排序方式： 共有10条查询结果，搜索用时 15 毫秒
1
1.
孙志宏 《测绘与空间地理信息》2014,(8):174-175
针对无人机起飞安全问题,介绍了利用弹射架弹射起飞方式来提高无人机起飞安全系数,并详细阐述了弹射架种类及工作原理。 相似文献
2.
5.12汶川特大地震发生在极其特殊的地质环境中。地震造成的次生地质灾害在有地震记载以来是发育最多,规模最大,摧毁力最强的一次。通过现场调查和资料收集分析,初步分析了地震地质灾害的发育特点,阐明了地震次生地质灾害发生时经历的岩体爆发-弹射抛撒-堆积-再发展的四个过程,同时预测了未来地质灾害发展的趋势。 相似文献
3.
4.
《广东海洋大学学报》2019,(6)
【目的】设计一种适用于大规模网箱养殖的船载式投饵系统。【方法】投饵系统主要由上料装置、下料装置、动力装置、抛撒装置和集中控制系统组成,并安装固定于船舷,进行饵料投喂。其中,以PLC作为集中控制系统的控制核心,通过触摸屏界面实现设备的启停、投料速度调控、运行状态监控及网箱饵料投喂数据的记录等。对投饵系统样机进行试验研究。【结果与结论】投饵系统的投饵速度在0～230 kg/min范围内可调,投饵量精度误差为0.1～1.6 kg,满足容积为127.3～1 145.9 m3的深水网箱投喂要求,降低养殖人员的劳动强度。 相似文献
5.
6.
7.
8.
通过开展含预制单裂隙花岗岩的真三轴单面临空岩爆试验,并利用高速摄像系统和声发射（acoustic emission,简称AE）系统监测岩爆过程,探究了不同产状裂隙岩石的破坏模式、强度变形和声发射演化特性,分析了裂隙产状与岩爆过程及弹射动能之间的关系,对比了含裂隙岩石岩爆发生机制与无裂隙完整岩石的差异。有关力学特性的分析表明,随着裂隙倾角的减小,岩样破坏模式大体呈现由“内剪外劈”向“Z型斜剪”变化的趋势,裂隙对岩石强度的削弱作用不断增大。当裂隙倾角小于30°时,岩石峰值应力普遍仅为完整岩样的一半左右;小倾角裂隙的长度越大,岩样岩板劈裂现象变得显著,形成岩爆坑略微变大,且强度折减幅度越大,峰值轴向应变相应变小;裂隙位置向临空面靠近会加剧岩板的劈裂效应,塑性阶段普遍会产生较大变形并萌生大量裂纹,当裂隙已出露且切断临空面将不易形成岩爆坑。有关岩爆过程及弹射动能的分析表明,随着裂隙倾角的减小,岩样弹射动能呈现先显著降低后小幅回升的变化规律,30°倾角为转变拐点;岩样内部裂隙距临空面越近,裂隙岩样的弹射动能越小;树脂填充裂隙使得岩样弹射动能极大提升,而水泥填充的则无明显提升。有关声发射特征的分析表... 相似文献
9.
The search for periodic behavior in Blazars has been an important subject,which is helpful for providing significant clues to the structure and physical processes of their central energy engine. A binary black hole system has recently been suggested for causing precession of relativistic jets and rotation of the ejection position angle of VLBI knots in superluminal sources. It has been suggested that in QSO 3C345, the ejection direction of the superluminal knots rotates due to the precession of the central engine and thus the ejection position angle of the successive knots shows a periodic behavior. Some authors argue for a period of precession being～5.6 yr (Abraham & Caproni), ～8-10 yr (Klare et al.) and～9.5 yr (Lobanov & Roland). Applying the helical model proposed by Qian et al. and selecting appropriate parameters to fit the initial trajectories (within 0.3 mas) of all the components (C4 to C10), we derive the relation between the ejection position angle of the components and their precession phase, and thus find a 6.9-year precession period (4.3 yr in the source frame), which can fit the ejection position angle of all these superluminal knots well. Since the VLBI observations have covered more than two precession periods, confirmation in one or more future periods would be important.In addition, we emphasize that the initial parts of the trajectories of these knots can be fitted by a common helical pattern (channel) through a precessing of its initial phase.This scenario (or helical precessing model) is different from the usual ballistic precessing model in which the individual superluminal knots move along straight-lines after ejection (Tateyama & Kingham). 相似文献
10.
1