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11.
参数振动问题是直升机的基本动力学问题之一,旋翼桨叶的挥舞弯曲微分方程和摆振弯曲微分方程都是复杂的参数振动问题,在许多计论直升机旋翼动力学的论著中~[1-4],有的虽然推导了复尽杂的参数振动方程,却没有提到求解的方法,有的对此根本没有论及.本文旨在讨论参数问题的数值解法. 相似文献
12.
分析了高过载对固体火箭发动机流场和绝热层烧蚀的影响规律,提出一种新的研究思路:采用数值模拟方法来预示发动机三维两相流场,建立高过载流场模拟实验装置,开展绝热层烧蚀实验,建立高过载条件下的绝热层烧蚀模型,在此基础上发展高过载发动机绝热层设计和烧蚀预示方法。其中关键技术是高过载流场的模拟,对粒子加入法和弯管分离法两种方案进行了论证,认为弯管分离法原理上是可行的。为了验证这种方案的可行性,开展了弯管通道两相流的数值模拟研究,计算结果表明弯管装置具有使凝相粒子聚集形成高浓度粒子流的功能。 相似文献
13.
14.
Flight Flutter Modal Parameters Identification with Atmospheric Turbulence Excitation Based on Wavelet Transformation 总被引:2,自引:0,他引:2
Zhang Bo Shi Zhongke Li Jianjun 《中国航空学报》2007,20(5):394-401
针对基于大气紊流激励的飞机颤振试验数据具有信噪比低以及测量数据以加速度响应形式给出等特点,将小波变换与随机减量法相结合对飞机颤振模态参数进行识别,首先利用随机减量法获得结构在非零初始加速度条件下的自由衰减响应,然后对该自由衰减响应进行Morlet连续小波变换,为使变换简单,本文采用了Parseval定理和留数定理,利用Morlet的带通滤波特性,通过搜索小波变换系数在不同的尺度区域内的极大值,再根据小波变换系数的极大值、相角与固有振动频率及阻尼系数间的关系,即可识别出各模态参数。并对利用小波变换识别颤振模态参数时,实现模态解耦应满足的条件进行了分析研究。通过仿真和飞机颤振试验数据分析,验证了该识别方法不仅简单、有效和可行,而且具有较强的抗噪性。 相似文献
15.
张明影 《西安航空技术高等专科学校学报》2002,20(1):49-50
在理论力学教学中,平面运动刚体的转动与基点无关的证明过于简单,本利用矢量代数的知识,证明平面运动刚体的角度与角加速度与基点的选择无关。 相似文献
16.
17.
MESSENGER: Exploring Mercury’s Magnetosphere 总被引:1,自引:0,他引:1
James A. Slavin Stamatios M. Krimigis Mario H. Acuña Brian J. Anderson Daniel N. Baker Patrick L. Koehn Haje Korth Stefano Livi Barry H. Mauk Sean C. Solomon Thomas H. Zurbuchen 《Space Science Reviews》2007,131(1-4):133-160
The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission to Mercury offers our first opportunity
to explore this planet’s miniature magnetosphere since the brief flybys of Mariner 10. Mercury’s magnetosphere is unique in
many respects. The magnetosphere of Mercury is among the smallest in the solar system; its magnetic field typically stands
off the solar wind only ∼1000 to 2000 km above the surface. For this reason there are no closed drift paths for energetic
particles and, hence, no radiation belts. Magnetic reconnection at the dayside magnetopause may erode the subsolar magnetosphere,
allowing solar wind ions to impact directly the regolith. Inductive currents in Mercury’s interior may act to modify the solar
wind interaction by resisting changes due to solar wind pressure variations. Indeed, observations of these induction effects
may be an important source of information on the state of Mercury’s interior. In addition, Mercury’s magnetosphere is the
only one with its defining magnetic flux tubes rooted beneath the solid surface as opposed to an atmosphere with a conductive
ionospheric layer. This lack of an ionosphere is probably the underlying reason for the brevity of the very intense, but short-lived,
∼1–2 min, substorm-like energetic particle events observed by Mariner 10 during its first traversal of Mercury’s magnetic
tail. Because of Mercury’s proximity to the sun, 0.3–0.5 AU, this magnetosphere experiences the most extreme driving forces
in the solar system. All of these factors are expected to produce complicated interactions involving the exchange and recycling
of neutrals and ions among the solar wind, magnetosphere, and regolith. The electrodynamics of Mercury’s magnetosphere are
expected to be equally complex, with strong forcing by the solar wind, magnetic reconnection, and pick-up of planetary ions
all playing roles in the generation of field-aligned electric currents. However, these field-aligned currents do not close
in an ionosphere, but in some other manner. In addition to the insights into magnetospheric physics offered by study of the
solar wind–Mercury system, quantitative specification of the “external” magnetic field generated by magnetospheric currents
is necessary for accurate determination of the strength and multi-polar decomposition of Mercury’s intrinsic magnetic field.
MESSENGER’s highly capable instrumentation and broad orbital coverage will greatly advance our understanding of both the origin
of Mercury’s magnetic field and the acceleration of charged particles in small magnetospheres. In this article, we review
what is known about Mercury’s magnetosphere and describe the MESSENGER science team’s strategy for obtaining answers to the
outstanding science questions surrounding the interaction of the solar wind with Mercury and its small, but dynamic, magnetosphere. 相似文献
18.
Matthew G. Baring 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
It is widely accepted that the prompt transient signal in the 10 keV–10 GeV band from gamma-ray bursts (GRBs) arises from multiple shocks internal to the ultra-relativistic expansion. The detailed understanding of the dissipation and accompanying acceleration at these shocks is a currently topical subject. This paper explores the relationship between GRB prompt emission spectra and the electron (or ion) acceleration properties at the relativistic shocks that pertain to GRB models. The focus is on the array of possible high-energy power-law indices in accelerated populations, highlighting how spectra above 1 MeV can probe the field obliquity in GRB internal shocks, and the character of hydromagnetic turbulence in their environs. It is emphasized that diffusive shock acceleration theory generates no canonical spectrum at relativistic MHD discontinuities. This diversity is commensurate with the significant range of spectral indices discerned in prompt burst emission. Such system diagnostics are now being enhanced by the broad-band spectral coverage of bursts by the Fermi Gamma-Ray Space Telescope; while the Gamma-Ray Burst Monitor (GBM) provides key diagnostics on the lower energy portions of the particle population, the focus here is on constraints in the non-thermal, power-law regime of the particle distribution that are provided by the Large Area Telescope (LAT). 相似文献
19.
Matteo Ceriotti Gregory May-Wilson 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2021,67(9):2865-2877
The direction and magnitude of a solar sail acceleration are strongly related. For this reason, once the characteristic acceleration has been fixed, it is not possible to modulate the acceleration in a particular direction. In this work, a semi-analytical switching control law is derived, enabling a solar sail to emulate a smaller effective characteristic acceleration (without changes in geometry or optical properties); by periodically changing the pitch (cone) angle of the sail, in average over time, the acceleration produced by the sail matches exactly (in both direction and magnitude) that of a “smaller” sail. The range in which this is possible is determined, and the limitations on this range due to the size difference is computed. The method is validated on optimal Earth-Mars trajectories. 相似文献
20.
摘要: Hexapod多自由度微激励系统常用于航天器有效载荷在轨微振动环境的模拟,但采用现有控制方法无法精确稳定跟踪低频正弦加速度,这是由于系统耦合度高、非线性在低频段较强,被控对象相位滞后过大造成的.针对此问题,基于传统离线迭代控制方法,提出一种复合超前校正、多倍频陷波滤波器的改进离线迭代控制方法.其中,离线迭代进行补偿控制,超前校正进一步补偿系统相位,多倍频陷波滤波器去除非线性干扰.跟踪低频定频正弦加速度的实验结果表明,对比传统离线迭代控制方法,改进方法收敛快、控制精度高;对比现有自适应正弦振动控制方法,改进方法将符合精度要求的加速度控制频带下限由14.5 Hz扩宽至8 Hz.实验结果验证了所提方法的有效性. 相似文献