Sunspot activity and cosmic ray modulation at 1 a.u. for 1900–2013

The descent of sunspot cycle 23 to an unprecedented minimum of long duration in 2006–2009 led to a prolonged galactic cosmic ray (GCR) recovery to the highest level observed in the instrumental era for a variety of energetic charged particle species on Earth, over a wide range of rigidities. The remarkable GCR increase measured by several ground-based, balloon-borne, and detectors on a satellite is described and discussed. It is accompanied by a decrease in solar wind velocity and interplanetary magnetic field at 1 a.u., reaching the lowest values since measurements of the solar wind began in October 1963; the solar polar field strength (μT) measured at the Wilcox Solar Observatory (WSO) is also significantly reduced compared to prior cycles since the start of the program in 1976, the polar field in the northern hemisphere reversed in June 2012 and again in February 2014, that in the southern hemisphere reversed in July 2013. If updates of WSO data confirm the second reversal in northern solar hemisphere, it would pose a serious challenge to the Dynamo Theory. The long-term change in solar behavior may have begun in 1992, perhaps earlier. The physical underpinnings of these solar changes need to be understood and their effect on GCR modulation processes clarified. The study discusses the recent phenomena in the context of GCR modulation since 1900. These happenings affected our empirical predictions for the key parameters for the next two sunspot cycles (they may be progressively less active than sunspot cycle 24) but it enhanced support for our prediction that solar activity is descending into a Dalton-like grand minimum in the middle of the twentyfirst century, reducing the frequency of the coronal mass ejections; they determine the space weather affecting the quality of life on Earth, radiation dose for hardware and human activities in space as well as the frequency of large Forbush decreases at 1 a.u.     

工艺参数对电弧增材制造2219铝合金微气孔缺陷的影响分析北大核心CSCD

微气孔是电弧增材制造2219铝合金面临的主要问题。采用Advanced CMT+P(变极性CMT+脉冲)熔滴过渡模式,研究了EP/EN(正负半周波数)、扫描速度、送丝速度等电弧增材工艺参数对成形2219铝合金微气孔缺陷的影响规律。结果表明:通过改变EP/EN、扫描速度、送丝速度等参数调控热输入可影响气孔率;在热输入较低时,气孔以形核和长大为主,随热输入增加微气孔数量增多、尺寸增大;在热输入较高时,气孔逸出开始占优,随热输入增加微气孔数量减少;在热输入低至230.5或高至439.5 J/mm时,平均气孔率均可降低至0.2%以下。     

气体自发光在高超声速流场显示中的应用

提出了利用高焓气体自发光作为高超声速流场显示的方法,介绍了在使用高焓运行的激波风洞中,对二维模型的高超声速绕流流场使用此种方法的初步结果,可观察到二维棱形柱的尾流和马赫波的相交。结果表明此种方法不需外加光源,对于结构限制无法设置透明部件的模型,无疑是简单可行的。     

鸭式布局飞机矢量喷流对地面效应影响的风洞试验

针对单发鸭式布局飞机,通过低速风洞试验,研究了矢量喷流对飞机地面效应的影响特性。研究结果表明：发动机喷流使得飞机的地面效应增强,升力系数增加,降低飞机起飞/降落时的飞行速度,缩短起降距离,从而改善飞机起降性能。发动机喷管上/下偏转时,矢量喷流对飞机上下表面气流诱导不对称,均使地面效应阻力系数增量减小。在此基础上,基于数值模拟结果对喷流与地面效应的相互作用机理进行了分析。     

利用常规风洞进行二元翼型试验的竖置全跨方法

采用竖置全跨试验方案,在CARDC(中国空气动力研究与发展中心)4米×3米风洞进行了几个二元翼型模型风洞试验。最初选用的模型是NASA GA(W)-1翼型,并作为校验模型。试验雷诺数高达4.69×100~6,攻角范围为-10～24°,试验结果相当满意。     

高升力多段翼型洞壁干扰修正

 Erisson对高升力多段翼型的洞壁干扰问题进行过理论计算。Moury和Labrujère对上述问题也进行过一些研究,可惜Moury的实验是在开闭比为20％的开孔壁风洞中进行的,而Labrujère仅给出个别情况的实验结果,且其测压点较多,计算较繁,不易实时处理。     

低速风洞半模实验壁压法洞壁干扰修正

 <正> 1.前言 低速风洞半模实验有许多优点,但伴随而来的是洞壁干扰修正问题。大迎角、大堵塞度情况洞壁干扰修正值相当大。如某后掠大展弦比机翼半模,迎角90°时堵塞度达18％,阻力系数洞壁干扰修正值可达真实值的70％。又如某农机机翼半模,迎角40°时堵塞度达8％。压力系数洞壁干扰修正值达真实值的30％。因此,在进行半模实验时,洞壁干扰修正的准确性十分重要。     

风对建筑绕流流动的数值方法

本文利用k-ε湍流模型及SIMPLE方法,在二维条件下,就风对建筑绕流流动进行了数值模拟,建筑及地面的边界条件采用以低Re数k-ε湍流模型中导出的壁函数处理近壁湍流。自由边界采用外推格式。对于计算域中的建筑物则利用控制粘性系数的方法处理。并对计算结果和风洞实验进行了比较。 为了研究建筑物之间的气流及压力分布,本文还对并列两栋建筑的不同情况进行了数值计算和分析。     

Global Response of Martian Plasma Environment to an Interplanetary Structure: From Ena and Plasma Observations at Mars

As a part of the global plasma environment study of Mars and its response to the solar wind, we have analyzed a peculiar case of the subsolar energetic neutral atom (ENA) jet observed on June 7, 2004 by the Neutral Particle Detector (NPD) on board the Mars Express satellite. The “subsolar ENA jet” is generated by the interaction between the solar wind and the Martian exosphere, and is one of the most intense sources of ENA flux observed in the vicinity of Mars. On June 7, 2004 (orbit 485 of Mars Express), the NPD observed a very intense subsolar ENA jet, which then abruptly decreased within ∼10 sec followed by quasi-periodic (∼1 min) flux variations. Simultaneously, the plasma sensors detected a solar wind structure, which was most likely an interplanetary shock surface. The abrupt decrease of the ENA flux and the quasi-periodic flux variations can be understood in the framework of the global response of the Martian plasma obstacle to the interplanetary shock. The generation region of the subsolar ENA jet was pushed towards the planet by the interplanetary shock; and therefore, Mars Express went out of the ENA jet region. Associated global vibrations of the Martian plasma obstacle may have been the cause of the quasi-periodic flux variations of the ENA flux at the spacecraft location.