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961.
Our current understanding of the acceleration of solar-energetic particles is reviewed. The emphasis in this paper is on analytic
theory and numerical modeling of the physics of diffusive shock acceleration. This mechanism naturally produces an energy
spectrum that is a power law over a given energy interval that is below a characteristic energy where the spectrum has a break,
or a rollover. This power law is a common feature in the observations of all types of solar-energetic particles, and not necessarily just those associated with shock waves (e.g. events associated with
impulsive solar flares which are often described in terms of resonant stochastic acceleration). Moreover, the spectral index
is observed to have remarkably little variability from one event to the next (about 50%). Any successful acceleration mechanism
must be able to produce this feature naturally and have a resulting power-law index that does not depend on physical parameters
that are expected to vary considerably. Currently, only diffusive shock acceleration does this. 相似文献
962.
J. Büchner 《Space Science Reviews》2006,124(1-4):345-360
Reconnection is a major commonality of solar and magnetospheric physics. It was conjectured by Giovanelli in 1946 to explain
particle acceleration in solar flares near magnetic neutral points. Since than it has been broadly applied in space physics
including magnetospheric physics. In a special way this is due to Harry Petschek, who in 1994 published his ground breaking
solution for a 2D magnetized plasma flow in regions containing singularities of vanishing magnetic field. Petschek’s reconnection
theory was questioned in endless disputes and arguments, but his work stimulated the further investigation of this phenomenon
like no other. However, there are questions left open. We consider two of them – “anomalous” resistivity in collisionless
space plasma and the nature of reconnection in three dimensions. The CLUSTER and SOHO missions address these two aspects of
reconnection in a complementary way -- the resistivity problem in situ in the magnetosphere and the 3D aspect by remote sensing of the Sun. We demonstrate that the search for answers to both questions
leads beyond the applicability of analytical theories and that appropriate numerical approaches are necessary to investigate
the essentially nonlinear and nonlocal processes involved. Necessary are both micro-physical, kinetic Vlasov-equation based
methods of investigation as well as large scale (MHD) simulations to obtain the geometry and topology of the acting fields
and flows. 相似文献
963.
Helioseismology uses solar p-mode oscillations to probe the structure of the solar interior. The modifications of p-mode properties
due to the presence of solar magnetic fields provide information on the magnetic fields in the solar interior. Here we review
some of results in helioseismology on the magnetic fields in the solar convection zone. We will also discuss a recent result
on the magnetic fields at the base of the convection zone.
This revised version was published online in August 2006 with corrections to the Cover Date. 相似文献
964.
神舟飞船生长GaMnSb材料过程及性能分析 总被引:1,自引:0,他引:1
利用神舟3号飞船(SZ-3)上的多样品空间晶体炉制备出GaMnSb材料.所设计的石英安瓿使用氧化铝棉毡和特殊设计制造的氮化硼坩锅进行减震,经受住了严峻的力学环境的考验,完成了材料的空间生长实验,达到了空间生长材料的初步要求.对空间生长的GaMnSb晶体进行了X射线能谱分析和X射线衍射分析,发现空间生长的GaMnSb是多晶结构.对未获得GaMnSb单晶的原因进行了分析,发现空间晶体炉温度的波动和提供能量的不足是导致生成GaMnSb多晶结构的主要原因.由于在晶体生长的初始阶段晶体炉提供的能量不足,使GaSb单晶部分未能熔化,从而导致GaMnSb材料的生长在没有籽晶的情况下进行. 相似文献
965.
潜在电路计算机辅助网络树生成系统研究与工程应用 总被引:3,自引:0,他引:3
网络树是规范潜在电路分析(SCA)技术的两大工具之一,而计算机辅助网络树生成系统是对航天等复杂控制系统进行SCA所必备的辅助手段。本文介绍了一个能真正用于实际工程SCA的网络树生成系统。 相似文献
966.
I.S. Veselovsky V. Bothmer P. Cargill A.V. Dmitriev K.G. Ivanov E. Romashets A.N. Zhukov O.S. Yakovchouk 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2005,36(12):2460-2464
Times of sustained strong northward IMF can interrupt the magnetic storm development and lead to lower levels of geomagnetic activity for many hours. During 1997–2000 we have found two events of this kind observed on November 8, 1998 and October 13, 2000. In both cases, the storms started as usual after arrival of ejecta with a southward IMF component from the Sun to the Earth, but ceased after several hours due to the onset of sustained northward IMF leading to the faster recovery process. After the passage of this so-called positive domain, the storm development started again. The heliospheric magnetic field intensity remained enhanced and nearly constant. The solar origins of the geomagnetic storm interruptions have been investigated. Tentatively they may be related to strong nonlinear Alfvйn type solitary waves excited by non-stationary coronal current variations with a characteristic time-scale of about a day. 相似文献
967.
968.
S.S. Hasan 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008
This review focuses on dynamics of the solar chromosphere, which serves as a good proxy for understanding processes in stellar chromospheres as well. In the quiet chromosphere it is useful to distinguish between the magnetic network on the boundaries of supergranulation cells, where strong magnetic fields are organized in mainly vertical magnetic flux tubes, and internetwork regions in the cell interior, where magnetic fields are weaker and dynamically less important. Recently, some progress has been made in understanding the physics of the non-magnetic chromosphere. On the other hand, the physical processes that heat the magnetic network have not been fully identified. Is the network heated by wave dissipation and if so, what are their physical characteristics? These and other aspects relating to the dynamics and energy transport mechanisms will be discussed in detail. In addition, some of the outstanding problems in the field such the driving mechanism for spicules and the nature of internetwork magnetic fields will also be highlighted. Furthermore, a critical assessment will be made on the challenges facing theory and the direction for future investigations, particularly in the light of the new space experiments, will be highlighted. 相似文献
969.
970.
A type of 2D magnetic equivalent circuit framework of permanent magnet for magnetic system in AEMR 总被引:1,自引:1,他引:0
Modeling of permanent magnet(PM) is very important in the process of electromagnetic system calculation of aerospace electromagnetic relay(AEMR). In traditional analytical calculation, PM is often equivalent to a lumped parameter model of one magnetic resistance and one magnetic potential, but great error is often caused for the inner differences of PM; based on the conception of flux tube, a type of 2D magnetic equivalent circuit framework of permanent magnet model(2D MECF) is established; the element is defined, the relationship between elements is deduced, and solution procedure as well as verification condition of this model is given; by a case study of the electromagnetic system of a certain type of AEMR, the electromagnetic system calculation model is established based on 2D MECF and the attractive force at different rotation angles is calculated; the proposed method is compared with the traditional lumped parameter model and finite element method(FEM); for some types of electromagnetic systems with symmetrical structure, 2D MECF proves to be of acceptable accuracy and high calculation speed which fit the requirement of robust design for AEMR. 相似文献