低铝低燃速HTPB推进剂工艺性能影响研究

为研究固体填料粒度级配及工艺助剂对低铝低燃速HTPB推进剂工艺性能的影响,本文依据固体颗粒堆积最密集排列理论,建立了固体颗粒级配模型,结合固体填料实际粒径,计算得到两种理想刚性球的堆积结果,并在此基础上考察了不同级配配方药浆流动性及触变性。同时,通过筛选工艺助剂种类及优化最适助剂用量,对比了加入不同工艺助剂配方药浆的触变性。结果表明：当采用双二级配模型,计算出的固体颗粒级配比例最优;通过进一步优化固体颗粒级配,结合药浆触变环大小快速判定了推进剂固体级配的合理性,提高了低铝低燃速HTPB推进剂配方工艺性能的可设计性;当工艺助剂选用SU-2,且用量为0.03%时,推进剂工艺性能明显改善,适用期可达596min。     

低铝低燃速HTPB推进剂工艺性能研究

为研究固体填料粒度级配及工艺助剂对低铝低燃速HTPB推进剂工艺性能的影响，依据固体颗粒堆积最密集排列理论，建立了固体颗粒级配模型，结合固体填料实际粒径，计算得到两种理想刚性球的堆积结果，并在此基础上考察了不同级配配方药浆流动性及触变性。同时，通过筛选工艺助剂种类及优化最适助剂用量，对比了加入不同工艺助剂配方药浆的触变性。结果表明：当采用双二级配模型，计算出的固体颗粒级配比例最优；通过进一步优化固体颗粒级配，结合药浆触变环大小快速判定了推进剂固体级配的合理性，提高了低铝低燃速HTPB推进剂配方工艺性能的可设计性；当工艺助剂选用SU-2，且用量为0.03%时，推进剂工艺性能明显改善，适用期可达596min。     

复合固体推进剂性能的一个转折点

复合固体推进剂其结构可视为有机液体粘合剂和无机固体填料两部分组成。其固体填料的重量百分数已达八十以上。所以固钵填料的含量,颗粒级配,颗粒形状及颗粒的表面性质将对装药工艺和推进剂药柱性能产生很大影响。本文通过对固体氧化剂颗粒的性质研究,并对氧化剂颗粒对药浆流变性、力学性能和燃烧性能影响的资料作了初步分析发现:在氧化剂颗粒临界直径附近处,各项性能存在着一个转折点。我们可以利用这个转折点来进行配方设计,调节配方性能的依据。对该转折点的认识,将有利于进一步开展性能研究和预测,对转折点存在的机理也有待于进一步探讨。     

推进剂药浆粘弹性特征研究

用ＣＶ２０Ｎ流变仪研究了ＨＴＰＢ推进剂、ＣＴＰＢ推进剂和聚醚推进剂药浆的粘弹性特征。结果表明：推进剂药浆为粘弹性流体,复合粘度随推进剂品种、配方特点、频率范围不同而呈不同变化规律,复合模量、损耗模量和贮能模量随频率增加均呈上升趋势;损耗模量一般比相应贮能模量高约一个数量级;贮能模量存在数个衰减峰;衰减峰与损耗角正切峰成对映。提出了推进剂药浆流体的结构模式,并用它解释了药浆的粘弹性。     

复合固体推进剂药浆粘度的预估

本文通过对影响固体推进剂药浆粘度的因素进行分析和相关试验,导得了药浆粘度预估的数学关系式。试验结果表明,对含过氯酸铵推进剂药浆粘度的预估值93％的数据在实验值的±15％内;对含铝粉推进剂药浆粘度的预估值92％的数据在实测值的±20％范围内。     

关于复合固体推进剂批次间性能差异的研究(报告之二:药浆的粘度分析)

复合固体推进剂药浆是固体粒子含量很高的粘性流体。影响其粘度的除了粘结剂的度粘外,主要还有固体粒子的容积百分比和尺寸匹配。文中介绍了计算药浆粘度公式,还就粒子形状、尺寸、表面性质对有粒子悬浮的浆液粘性影响作简要回顾。文中还指出,由于药浆的固体粒子含量高,用不同测试方法测得的药浆粘度可能会差距甚大以及粒子容积含量的少量不均匀性可能会导致粘度值差很多。     

AP包覆硼对富燃推进剂药浆流变特性的影响

用四种不同量AP包覆的硼粉,对硼含量达30%的富燃推进剂实验配方中的药浆流变特性进行了研究,结果表明:20%AP包覆硼粉的含硼富燃固体推进剂药浆的流变性与另三种硼粉的明显不同———近6h粘度为2 2kPa·s,屈服值在300Pa以下,表明其药浆流平性好并可满足浇铸要求。20%AP包覆硼的合适包覆量、包覆完整的表面性质及近似球型粒子的形状决定了其药浆的流变特性最优。     

双级配的氧化剂粒度对推进剂中铝燃烧的影响

本文通过实验研究,从凝聚程度的大小和燃烧完全性两方面,证实了氧化剂AP粒度是影响推进剂中铝燃烧的重要因素,实验结果支持了Cohen,N.S.提出的“口袋模型”。本文对双级配的AP粒度的影响进行了较为详细的讨论,提出在实际配方中较为合适的氧化剂级配比例范围。     

氨基甲酸酯基对推进剂工艺性能的影响

用甲苯二异氰酸酯封端的丁羟粘合剂进行推进剂制药实验，经测定药浆流变特性，研究了聚氨酯推进剂中氨基甲酸酯基对药浆工艺性能的影响。结果表明：氨基甲酸酯基对改善聚氨酸推进剂的药浆工艺性能有重要作用。氨基甲酸酯基与相连的粘合剂大分子一起作用，可增加推进剂填料颗粒的表面润湿性、分散性和推进剂药浆二相流的连续性，从而显著降低药浆屈服值、减少假塑性，改善推进剂的工艺性能。     

NEPE高能推进剂力学性能模拟计算

将颗粒填充聚合物三相结构(颗粒相-中间相-基体相)和粘弹模型相结合,提出了NEPE高能固体推进剂三相结构粘弹模型,建立了NEPE高能推进剂力学性能与其配方组成、固体填料粒径及级配、弹性母体(基体)的拉伸强度和模量、界面层模量等参数的数学关系,进行了编程计算,其拉伸强度和伸长率90%的计算值和测试结果相对误差小于20%。     

固体火箭喷管颗粒尺寸分级两相跨音速流场计算

本文中对固体火箭喷管颗粒尺寸分级的两相跨音速流场作了计算.气相控制方程采用隐式近似因子分解法求解,尺寸分级的颗粒控制方程采用特征线求解,然后,二者进行充分的耦合,可以获得固体火箭发动机含有任意颗粒质量分数和不同颗粒尺寸时轴对称喷管跨音速流场的参数分布.文中讨论了不同颗粒半径和质量分数对流场的影响,对单一颗粒尺寸和颗粒尺寸分级的参数进行了比较.两相耦合计算的迭代收敛速度取决于气相,本文中气相方程求解的格式除部分边界外是隐式的,CFL数可取至6左右,收敛速度快.特别是对颗粒尺寸分级的计算,得益更大,其得益的倍数为颗粒的分级数.     

纳米/微米粉体填料对推进剂浆料特性的影响

高性能固体推进剂配方中往往需要引入纳米或微米级粉体材料。为了获得各种超细粉体对推进剂浆料特性的影响，分别研究了粉体填料的粒度大小、品种、组合使用以及表面包覆处理等对推进剂浆料的粘度、分散性及机械感度的影响。结果表明，粉体填料的粒度减小，浆料的粘度增大；粉体填料的种类不同，对浆料粘度的影响也不同，其中超细高氯酸铵对浆料粘度影响最大；粉体填料的表面经适当包覆处理后对浆料的粘度、机械感度及分散性都有明显改善。     

模型发动机内凝相颗粒碰撞的数值模拟

针对燃烧室内的高温液态凝相粒子,利用所建立的数学模型对聚集状态下粒子间的碰撞与聚合及其与发动机壳体之间的相互作用过程开展了数值分析,获得了收敛管内壁面上液膜厚度及从出口处逃逸的粒子直径分布,并和实验数据进行了比较分析。结果表明在发动机两相内流场计算中,将凝相粒子看成无蒸发的液滴更为合适;聚集状态下凝相粒子间的碰撞与聚合对粒子直径的分布有很大的影响;粒子和壁面之间的相互碰撞不但会导致大量小尺寸粒子的生成,而且也是收敛管内壁面上金属膜形成的直接原因。     

对二维复杂湍流剪切流动数学模型的新探索

 在复杂湍流剪切流中经常会遇到雷诺剪应力与法向速度梯度的反号问题,此时涡粘性假设不再适用。Hinze从湍流结构中存在大涡的概念出发提出了包含台劳级数二阶项的剪应力表达式,取得了正确的定性结果。作者进一步分析了Hinze公式,认为他未能取得合理的定量结果的主要原因,在于他的公式隐含着假设流体微团在大涡的输送作用下能对原有的平均动量有足够的记忆。本文从实验与计算的比较以及近代对湍流结构的知识出发,提出了新的假设。认为较小尺度的湍流结构在大涡的输送作用下能对所包含的剪应力有足够的记忆,在此假设下,推出了新的湍流剪应力表达式,计算结果与实验数据的初步比较说明了此假设的合理性。     

Viscosity effects on weak irregular reflection of shock waves in steady flow

The viscosity effects on weak shock wave reflection are investigated with the Navier–Stokes and DSMC flow solvers. It is shown that the viscosity plays a crucial role in the vicinity of three-shock intersection. Instead of a singular triple point, in viscous flow there is a smooth three shock transition zone, where one-dimensional shock jump relations cannot be applied. At the flow parameters corresponding to the von Neumann reflection, when no inviscid three-shock solution exists, the computations predict an irregular shock-wave configuration similar to that observed previously in experiments. The existence of a viscous zone in the region of shock-wave interaction allows a continuous transition from the parameters behind the Mach stem to the parameters behind the reflected shock, which is impossible in the inviscid three-shock theory. Results of numerical simulations agree qualitatively with the conclusions of the approximate viscous theory, which describes the flow in the vicinity of the three-shock intersection.     

Evolution of the Protosolar Nebula and Formation of the Giant Planets

The formation of planetary systems is intimately tied to the question of the evolution of the gas and solid material in the early nebula. Current models of evolution of circumstellar disks are reviewed here with emphasis on the so-called “alpha models” in which angular momentum is transported outward by turbulent viscosity, parameterized by an dimensionless parameter α. A simple 1D model of protoplanetary disks that includes gas and embedded particles is used to introduce key questions on planetesimal formation. This model includes the aerodynamic properties of solid ice and rock grains to calculate their migration and growth. We show that the evolution of the nebula and migration and growth of its solids proceed on timescales that are generally not much longer than the timescale necessary to fully form the star-disk system from the molecular cloud. Contrary to a widely used approach, planet formation therefore can neither be studied in a static nebula nor in a nebula evolving from an arbitrary initial condition. We propose a simple approach to both account for sedimentation from the molecular cloud onto the disk, disk evolution and migration of solids. Giant planets have key roles in the history of the forming Solar System: they formed relatively early, when a significant amount of hydrogen and helium were still present in the nebula, and have a mass that is a sizable fraction of the disk mass at any given time. Their composition is also of interest because when compared to the solar composition, their enrichment in elements other than hydrogen and helium is a witness of sorting processes that occured in the protosolar nebula. We review likely scenarios capable of explaining both the presence of central dense cores in Jupiter, Saturn, Uranus and Neptune and their global composition. This revised version was published online in August 2006 with corrections to the Cover Date.     

A cosmochemical view of cosmic rays and solar particles

The composition of cosmic rays and solar particles is reviewed with emphasis on the question of whether they are representative samples of Galactic and solar matter. The composition of solar particles changes with energy and from flare to flare. A strong excess of heavy elements at energies below a few MeV/nuc decreases with energy, and at energies above 15 MeV/nuc the composition of solar particles resembles that of galactic cosmic rays somewhat better than that of the solar atmosphere. The elements Ne through Pb have remarkably similar abundances in cosmic ray sources and in the matter of the solar system. The lighter elements are depleted in cosmic rays, whereas U and Th may be enriched or not, depending on whether the meteoritic or solar abundance of Th is used. Two prototype sources of cosmic rays are considered: gas with solar system composition but enriched in elements with Z > 8 during acceleration and emission (by analogy with solar particle emission), and highly evolved matter enriched in r-process elements such as U, Th and transuranic elements. The energy-dependence of cosmic ray composition suggests that both sources may contribute at different energies.Miller Institute Professor, 1972–73.     

团聚硼粉与HTPB混合物流变特性

利用HAAKE流变仪研究了硼粉团聚方法、粒度、填充比例对B/HTPB混合物流变性能影响。结果表明,对于LiF包覆的硼粉(B/F),小颗粒的LiF增强了与HTPB预聚物的物理吸附作用,使体系的表观黏度反而大于未包覆的硼粉;采用HTPB包覆的硼粉(B/H,B/F/H)与HTPB混合物的表观黏度和屈服值远小于未处理硼粉,且随混合时间增加而保持不变。在相同填充质量下,小粒度团聚硼粉的黏度系数K值较大,n值较小,严重偏离牛顿流体。当团聚硼粉/HTPB质量比为55/45时,混合物的流动方程转变为Herschel-Bulkley方程,大粒度团聚硼粉的屈服值较小。因此,与小粒度硼粉相比,大粒度团聚硼粉与HTPB的混合物具有较好的流变性能。含大粒度团聚硼粉富燃料推进剂药浆具有良好的工艺性能,6 h内表观黏度小于1500 Pa.s,屈服值小于150 Pa。