Cf/SiC复合材料先驱体转化法浸渍工艺条件优化

主要研究了先驱体转化法制备碳纤维三维编织物增强陶瓷基复合材料的浸渍工艺条件,探讨了不同温度,压力对PCS／DVB溶液法和PCS熔融法浸渍效率的影响,优化出最佳浸渍工艺参数。结果表明,温度对PCS／DVB溶液粘度影响较大,升高温度可急剧降低PCS／DVB溶液的粘度,有利于浸渍。PCS／DVB溶液法浸渍的最佳工艺参数为：50－60度,2MPa,PCS熔融法浸渍的最佳工艺参数为：300度,2MPa,采用PCS／DVB溶液法浸渍时的浸渍效率优于PCS熔融法,经四个浸渍裂解周期后溶液法制备的材料密度（1．53g/cm3-1.61g/cm3)明显优于先驱体熔融法（1．43g/cm3-1.52g/cm3)     

航空发动机用连续SiC_f/SiC复合材料制备工艺及应用前景

介绍了连续碳化硅纤维增强碳化硅基复合材料(SiC_f/Si C)常见的3种制备工艺,即化学气相渗透(CVI)工艺、前驱体浸渍/裂解(PIP)工艺及熔渗(MI)工艺的不同特点,探讨了国外不同工艺制备的复合材料的基本性能,并简述了SiC_f/SiC陶瓷基复合材料在航空发动机上的应用情况,以期为该材料在国内航空发动机领域的发展提供一定的参考。     

有机硅聚合物制备的陶瓷材料高温结晶与氧化机理研究进展

综述了高温结构陶瓷材料在高温条件下结晶机理及氧化理论，对各种理论模型进行了评介，其中重点介绍了Si-C-(O)-(N)体系的“无定型－成核－晶粒长大”结晶机理和Si-C-N体系的“分离－分解－结晶”结晶机理，并具体介绍了Si-C-N-O和Si-(B)-C-N高温氧化机理。     

二乙烯基苯/聚碳硅烷的配比与交联研究

以二乙烯基苯(DVB)为交联剂，通过改变其与先驱体聚碳硅烷(PCS)的配比，研究了PCS体系的交联性质。结果表明：DVB在该体系中具有交联剂和溶剂双重作用，降低DVB的配比，可以提高陶瓷产率，DVB的配比以0．4为宜；为减少体系中的DVB，添加了PCS的良性溶剂四氢呋喃，使陶瓷产率达到了76％。结构研究还发现，该体系交联反应主要以DVB自交联形式进行，DVB与PCS之间的硅氢化反应不明显。     

低氧含量SiC纤维研究进展

为制备耐高温性能良好的SiC纤维，必须降低纤维中的氧含量，本文详细综述了国内外先驱体转化法制备Sic纤维中降低氧含量的方法，分析了各种方法的优缺点，比较可行有效的方法有电子束／γ射线辐射交联法、高温脱氧法和低度预氧化 热交联法，为制备高性能SiC纤维提供了一些参考。     

液态聚碳硅烷先驱体制备陶瓷基复合材料的工艺适应性研究

陶瓷先驱体是先驱体浸渍裂解工艺(PIP)制备陶瓷基复合材料的关键,先驱体工艺性能对复合材料制备工艺和材料性能有着决定性的影响。以一种新型液态聚碳硅烷先驱体(VHPCS)为研究对象,利用红外光谱分析差示扫描量热分析、热重分析、X-射线衍射分析等分析手段对VHPCS及其裂解产物的热稳定性进行表征。从PIP工艺角度出发,对VHPCS固化行为和裂解行为进行分析。结果表明,VHPCS中含有活性的Si-H和Si-CH=CH2基团,可在165℃开始固化反应。VHPCS在1000℃的N2气氛下的陶瓷产率为60%,其裂解产物在1000~1300℃内晶相稳定,是比较理想的陶瓷先驱体。     

氮化硅高温透波材料的研究现状和展望

从氮化硅的晶体结构出发,介绍了氮化硅陶瓷优良的性能,综述了近年来氮化硅透波纤维和氮化硅基透波复合材料的研究进展,并对现有氮化硅高温透波材料体系存在的问题及其未来的发展趋势作了展望.     

聚硅乙炔改性硅硼碳氮前驱体的合成与性能研究

以聚硅乙炔(PMSA)为交联剂,改性硅硼碳氮(SiBCN)陶瓷前驱体,对前驱体的合成与裂解行为进行了详细研究.该前驱体陶瓷产率高(＞80wt％),并且陶瓷产物致密、抗氧化性能优良.采用FT-IR对改性前驱体的结构进行了表征,采用DSC、TGA、XRD、马弗炉煅烧等方法对改性前驱体固化行为及其裂解产物的高温稳定性能、抗氧...     

An application of the weighted horizontal magnetic gradient to solar compact and eruptive events

We propose to apply the weighted horizontal magnetic gradient (${\mathit{WG}}_M$), introduced in Korsós et al., 2015, for analysing the pre-flare and pre-CME behaviour and evolution of Active Regions (ARs) using the SDO/HMI-Debrecen Data catalogue. To demonstrate the power of investigative capabilities of the ${\mathit{WG}}_M$ method, in terms of flare and CME eruptions, we studied two typical ARs, namely, AR 12158 and AR 12192. The choice of ARs represent canonical cases. AR 12158 produced an X1.6 flare with fast “halo” CME ($v_{\mathit{linear}}$ = 1267 $\text{km}{\text{s}}^{-1}$) while in AR 12192 there occurred a range of powerful X-class eruptions, i.e. X1.1, X1.6, X3.1, X1.0, X2.0 and X2.0-class energetic flares, interestingly, none with an accompanying CME. The value itself and temporal variation of ${\mathit{WG}}_M$ is found to possess potentially important diagnostic information about the intensity of the expected flare class. Furthermore, we have also estimated the flare onset time from the relationship of duration of converging and diverging motions of the area-weighted barycenters of two subgroups of opposite magnetic polarities. This test turns out not only to provide information about the intensity of the expected flare-class and the flare onset time but may also indicate whether a flare will occur with/without fast CME. We have also found that, in the case when the negative polarity barycenter has moved around and the positive one “remained” at the same coordinates preceding eruption, the flare occurred with fast “halo” CME. Otherwise, when both the negative and the positive polarity barycenters have moved around, the AR produced flares without CME. If these properties found for the movement of the barycenters are generic pre-cursors of CME eruption (or lack of it), identifying them may serve as an excellent pre-condition for refining the forecast of the lift-off of CMEs.     

Detailed analysis of dynamic evolution of three Active Regions at the photospheric level before flare and CME occurrence

We present a combined analysis of the applications of the weighted horizontal magnetic gradient (denoted as ${\mathit{WG}}_M$ in Korsós et al. (2015)) method and the magnetic helicity tool (Berger and Field, 1984) employed for three active regions (ARs), namely NOAA AR 11261, AR 11283 and AR 11429. We analysed the time series of photospheric data from the Solar Dynamics Observatory taken between August 2011 and March 2012. During this period the three ARs produced a series of flares (eight M- and six X-class) and coronal mass ejections (CMEs). AR 11261 had four M-class flares and one of them was accompanied by a fast CME. AR 11283 had similar activities with two M- and two X-class flares, but only with a slow CME. Finally, AR 11429 was the most powerful of the three ARs as it hosted five compact and large solar flare and CME eruptions. For applying the ${\mathit{WG}}_M$ method we employed the Debrecen sunspot data catalogue, and, for estimating the magnetic helicity at photospheric level we used the Space-weather HMI Active Region Patches (SHARP’s) vector magnetograms from SDO/HMI (Solar Dynamics Observatory/Helioseismic and Magnetic Imager). We followed the evolution of the components of the ${\mathit{WG}}_M$ and the magnetic helicity before the flare and CME occurrences. We found a unique and mutually shared behaviour, called the U-shaped pattern, of the weighted distance component of ${\mathit{WG}}_M$ and of the shearing component of the helicity flux before the flare and CME eruptions. This common pattern is associated with the decreasing-receding phases yet reported only known to be a necessary feature prior to solar flare eruption(s) but found now at the same time in the evolution of the shearing helicity flux. This result leads to the conclusions that (i) the shearing motion of photospheric magnetic field may be a key driver for solar eruption in addition to the flux emerging process, and that (ii) the found decreasing-approaching pattern in the evolution of shearing helicity flux may be another precursor indicator for improving the forecasting of solar eruptions.