纳米钡铁氧体吸波材料的研究进展

介绍了纳米钡铁氧体的制备方法与吸波性能,结合最新文献论述了离子掺杂纳米钡铁氧体、稀土掺杂纳米钡铁氧体、纳米钡铁氧体复合材料的研究进展,讨论了纳米钡铁氧体吸波材料目前存在的问题及改进措施.     

W 型钡铁氧体的研究进展

W型钡铁氧体具有吸波性能好、价格低廉的特点,因此,越来越引起广泛的重视和深入的研究。本文介绍了W型钡铁氧体BaMe2Fe16O27的主要制备方法,总结了Me为不同元素以及稀土离子掺杂时W型钡铁氧体的研究现状,展望了W型钡铁氧体未来的研究方向。     

镍锌铁氧体吸波材料研究进展

综述了镍锌铁氧体吸波材料的研究情况。从磁性能、配方对吸波性能的影响,以及与其他材料复合对吸波性能的影响等方面,对镍锌铁氧体吸波材料进行比较全面的总结,并与我司研究情况进行对比,希望对镍锌铁氧体吸波材料的开发与应用提供支持。     

前沿碳系/铁氧体复合材料的吸波性能研究

采用雷达吸波材料(RAM)是提高飞机隐身性能的一种有效方法。介绍了RAM的吸波机理,简述了膨胀石墨酚醛树脂、石墨烯碳纳米管复合材料、陶瓷基多层纳米碳管复合材料、手性聚苯胺钡铁氧体复合材料、聚苯胺纳米镍铁氧体复合材料的制备方法,并分别比较分析了各个材料的吸波性能。纳米碳系吸波复合材料具有对X波段电磁波吸收作用强、质量轻、耐环境腐蚀的特点。聚苯胺陶瓷基复合材料具有热稳定性强、耐氧化和腐蚀的特点,其突出优势是在高温下,还能保持很高的吸波性能和机械性能。铁氧体复合材料具有电磁性能强、硬度高、化学稳定性高等特点,并且适用于X波段外电磁波的吸收,吸波范围广。     

镧掺杂镍锌铜铁氧体-聚苯胺复合材料的制备

采用凝胶法制备了Ni0.25Zn0.5Cu0.25LaxFe2-xO4(x=0、0.05、0.1、0.15、0.2)和Ni0.5-yZn0.5CuyLa0.05Fe1.95O4(y=0、0.05、0.1、0.15、0.2),分别在850℃、950℃和1050℃下煅烧得到铁氧体,再与苯胺进行复合制备出镧掺杂镍锌铜铁氧体-聚苯胺复合材料。通过X射线衍射、红外光谱和透射电镜对铁氧体和复合物的结构、形貌和粒径等进行分析,得出铁氧体为尖晶石,复合物形貌呈圆形颗粒状。煅烧温度为1050℃时的复合物粒径为66.7nm,煅烧温度低有利于聚苯胺包裹铁氧体,同时复合物磁性降低;煅烧温度高可以更好地减少杂质和中间体,且随着煅烧温度的升高制得的铁氧体颗粒也增大。随着镧掺杂量的增多,铁氧体的粒径先减小后增大再减小,随着铜的掺杂量的增多,颗粒粒径先减小再增大,表明镧和铜的掺杂影响铁氧体和复合物的性质。     

Zn2+取代W型钡钴铁氧体的制备及其电磁性能研究

采用溶胶-凝胶法制备Zn2+取代W型钡钴铁氧体BaZnxCo2-xFe16O27(x=0.8,1.0,1.2)粉体。利用X-射线衍射、扫描电子显微镜、振动样品磁强计和矢量网络分析仪对样品进行表征。研究焙烧温度以及Zn2+取代量对W型钡钴铁氧体晶体结构的影响。分析不同Zn2+取代量下,W型钡钴铁氧体的微观形貌、磁性能以及微波电磁特性。结果表明:采用溶胶-凝胶法,在焙烧温度为1300℃时,可获得平均晶粒尺寸约为25.06～32.04nm,粒径分布均匀,颗粒尺寸约为3～9μm、部分形状规则且呈六角片状的W型钡钴铁氧体粉体;当x=1.2时,样品室温比饱和磁化强度Ms达最大值,为105.99 A.m2.kg-1;在4～11GHz频段内,样品的磁损耗随着Zn2+取代量的增加而增加,其值为0.2～0.8,而在11～18GHz频段内,磁损耗随着Zn2+掺杂量的增加而减小,其值为0～0.5。     

石墨烯基吸波材料研究新进展

吸波材料的性能是影响雷达隐身的关键因素,其研究对军用和民用都具有非常重要的意义。石墨烯由于其独特的吸波性能,成为吸波材料研究的一大热点。本文综述了石墨烯/铁氧体、石墨烯/金属微粉、石墨烯/磁性金属、石墨烯/导电聚合物和石墨烯/磁性材料/导电聚合物等复合吸波材料在吸波领域的最新研究应用现状,并展望了吸波材料未来发展趋势。     

ZrC/C复合材料性能及微观结构的研究

通过向石墨材料中掺杂氧化锆，制备ZrC／C复合材料。较系统地研究了Zr的加入量对材料性能的影响。结果表明：随着掺Zr量的增加，力学性能不断提高，在掺Zr量为10％时，材料的弯曲强度达最大值，而在掺Zr量为7．5％时，热导率达到最高；进一步研究表明，微观结构影响着材料的力学、热导率等宏观性质。     

烧结温度对Mn-Zn铁氧体吸波性能的影响

研究Mn-Zn铁氧体的烧结温度对其微波吸收性能的影响,选用了5种烧结温度制备铁氧体,并对其作了X-射线衍射相组成分析。实验表明采用1500℃高烧结的铁氧体较其他温度下烧结的吸波性好。     

吸收剂复合改性对材料电磁性能的影响

采用硅烷偶联剂对W型铁氧体类吸收剂和F型铁氧体类吸收剂进行复合改性,通过扫描电镜(SEM)研究偶联剂改性对吸收剂微观结构的影响,分析复合改性对吸波材料电磁性能的影响,并通过有效媒质理论(effective medium theory)讨论吸收剂电磁参数理论值与实际值的差异。结果表明:通过吸收剂复合改性可以实现复合吸波材料的电磁性能调整,实现材料宽带匹配,提高吸波材料吸收效率;改性后的吸波材料在8～18 GHz时反射率小于–10 dB,最小反射值可达–14.5 dB,附着力为6.32 MPa;耐热性能实验后,吸波材料外观和反射率无明显变化,说明复合改性后吸波材料耐环境性能优异。     

La3＋掺杂 Ni0．35 Co0．15 Zn0．5 Fe2 O4铁氧体的制备及微波吸收性能

采用溶胶-凝胶自蔓延法制备 La3＋掺杂 Ni0．35 Co0．15 Zn0．5 Fe2 O4,并研究不同掺杂量对样品微观结构、电磁参数及微波吸收性能的影响。通过 X 射线衍射仪、扫描电镜研究了样品的相结构和微观形貌,使用振动样品磁强计与矢量网络分析仪分别对样品的静态磁性能及在1～12GHz 的电磁参数进行了研究,并计算了不同厚度（3 mm、5 mm、8 mm）下材料的反射损耗。研究表明,适量掺杂 La3＋能够提高 Ni0．35 Co0．15 Zn0．5 Fe2 O4铁氧体的吸波性能,并使吸收频带向高频移动。其中样品 Ni0．35 Co0．15 Zn0．5 La0．04 Fe2 O4与石蜡混合厚度为5mm 时,最小反射损耗为－28．4dB,小于－10dB 带宽为3．7GHz。     

Ti/Al/Ti_(46)Zr_(26)Cu_(17)Ni_(11)非晶层状复合材料界面相组成

利用DSC对真空甩带法制得的Ti_(46)Zr_(26)Cu_(17)Ni_(11)非晶薄带进行热分析,据此选择在693 K(T_g),753 K(T_g~T_(x1)),813 K(T_(x1))下对非晶合金进行不同时间真空热处理,分析非晶晶化行为,并以Ti_(46)Zr_(26)Cu_(17)Ni_(11)非晶合金、TA2和纯Al为原材料,利用Gleeble-3500热模拟试验机在873 K/10 MPa/8 h下制备层状复合材料,采用SEM、TEM、显微硬度计并结合热力学和元素扩散理论对界面层相组成、析出次序和性能进行研究。结果表明:Ti_(46)Zr_(26)Cu_(17)Ni_(11)非晶玻璃转变温度T_g=720 K,初始晶化温度T_(x1)=788 K;非晶晶化首先生成亚稳相I相,随后进一步析出三元或四元Laves相和Ti Ni相;热压后,纯Al和非晶晶化层间界面由薄层Al_3Ni和晶粒细小结构均匀的Al3(Ti0.6Zr0.4)层组成,界面平直无缺陷,总厚度与纯Ti、纯Al间界面层厚度比约为6.5∶1;Al_3(Ti_(0.6)Zr_(0.4))和Al_3Ti硬度相近,分别为(564.20±10.46)HV和(579.83±15.26)HV,但Al_3(Ti_(0.6)Zr_(0.4))层塑性更好。     

钙钛矿型La_(1-x)Ba_xMnO_3(0≤x≤0.5)的红外发射率和微波吸收性能

通过溶胶凝胶法制备钙钛矿结构的La_(1-x)Ba_xMnO_3(0≤x≤0.5),利用X射线衍射、四探针电阻测量仪、红外发射率测试仪、矢量网络分析仪分别研究Ba~(2+)掺杂对镧锰氧化物晶体结构、电阻率、红外发射率和微波吸收性能的影响。研究结果表明:当Ba~(2+)掺杂浓度比较低时,掺杂的元素几乎不改变镧锰氧化物的晶体结构;当掺杂浓度增加时,晶格畸变开始增大;样品红外发射率随Ba~(2+)离子掺杂浓度的增大先降低后缓慢增加,与电阻率的变化保持一致;Ba~(2+)离子可以对样品在2~18 GHz微波吸收性能进行调控,当掺杂浓度x=0.3时,样品的吸收效果最佳;在频率为10.8 GHz时,最低反射率为-32 d B;掺杂合适元素的镧锰氧化物材料有可能应用在红外/雷达兼容隐身领域。     

Al-Cu-Li系合金热轧板材组织、性能和织构的研究

研究了 Al-Cu-Li-( Mn) -( Zr)合金热轧板在 T8态下的显微组织、性能和织构情况。发现因合金的成分不同 ,T8处理对它们造成的影响也不同。其原因主要是由于 Mn、Zr对合金内部的再结晶过程产生了不同的影响。对热轧板的织构和性能测试结果表明 ,晶体学织构与材料的各向异性之间存在着对应关系 ,材料的塑性各向异性比强度各向异性更为严重 ,Mn可以作为控制合金织构和各向异性的重要合金化元素     

时效对快速凝固铝锂合金组织和性能的影响

研究了时效对快速凝固Ａｌ—３．２Ｌｉ—１．２Ｍｇ—０．３Ｃｕ—０．２Ｚｒ合金拉伸性能和微观组织的影响。结果表明,低温长时间时效达到接近峰值状态,合金的综合性能优于高温短时间时效达到峰值状态的综合性能。合金中主要强化相为δ＇（Ａｌ３Ｌｉ）相,Ｃｕ、Ｍｇ起固溶强化。合金中Ｚｒ主要以亚稳态的Ａｌ３Ｚｒ存在,并同时与δ＇相形成（δ＇／Ａｌ３Ｚｒ）相。文中讨论了影响合金塑性的因素,指出界面析出相是快速凝固Ａｌ—Ｌｉ合金中值得重视的问题。     

Characteristics and interpretation of the photometric variability of eta carinae and its nebula

A short review is given on the history of the peculiar variable object Car and on a number of relevant references describing and discussing its physical characteristics and behaviour, based on different types of observational techniques. The star is known to be variable since the 17th century. The excessive mass loss to which it was subject during the 19th century is now visible as an ellipsoidal reflection nebula of 15 diameter: the so-called homunculus. The remainder of the paper is spent on different kinds of problems partly based on the results of a decade of photometric monitoring in the VBLUW photometric system of Walraven. Foreground reddening and reddening by dust in the homunculus are determined and amount to E(B - V) _J = 0 50 and < 6, respectively. Scanning of the homunculus revealed an estimate for the photometric characteristics of the central object, which presumably consists of a massive hot star surrounded by a cooler gas envelope. The total luminosity is derived using fluxes of various sources in the wavelength region 0.15 < < 175 n resulting in M _bol = - 12 3 ± 0 2. The total observed flux corrected for foreground extinction corresponds to a star with R 96 R if T _eff 30 000 K. The mass may be near 150 M . The excess luminosity in 1843, when the star was presumably bolometrically at least 2 5 brighter than at present, may have been caused by envelope-energized pulsations when the star's luminosity was close to its Eddington limit. The temperature should then have been 50 000 K. The mass loss rate, during the excess luminosity phase lasting 30 yr, is estimated to amount to M 4 × 10^-3 M yr^-1. At present the mass loss may be M 10^-4M yr^-1. Since the homunculus is mainly built up from material expelled in the 30 yr interval (from 1830 to 1860), its total mass amounts to M _hom 0.15 M . The historical observations of the colours of Car and a comparison with the characteristics of S Dor type stars, suggest that Car was subject to a number of S Dor type phases similar to those of P Cyg (in the 17th century), S Dor and others. A satisfactory explanation is found for the complete historical light curve. The decrease in light after the 1843 maximum by 9 ^m , presumably consists of a fading of the luminosity excess and the S Dor effect by 2 5 and 3^m, respectively, and a 3 5 extinction by circumstellar dust. The small amplitude light variations which Car showed during the last decade, were studied with the aid of the variations of the Balmer jump. They are presumably caused by temperature variations of the central star.Percy and Welch (1983) (Publ. Astron. Soc. Pacific 95, 491) have observed P Cyg on a number of nights in 1982 and found for the photometric variations a time scale of 30 to 50 days and an amplitude of 0 _. ^m 15.Based partly on observations collected at the ESO, La Silla, Chile.     

Ureilites

Ureilites are a rare group of five stony meteorites — feldsparless achondrites containing diamonds of preterrestrial origin the total weight of them being 315 carats. The whole carbon content in ureilites makes up 1.5–4.1%. Ureilites substantially differ from the other stony meteorites. In comparison with chondrites they are enriched in Mg but depleted in metal, troilite, alkaline elements. All ureilites are very similar by their structure. They contain elongated cavities generally stretched in the same direction. The structure of ureilites is an achondritic porphyric one. These meteorites consist of large olivine grains, there is less clinopyroxene (pigeonite). They contain kamacite (Ni content being 1.5–4%), troilite FeS, chromite. Carbon material is represented by diamond, graphite and organic material being present in a disequilibrium state. Two ureilites (North Haig and Dingo Pup Donga) were considerably oxidized during terrestrial weathering and contain secondary iron oxides.Diamonds are present in ureilites in thin intergrowths with graphite being disposed between silicate grains more or less evenly in the meteorite. The sizes of such black diamond-graphite aggregates are 0.3–0.9 mm. The sizes of the micromonocrystals of diamond and graphite are less than 1. The diamond-graphite aggregates contain dispersed particles of kamacite, troilite, chromite, nickelchrome, being present in very thin intergrowths with one another. Besides the usual diamond there is an admixture of lonsdaleite in the aggregates representing a hexagonal diamond with a würtzite-like structure. Lonsdaleite has been identified in the ureilites Novo Urei, Goalpara, North Haig. The diamonds of ureilites are characterized by inhomogeneities in the crystalline structure which are at least partly caused by the presence of donor nitrogen. According to the isotopic carbon composition the diamond in the meteorite Novo Urei has the value C¹³ = -5.7.The structure peculiarities of ureilites bear witness of the fact that these meteorites had been subject to the action of dynamic pressure about 300–600 kbar. The impact had taken place in cosmic space. All ureilites subdivide into two types: the first type are Novo Urei, Dyalpur, Dingo Pup Donga, the second type are Goalpara, North Haig according to the following signs: (1) olivine grains are finer in ureilites of the second type; (2) twinning is more typical of clinopyroxenes of ureilites belonging to the first type; (3) in ureilites of the first type a net-like iron distribution is observed, in ureilites of the second type kamacite plates are chiefly present between silicate grains; (4) the size of diamondgraphite intergrowths in ureilites of the first type does not exceed 0.3 mm, in ureilites of the second type it reaches 0.9 mm. Ureilites of the first type have undergone a less intensive impact than ureilites of the second type. Certain similarity of the material composition of ureilites and of the material composition of carbonaceous chondrites, the distinction of these two groups of meteorites from all other meteorites bear witness of the fact that ureilites have formed from carbonaceous chondrites during a collision of asteroid bodies in cosmic space, diamonds having been formed from the carbon material of carbonaceous chondrites.