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41.
通过对硅橡胶P6144密封圈的加速老化试验,建立了该密封圈材料在贮存温度下的压缩永久变形和时间的关系,预测了25℃、35℃、45℃、55℃、65℃和75℃温度条件下硅橡胶P6144密封材料的贮存寿命,研究了温度对硅橡胶密封圈贮存寿命的影响规律。 相似文献
42.
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
43.
H. J. Völk 《Space Science Reviews》2007,130(1-4):431-438
The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient
of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce
the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of
Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount
of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar
initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic
Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in
the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming
from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×1018 eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall
Cosmic Ray spectrum. 相似文献
44.
45.
介绍了某型发动机的RT-11燃油调节器加速性不稳定、起飞状态燃油供油量停滞的情况,分析了产生故障的原因和故障机理,并提出了修理中的改进措施。 相似文献
46.
首先对民用飞机电源系统负加速度试飞进行简要说明,提出民用飞机电源系统负加速度试飞的原因和目的。其次对电源系统负加速度试飞条件、试飞方法和试飞程序进行说明。对电源系统负加速试飞结果进行分析评估,表明电源系统设计是满足设计要求和民用航空标准要求的。最后对负加速度试飞中注意事项进行了详细说明,为其它机型飞机进行负加速度试飞提供借鉴。 相似文献
47.
48.
针对退化发动机加速性能下降的现象,提出一种变喘振裕度约束的模型预测控制方法。通过分析退化发动机在加速过程中的工作特点,将加速过程分为三个阶段,在不同阶段采取不同的喘振裕度约束。鉴于模型预测控制能够显式处理约束、采用在线滚动优化来获取最优控制输入,采取模型预测控制方法,并采用具有较高实时性的交替方向乘子法求解优化问题,实现了退化发动机加速性能的恢复。数字仿真结果表明,采用本文所提出的加速性能恢复控制方法后,相比退化发动机,加速过程中所耗费的时间缩短了35%以上。 相似文献
49.
为进行飞机结构载荷安全监控并为飞机结构疲劳寿命评估积累相关数据,需建立与飞行参数相关的 飞机结构载荷模型。针对飞机结构载荷与飞行参数之间的非线性关系,采用改进停机准则的 SMO 算法及粒 子群模型参数优化算法对支持向量机回归方法进行改进,并通过飞行动力学理论分析结合皮尔逊相关系数的 方法对参与建模的飞行参数进行选取。以飞机跨声速俯仰机动为例,建立机翼某一测载剖面结构剪力模型,并 对该建模方法进行仿真验证。结果表明:采用改进支持向量机回归方法所建立模型精度优于原始支持向量机回归方法建立的模型,即采用改进支持向量机回归方法可提高建模精度及泛化能力。 相似文献
50.
为解决普通加工方式易出现工程陶瓷边缘碎裂的问题,本文对超声内圆磨削工程陶瓷边界损伤预测系统进行了研究。在35 kHz轴向超声磨削与普通磨削两种条件下独立进行试验,运用支持向量机研究工艺参数与边界损伤影响规律,采用改进的粒子群算法优化支持向量机,建立采用混合核函数的AHPSO-SVM预测模型。研究结果表明,超声激励下试件边界损伤降幅为10.05%~21.23%,AHPSO-SVM预测模型MSE为0.378 4、平均相对误差为1.369 0%、30次适应度值标准差为0.020 2。相比于普通磨削,超声磨削可使ZTA陶瓷边界损伤值显著降低;建立的AHPSO-SVM模型具有较好的学习能力、泛化性能与良好的稳定性。 相似文献