全文获取类型
收费全文 | 1111篇 |
免费 | 207篇 |
国内免费 | 128篇 |
专业分类
航空 | 744篇 |
航天技术 | 335篇 |
综合类 | 128篇 |
航天 | 239篇 |
出版年
2024年 | 3篇 |
2023年 | 23篇 |
2022年 | 19篇 |
2021年 | 41篇 |
2020年 | 43篇 |
2019年 | 39篇 |
2018年 | 34篇 |
2017年 | 36篇 |
2016年 | 46篇 |
2015年 | 40篇 |
2014年 | 88篇 |
2013年 | 68篇 |
2012年 | 72篇 |
2011年 | 82篇 |
2010年 | 78篇 |
2009年 | 103篇 |
2008年 | 105篇 |
2007年 | 89篇 |
2006年 | 99篇 |
2005年 | 69篇 |
2004年 | 36篇 |
2003年 | 40篇 |
2002年 | 22篇 |
2001年 | 23篇 |
2000年 | 26篇 |
1999年 | 19篇 |
1998年 | 12篇 |
1997年 | 22篇 |
1996年 | 6篇 |
1995年 | 15篇 |
1994年 | 10篇 |
1993年 | 12篇 |
1992年 | 4篇 |
1991年 | 7篇 |
1990年 | 6篇 |
1989年 | 6篇 |
1988年 | 1篇 |
1984年 | 1篇 |
1981年 | 1篇 |
排序方式: 共有1446条查询结果,搜索用时 15 毫秒
81.
Kh. Karami S. Ghader A. Raeen 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
In the present work values of peak electron density (NmF2) and height of F2 ionospheric layer (hmF2) over Tehran region at a low solar activity period are compared with the predictions of the International Reference Ionosphere models (IRI-2001 and IRI-2007). Data measured by a digital ionosonde at the ionospheric station of the Institute of Geophysics, University of Tehran from July 2006 to June 2007 are used to perform the calculations. Formulations proposed by and are utilized to calculate the hmF2. The International Union of Radio Science (URSI) and International Radio Consultative Committee (CCIR) options are employed to run the IRI-2001 and IRI-2007 models. Results show that both IRI-2007 and IRI-2001 can successfully predict the NmF2 and hmF2 over Tehran region. In addition, the study shows that predictions of IRI-2007 model with CCIR coefficient has closer values to the observations. Furthermore, it is found that the monthly average of the percentage deviation between the IRI models predictions and the values of hmF2 and NmF2 parameters are less than 10% and 21%, respectively. 相似文献
82.
Anand K. Singh A.K. Sinha Rahul Rawat Bulusu Jayashree B.M. Pathan Ajay Dhar 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
Magnetic data from a newly commissioned Indian Antarctic station Bharati (corrected geomagnetic (CGM) coordinates 74.7°S, 97.2°E) and closely-spaced IMAGE chain observatories (∼100° magnetic meridian in Northern hemisphere) has been analyzed to study the climatology of substorms which were localized poleward of the standard auroral oval. We considered four austral summers (year 2007–2010) when data from Bharati was available. Several very high latitude substorms were observed in this duration when the solar activity remained unexpectedly low for a long time. Various features of very high latitude substorms, e.g., local time dependence, interplanetary state, hemispherical asymmetry and their nightside low latitude signatures are examined. Events studied here, suggested the following properties of substorms occurring at very high latitudes: (1) maximum occurrence was observed near magnetic midnight (21:00–02:00 MLT). (2) In contradiction to earlier reports, many substorms were observed even during negative IMF Bz condition. In addition, majority of substorms occurred during low or moderate solar wind streams. (3) Magnetic signatures were often pronounced in the winter hemisphere. (4) Even if widely used standard AE indices fail to monitor very high latitude substorms, their low latitude signatures are often evident. 相似文献
83.
O.S. Oyekola 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2010
We use hourly monthly median values of propagation factor M(3000)F2 data observed at Ouagadougou Ionospheric Observatory (geographic12.4°N, 1.5°W; 5.9o dip), Burkina Faso (West Africa) during the years Januar1987–December1988 (average F10.7 < 130 × 10−22 W/m2/Hz, representative of low solar flux conditions) and for January 1989–December1990 (average F10.7 ? 130 × 10−22 W/m2/Hz, representative of high solar epoch) for magnetically quiet conditions to describe local time, seasonal and solar cycle variations of equatorial ionospheric propagation factor M(3000)F2 in the African region. We show that that seasonal trend between solar maximum and solar minimum curves display simple patterns for all seasons and exhibits reasonable disparity with root mean square error (RMSE) of about 0.31, 0.29 and 0.26 for December solstice, June solstice and equinox, respectively. Variability Σ defined by the percentage ratio of the absolute standard deviation to the mean indicates significant dissimilarity for the two solar flux levels. Solar maximum day (10–14 LT) and night (22–02 LT) values show considerable variations than the solar minimum day and night values. We compare our observations with those of the IRI 2007 to validate the prediction capacity of the empirical model. We find that the IRI model tends to underestimate and overestimate the observed values of M(3000)F2, in particular, during June solstice season. There are large discrepancies, mainly during high solar flux equinox and December solstice between dawn and local midnight. On the other hand, IRI provides a slightly better predictions for M(3000)F2 between 0900 and 1500 LT during equinox low and high solar activity and equinox high sunspot number. Our data are of great importance in the area of short-wave telecommunication and ionospheric modeling. 相似文献
84.
85.
储氢合金的性质及发展趋势 总被引:5,自引:0,他引:5
本文介绍了储氢合金的性质,Ni-MH电池原理,以及储氢合金对Ni-MH电池所产生的影响,根据目前科学技术的发展以及市场的需求,提出了未来储氢合金及Ni-MH电池的发展趋势。 相似文献
86.
A monostatic 24-h debris observation campaign (BPE-1/2000) has been prepared and conducted using FGAN's TIRA L-Band system. Based on experiences from previous Beam-park experiments a similar largely automated data processing is applied on an extended range window of 300–2000km. More than 1500 detections are encountered, 471 of them are verified as being real objects in Low-Earth-Orbit (LEO). PROOF's observation forecasting of catalogued objects is evaluated against the observed objects, and the difficulties obtaining radar cross-sections (RCSs) and object sizes from Beam-park experiments are discussed. Sidelobe detections are identified by using background information like two-line element (TLE) sets and/or catalogued RCSs.In comparison with previous experiments, the statistics show similarities confirming the concept of Beam-park experiments for space debris observations, despite the snapshot character of 24-h experiments. The comparison with MASTER/PROOF'99 and ORDEM2000 leads to a reasonable agreement between models and observations. 相似文献
87.
首次采用共熔法制备超高温陶瓷基复合材料,三个样品初始组分分别为ZrB_2与鳞片石墨,ZrB_2、TaB_2、SiC及鳞片石墨,ZrB_2、MoSi_2与鳞片石墨。研究结果表明,共熔法制备的复合材料中各相分散均匀,产物中的石墨高度有序,石墨层间距分别为0.335 4、0.335 9与0.337 7 nm,且三者的微晶厚度分别为63.4、51.5及68.7 nm,拉曼光谱结果表明硼已经掺杂进入了石墨的网格结构。所制得的超高温陶瓷基复合材料样品中均存在一定的孔隙率,且制备的超高温陶瓷基复合材料的热导率较低。该方法为一种新型、快速、一步法制备超高温陶瓷基复合材料工艺。 相似文献
88.
K.A. Berényi V. Barta Á. Kis 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(5):1230-1243
In our study we analyze and compare the response and behavior of the ionospheric F2 and of the sporadic E-layer during three strong (i.e., Dst?<??100nT) individual geomagnetic storms from years 2012, 2013 and 2015, winter time period. The data was provided by the state-of the art digital ionosonde of the Széchenyi István Geophysical Observatory located at midlatitude, Nagycenk, Hungary (IAGA code: NCK, geomagnetic latitude: 46.17° geomagnetic longitude: 98.85°). The local time of the sudden commencement (SC) was used to characterize the type of the ionospheric storm (after Mendillo and Narvaez, 2010). This way two regular positive phase (RPP) ionospheric storms and one no-positive phase (NPP) storm have been analyzed. In all three cases a significant increase in electron density of the foF2 layer can be observed at dawn/early morning (around 6:00 UT, 07:00 LT). Also we can observe the fade-out of the ionospheric layers at night during the geomagnetically disturbed time periods. Our results suggest that the fade-out effect is not connected to the occurrence of the sporadic E-layers. 相似文献
在众多光阳极材料中,纳米结构材料α-Fe2O3由于其光吸收显著、化学稳定性好、储量丰富等优势,被认为是最有前途的材料之一。利用水热法制备了具有良好光解水性能的Co和P掺杂α-Fe2O3纳米材料。经过掺杂后α-Fe2O3纳米材料仍为纳米棒状形貌,纳米棒的粒径增加。实验发现,Co掺杂α-Fe2O3制成的电极在标准光照射下的最大光生电流密度为0.453 mA/cm2,是未掺杂样品的20.6倍,P掺杂α-Fe2O3制成的电极在标准光照射下的最大光生电流密度为0.276 mA/cm2,是未掺杂样品的12.5倍,具备了高效光解水性能。同时通过SEM、TEM、XRD、UV-Vis和Mott-Schottky测试等方法,结合形貌与结构表征,研究了α-Fe2O3的光电化学分解水性能影响机理。 相似文献
90.