding our data on the 0.24 821‐d orbital period, and correcting for the steady brightness decline following the outburst, we observed sinusoidal oscillations with hints of ellipsoidal modulations which became progressively more evident. Our data also show that the decline in brightness was faster in the V band than in the R and I bands. This suggests both the cooling of an irradiation-heated secondary star and the fading of an accretion disc over the nights of our observations. 相似文献
100.
B. W. Stappers B. M. Gaensler † S. Johnston 《Monthly notices of the Royal Astronomical Society》1999,308(3):609-617
Using the Australia Telescope Compact Array (ATCA) we have imaged the fields around five promising pulsar candidates to search for radio pulsar wind nebulae (PWNe). We have used the ATCA in its pulsar-gating mode; this enables an image to be formed containing only off-pulse visibilities, thereby dramatically improving the sensitivity to any underlying PWN. Data from the Molonglo Observatory Synthesis Telescope were also used to provide sensitivity on larger spatial scales. This survey found a faint new PWN around PSR B0906−49; here we report on non-detections of PWNe towards PSRs B1046−58, B1055−52, B1610−50 and J1105−6107. Our radio observations of the field around PSR B1055−52 argue against previous claims of an extended X-ray and radio PWN associated with the pulsar. If these pulsars power unseen, compact radio PWNe, upper limits on the radio flux indicate that a fraction of less than 10−6 of their spin-down energy is used to power this emission. Alternatively, PSRs B1046−58 and B1610−50 may have relativistic winds similar to other young pulsars and the unseen PWN may be resolved and fainter than our surface brightness sensitivity threshold. We can then determine upper limits on the local interstellar medium (ISM) density of 2.2×10−3 and 1×10−2 cm−3 , respectively. Furthermore, we derive the spatial velocities of these pulsars to be ∼450 km s−1 and thus rule out the association of PSR B1610−50 with supernova remnant (SNR) G332.4+00.1 (Kes 32). Strong limits on the ratio of unpulsed to pulsed emission are also determined for three pulsars. 相似文献