金属橡胶用冷拉拔奥氏体不锈钢丝的微观组织

利用OM(光学显微镜)、SEM(扫描电镜)、TEM(透射电镜)和EBSD(电子背散射衍射)等技术,对金属橡胶用冷拉拔奥氏体不锈钢丝的微观组织进行研究.结果表明,钢丝由α'相的形变诱发马氏体与残余奥氏体相组成,马氏体相的亚结构为孪晶和位错,而残余奥氏体晶粒被细化到微米尺度.同时研究发现了钢丝在拉拔方向上形成的以第二相硬质颗粒为核心的梭形微孔洞.进一步研究分析后认为,Cr17-Ni7系奥氏体不锈钢丝更适合制备高阻尼的金属橡胶材料.     

带旋流杯的模型回流燃烧室主燃孔射流研究

实验研究了带轴径向旋流杯、主燃孔和冷却气流的模型回流燃烧室在工作压力为300 kPa, 燃烧室压力损失为2.5%时主燃孔射流的特点以及其对燃烧室流场的影响.结果表明, 回流式燃烧室内外壁主燃孔射流进气方向与顺流式燃烧室不同, 即内壁主燃孔射流向流动方向下游倾斜, 外壁主燃孔射流向流动方向上游倾斜;主燃孔射流穿透深度很大, 几乎能穿透到对面火焰筒壁;中心回流区长度明显缩短, 其长度L与旋流杯出口直径D的比值(L/D)约为0.5, 而常规的顺流式燃烧室的L/D约为1.3.      

附加分叉射流喷注对气膜孔冷却特性的影响

利用三维数值计算研究具有附加分叉射流喷注的单排气膜孔冷却结构的强化冷却特性,考察了三种形式的分叉孔结构和四个吹风比的影响。研究结果表明,主气膜孔附近射流喷注孔的存在能够诱导一对反涡,削弱缘于主气膜孔下游气膜出流和主流相互作用的肾形涡对,有利于提高气膜冷却效率,同时也增强了对流换热;当分叉射流喷注孔出口与主气膜孔在同一流向位置时,可以获得较高的气膜冷却效率和相对较低的对流换热系数增强比。     

DD6单晶冷却涡轮叶片模拟试样蠕变寿命研究

研究了DD6单晶冷却涡轮叶片模拟试样中气膜孔对蠕变寿命的影响。分别对带气膜孔和不带气膜孔的薄壁圆管试样进行了蠕变测试,带气膜孔试样作为冷却叶片模拟件,不带气膜孔试样与之比较。900％与1000％的蠕变试验结果表明：在相同应力条件下,壁厚为2．0mm试样的蠕变寿命要比壁厚为1．5mm试样的长,带气膜孔试样的蠕变寿命要比不...     

头部及掺混孔对三级旋流器燃烧室出口温度分布影响的试验

对4种不同三级旋流器方案和两种不同掺混孔排布方案的燃烧室在不同进口速度、油气比参数下的出口温度分布进行了常压试验研究,研究结果表明:各方案的出口温度分布系数随进口速度和油气比有所变化,但变化范围不大;中间旋流器与外旋流器旋向相反时,出口温度分布更为均匀;对于两种不同的旋流数组合0.7-1-1.5和1.5-1-0.8,前者出口温度分布系数对外旋流器旋向的改变更为敏感;与方案B相比,方案A的掺混孔排布更加适合该三级旋流器燃烧室;掺混孔排布要与头部结构相匹配,这样才能优化出口温度分布.      

沟槽表面双排孔顺逆组合对气膜冷却的影响

数值模拟研究了双排气膜孔顺逆组合形式对沟槽表面气膜冷却效率影响,孔间距与气膜孔直径之比为5,孔排间距与气膜孔直径之比为12,吹风比为0.3、0.8和1.4。结果表明,在吹风比较小时,沟槽对气膜有显著的导向作用,冷气在相邻的沟槽内部流动。当吹风比增大时,冷气喷到沟槽顶部,导向作用减弱。顺向射流的气膜贴近冷却表面,在低吹风比下气膜冷却效率较高。在高吹风比下,逆向射流覆盖更宽,气膜孔排间叠加效应明显。吹风比为0.3时,逆-逆组合的气膜冷却效率最低,面平均气膜冷却效率为0.07,相比于最高的顺-顺组合的0.13降低46%。当吹风比为0.8时,顺-顺、逆-顺、顺-逆组合的面平均气膜冷却效率相近,约为0.11,其中顺-逆组合气膜冷却效率分布更均匀。吹风比为1.4时,逆-逆组合的面平均气膜冷却效率最高,为0.13,相比于顺-顺组合提升116%。     

带肋横流对凹槽孔气膜冷却特性影响的机理研究

为了探究带肋横流对凹槽孔气膜冷却特性的影响,运用Realizable k-ε湍流模型,对光滑通道、45°肋通道和135°肋通道进气的凹槽孔进行了数值研究,吹风比为0.5、1.0和2.0,主流和横流的进口雷诺数分别为1×104和1×105.结果表明:45°肋通道与光滑通道在气膜孔内具有相似的螺旋流动,但其流量系数相比光滑...     

Fuzzy energy-based dual contours model for automated coronal hole detection in SDO/AIA solar disk images

The presence of coronal holes in solar disk plays an important role in influencing the space weather and generation of the solar wind. As such there lies a requirement in proper study and prediction of coronal holes occurs in the solar disk. This, in turn, arises the necessity of detection of coronal holes present in the solar disk. In this work, a Hough transformed inspired fuzzy-energy simulated dual contours-based segmentation technique has been proposed for the detection and extraction of holes in solar disk. In the proposed method Hough transform has been induced to initialize the contour for the contour-based method of segmentation. In the algorithm, two contours (active and static) have been initiated and made to evolve based on the energy function by incorporating the gray-scale intensity. Here in the work one contour is made to deform its shape while the other contour is kept static for the coronal holes detection purpose. The experiment has been carried out on few benchmark datasets and the corresponding outcomes have been compared with the results of other existing algorithms. The comparison results highlight the performance of the proposed technique in detection of coronal holes in solar disk.     

Analysis of a long-duration AR throughout five solar rotations: Magnetic properties and ejective events

Coronal mass ejections (CMEs), which are among the most magnificent solar eruptions, are a major driver of space weather and can thus affect diverse human technologies. Different processes have been proposed to explain the initiation and release of CMEs from solar active regions (ARs), without reaching consensus on which is the predominant scenario, and thus rendering impossible to accurately predict when a CME is going to erupt from a given AR. To investigate AR magnetic properties that favor CMEs production, we employ multi-spacecraft data to analyze a long duration AR (NOAA 11089, 11100, 11106, 11112 and 11121) throughout its complete lifetime, spanning five Carrington rotations from July to November 2010. We use data from the Solar Dynamics Observatory to study the evolution of the AR magnetic properties during the five near-side passages, and a proxy to follow the magnetic flux changes when no magnetograms are available, i.e. during far-side transits. The ejectivity is studied by characterizing the angular widths, speeds and masses of 108 CMEs that we associated to the AR, when examining a 124-day period. Such an ejectivity tracking was possible thanks to the multi-viewpoint images provided by the Solar-Terrestrial Relations Observatory and Solar and Heliospheric Observatory in a quasi-quadrature configuration. We also inspected the X-ray flares registered by the GOES satellite and found 162 to be associated to the AR under study. Given the substantial number of ejections studied, we use a statistical approach instead of a single-event analysis. We found three well defined periods of very high CMEs activity and two periods with no mass ejections that are preceded or accompanied by characteristic changes in the AR magnetic flux, free magnetic energy and/or presence of electric currents. Our large sample of CMEs and long term study of a single AR, provide further evidence relating AR magnetic activity to CME and Flare production.     

A statistical study of CME-associated flare during the solar cycle 24

We investigate on the relationship between flares and coronal mass ejections (CMEs) in which a flare started before and after the CME events which differ in their physical properties, indicating potentially different initiation mechanisms. The physical properties of two types flare-correlated CME remain an interesting and important question in space weather. We study the relationship between flares and CMEs using a different approach requiring both temporal and spatial constraints during the period from December 1, 2008 to April 30, 2017 in which the CMEs data were acquired by SOHO/LASCO (Solar and Heliospheric Observatory/Large Angle Spectrometric Coronagraph) over the solar cycle 24. The soft X-ray flare flux data, such as flare class, location, onset time and integrated flux, are collected from Geostationary Environmental satellite (GOES) and XRT Flare catalogs. We selected 307 CMEs-flares pairs applying simultaneously temporal and spatial constraints in all events for the distinguish between two associated CME-flare types. We study the correlated properties of coincident flares and CMEs during this period, specifically separating the sample into two types: flares that precede a CME and flares that follow a CME. We found an opposite correlation relationship between the acceleration and velocity of CMEs in the After- and Before-CMEs events. We found a log-log relation between the width and mass of CMEs in the two associated types. The CMEs and flares properties show that there were significant differences in all physical parameters such as (mass, angular width, kinetic energy, speed and acceleration) between two flare-associated CME types.