全文获取类型
收费全文 | 376篇 |
免费 | 29篇 |
国内免费 | 32篇 |
专业分类
航空 | 123篇 |
航天技术 | 269篇 |
综合类 | 26篇 |
航天 | 19篇 |
出版年
2023年 | 12篇 |
2022年 | 9篇 |
2021年 | 19篇 |
2020年 | 20篇 |
2019年 | 16篇 |
2018年 | 19篇 |
2017年 | 3篇 |
2016年 | 8篇 |
2015年 | 14篇 |
2014年 | 20篇 |
2013年 | 27篇 |
2012年 | 17篇 |
2011年 | 31篇 |
2010年 | 25篇 |
2009年 | 32篇 |
2008年 | 28篇 |
2007年 | 19篇 |
2006年 | 14篇 |
2005年 | 13篇 |
2004年 | 12篇 |
2003年 | 8篇 |
2002年 | 8篇 |
2001年 | 9篇 |
2000年 | 3篇 |
1999年 | 6篇 |
1998年 | 6篇 |
1997年 | 4篇 |
1996年 | 7篇 |
1995年 | 9篇 |
1994年 | 3篇 |
1993年 | 1篇 |
1992年 | 4篇 |
1991年 | 2篇 |
1990年 | 7篇 |
1989年 | 1篇 |
1988年 | 1篇 |
排序方式: 共有437条查询结果,搜索用时 359 毫秒
431.
432.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2023,71(1):306-315
We investigate the geomagnetic and ionospheric effects of seismic activity during 1954 Sun spotless days (SSL) from 1995 to 2020. Two subsets of earthquakes (EQ) are evaluated for 676 events observed with the depth D1 ≤ 30 km and 1278 events with D2 > 30 km and the total set SSL. Newly developed 1 h geomagnetic index Hpo and the ionospheric WEQ index are used for the comparisons with the daily peak earthquake. The ionosphere WEQ index is derived at the EQ epicenter from JPL GIM-TEC map within the cell of 2.5°×5°, in latitude φ and longitude λ surrounding the epicenter at radius of about 200 km. We use the method of superposed epoch with the zero epoch time t0 taken at EQ to extract peak values of Hpo and WEQ during t0-24 h ≤ t < t0 (preEQ) and t0 < t ≤ t0 + 24 h (postEQ). It is found that the magnitude of Hpo(t0) is less that the both peaks of Hpo(preEQ) and Hpo(postEQ) in 91 % of events independent of EQ’s depth. Similar effect is observed with the peak of the positive/negative ionosphere indices and the absolute values of |W(preEQ)| and |W(postEQ)| the both exceeding |WEQ| in 77 % of events. The seismic activity tends to increase towards the solar minimum when SSLs occur. Our results provide evidence that EQ-related geomagnetic and ionospheric activities experience decline of intensity at the time of EQ under SSL. 相似文献
433.
针对光纤环的热致非互易误差的补偿方法进行研究,并通过仿真分析与实验验证,证明了某种光纤环尾纤长度与光纤环热致非互易误差之间的关系。根据等效介质理论和Mohr理论,建立了光纤环热致非互易相位误差仿真分析模型,并利用该模型计算了不同温度环境条件下,某类型光纤环顺逆时针方向光纤长度发生变化时,陀螺仪输出的全温零位漂移的变化量。仿真及实验结果表明,在1℃/min温变速率条件下,总长约800m的光纤环圈顺逆时针方向光纤长度相差约0.5m时,光纤环全温零位漂移量缩小了0.4(°)/h。研究结果得出了针对此类型的光纤环,当光纤环尾纤每减少0.5m,其热致非互易相位误差减小0.4(°)/h的规律。该项研究成果为后续优化光纤环的全温精度奠定了基础。 相似文献
434.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2023,71(5):2240-2251
This study examines the occurrences rate of geomagnetic storms during the solar cycles (SCs) 20–24. It also investigates the solar sources at SCs 23 and 24. The Disturbed storm time (Dst) and Sunspot Number (SSN) data were used in the study. The study establishes that the magnitude of the rate of occurrences of geomagnetic storms is higher (lower) at the descending phases (minimum phases) of solar cycle. It as well reveals that severe and extreme geomagnetic storms (Dst < -250 nT) seldom occur at low solar activity but at very high solar activity and are mostly associated with coronal mass ejections (CMEs) when occurred. Storms caused by CME + CH-HSSW are more prominent during the descending phase than any other phase of the solar cycle. Solar minimum features more CH-HSSW- associated storms than any other phase. It was also revealed that all high intensity geomagnetic storms (strong, severe and extreme) are mostly associated with CMEs. However, CH-HSSW can occasionally generate strong storms during solar minimum. The results have proven that CMEs are the leading cause of geomagnetic storms at the ascending, maximum and the descending phases of the cycles 23 and 24 followed by CME + CH-HSSW. The results from this study indicate that the rate of occurrence of geomagnetic storms could be predicted in SC phases. 相似文献
435.
436.
《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2023,71(1):46-66
Coronal mass ejection (CME) occurs when there is an abrupt release of a large amount of solar plasma, and this cloud of plasma released by the Sun has an intrinsic magnetic field. In addition, CMEs often follow solar flares (SF). The CME cloud travels outward from the Sun to the interplanetary medium and eventually hits the Earth’s system. One of the most significant aspects of space weather is the ionospheric response due to SF or CME. The direction of the interplanetary magnetic field, solar wind speed, and the number of particles are relevant parameters of the CME when it hits the Earth’s system. A geomagnetic storm is most geo-efficient when the plasma cloud has an interplanetary magnetic field southward and it is accompanied by an increase in the solar wind speed and particle number density. We investigated the ionospheric response (F-region) in the Brazilian and African sectors during a geomagnetic storm event on September 07–10, 2017, using magnetometer and GPS-TEC networks data. Positive ionospheric disturbances are observed in the VTEC during the disturbed period (September 07–08, 2017) over the Brazilian and African sectors. Also, two latitudinal chains of GPS-TEC stations from the equatorial region to low latitudes in the East and West Brazilian sectors and another chain in the East African sector are used to investigate the storm time behavior of the equatorial ionization anomaly (EIA). We noted that the EIA was disturbed in the American and African sectors during the main phase of the geomagnetic storm. Also, the Brazilian sector was more disturbed than the African sector. 相似文献
437.