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81.
Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections
(CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast
and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called
the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the
magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead
to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection
processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this
study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology.
This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic
field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic
topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’. 相似文献
82.
B.S. Shylaja 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2006,38(12):2850-2853
The chemically peculiar (CP) stars are classified into subgroups based on the type of peculiarities. A significant fraction of these are known to be binaries. The faster evolution of the massive component leads to a white dwarf or a neutron star. Further evolution of the binary is analysed taking into consideration, the orbital parameters, effect of magnetic field, spectroscopic peculiarities and finally the statistics of CP binaries and Low Mass X-ray Binaries (LMXB).
The possible consequences of the evolution to lead to the formation of Magnetic Cataclysmic Variables (MCV) and LMXB are discussed. 相似文献
83.
Coronal mass ejections and post-shock streams driven by them are the most efficient drivers of strong magnetospheric activity,
magnetic storms. For this reason there is considerable interest in trying to make reliable forecasts for the effects of CMEs
as much in advance as possible. To succeed this requires understanding of all aspects related to CMEs, starting from their
emergence on the Sun to their propagation to the vicinity of the Earth and to effects within the magnetosphere. In this article
we discuss some recent results on the geoeffectivity of different types of CME/shock structures. A particularly intriguing
observation is that smoothly rotating magnetic fields within CMEs are most efficient in driving storm activity seen in the
inner magnetosphere due to enhanced ring current, whereas the sheath regions between the shock and the ejecta tend to favour
high-latitude activity. 相似文献
84.
H. Raichur B. Paul S. Naik N. Bhatt 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2006,38(12):2785-2787
High mass X-ray binary (HMXB) pulsars are of two types, persistent and transient. 4U1538−52 is a persistent HMXB whose orbit was previously measured to be circular but the RXTE observations revealed an eccentric orbit. We observed this system with RXTE-PCA in August 2003 and our timing analysis supports the eccentric orbit of the system. However, we do not find any evidence for orbital evolution.
Rotational and tidal interactions between the stars of a closed binary system result in apsidal motion which can be measured in systems with eccentric orbit. 4U0115+63 is a Be-transient HMXB whose eccentric orbit was well-determined during its 1978 outburst. We report preliminary results from analysis of data obtained during the 1999 outburst of this source with the RXTE-PCA. 相似文献
85.
Nat Gopalswamy 《Space Science Reviews》2006,124(1-4):145-168
Interplanetary coronal mass ejections (ICMEs) originating from closed field regions on the Sun are the most energetic phenomenon
in the heliosphere. They cause intense geomagnetic storms and drive fast mode shocks that accelerate charged particles. ICMEs
are the interplanetary manifestations of CMEs typically remote-sensed by coronagraphs. This paper summarizes the observational
properties of ICMEs with reference to the ordinary solar wind and the progenitor CMEs. 相似文献
86.
周同礼 《南京航空航天大学学报》1988,(1)
陀螺力矩是在高速旋转的发动机转子和无人机的转动运动相互作用下产生的。在它的作用下,无人机在不同方向上的转动运动交连起来,共同影响无人机的飞行姿态。转动惯量是决定无人机的转动运动的另一个因素。本文着重研究了陀螺力矩在无人机几个特殊的飞行段落内对无人机转动运动的影响和燃料量以及无人机姿态角变化造成的燃料分布变化对无人机转动惯量以及转动运动的影响。 相似文献
87.
88.
为了掌握自动飞行器的工作特性,在它飞上空中之前,工程技术人员要在地面进行各种仿真试验。研制力矩控制系统的目的在于模拟随高度、速度变化且连续作用在飞行器翼面上的气动铰链力矩。这种装置广泛应用于各种型号舵机。 我们研制的力矩控制系统力案如图1所示。 相似文献
89.
金重 《中国民航学院学报》1992,10(2):37-45
本文采用一元线性回归法进行刚体转动惯量实验的数据处理,对通常在测量中运用的简化条件作了分析,从而提高了实验课的教学水平,并使该实验具有实用价值。 相似文献
90.
杨继松 《中国空间科学技术》1997,17(4):1-8
通过对几个具体实例的计算,证实了在电磁场边值问题的矩量法求解过程中,选用不同的基函数其解的数值稳定性会有很大的差别。从而有可能选择一种数值稳定性比较好的基函数来进行矩量法求解。另一方面,提出了选用多尺度子域基函数,并通过多次迭代来提高矩量法解的精度的算法。实例计算表明,该算法不仅可以有效地降低系数矩阵的条件数,而且还降低了对计算机内存容量的要求,是一种有效的、稳定的算法 相似文献