FINITE DIFFERENCE MODEL FOR SIMULATION OF DENSIFYING CARBON-CARBON COMPOSITES BY CHEMICAL VAPOR INFILTRATIONP ROCESSES

ＮｏｍｅｎｃｌａｔｕｒｅｓＡ０—ｃｏｅｆｉｃｉｅｎｔｏｆｔｈｅＡｒｈｅｎｉｕｓｅｑｕａｔｉｏｎＣ（ｎ）—ｈｙｄｒｏｃａｒｂｏｎｃｏｎｃｅｎｔｒａｔｉｏｎｉｎｕｎｉｔ（ｎ）（ｍｏｌ／ｃｍ３）Ｃ０—ｈｙｄｒｏｃａｒｂｏｎｃｏｎｃｅｎｔｒａｔｉｏｎａｔｅｘ...     

On initial steps of chemical prebiotic evolution: Triggering autocatalytic reaction of oligomerization

Searching for extraterrestrial life attracts more and more attention. However this searching hardly can be effective without sufficiently universal concept of life origin, which incidentally tackles a problem of origin of life on the Earth. A concept of initial stages of life origin is stated in the paper. The concept eliminates key difficulties in the problem of life origin, and allows experimental verification of it. According to the concept the predecessor of living beings has to be sufficiently simple to provide non-zero probability of self-assembling during short (in geological or cosmic scale) time. In addition the predecessor has to be capable of autocatalysis, and further complication (evolution). A possible scenario of initial stage of life origin, which can be realized both on other planets, and inside experimental facility is considered. In the scope of the scenario a theoretical model of multivariate oligomeric autocatalyst is presented. Results of computer simulation of two versions of oligomeric autocatalytic reactions are presented. It is shown that the contribution of monomer activation reaction is essential, and in some cases autocatalysis in polymerizing reaction can be achieved without catalyzing proper monomer binding reaction.     

Comets and Chemical Composition

It is commonly believed that comets are made of primordial material. As a consequence, they can reveal more information about the origin of our solar system. To interpret the coma composition measurements of comet Churyumov–Gerasimenko that will be collected by the Rosetta mission, models of the coma chemistry have to be constructed. However, programming the chemistry of a cometary coma is extremely complex due to the large number of species and reactions involved. Moreover, such a program needs to be very flexible as one may want to extend, change, or update the set of species, reactions, and reaction rates. Therefore, we developed software to manage a database of species and reactions and to generate code automatically to compute source/loss balances. This database includes the data from the UMIST database and the ion–molecule reactions collected by V.G. Anicich. To use all these databases together, a lot of practical problems need to be solved, but the result is an enormous source of information about chemical reactions that can be used in chemical models, not only for comets but also for other applications.     

The primordial Helium-4 abundance determination: systematic effects

By extrapolating to O/H = N/H = 0 the empirical correlations Y–O/H and Y–N/H defined by a relatively large sample of 45 Blue Compact Dwarfs (BCDs), we have obtained a primordial ⁴Helium mass fraction Y _p=0.2443±0.0015 with dY/dZ=2.4±1.0. This result is in excellent agreement with the average Y _p=0.2452±0.0015 determined in the two most metal-deficient BCDs known, I Zw 18 (Z /50) and SBS 0335–052 (Z /41), where the correction for He production is smallest. The quoted error (1) of 1% is statistical and does not include systematic effects. We examine various systematic effects including collisional excitation of hydrogen lines, ionization structure and temperature fluctuation effects, and underlying stellar Hei absorption, and conclude that combining all systematic effects, our Y _p may be underestimated by 2–4%. Taken at face value, our Y _p implies a baryon-to-photon number ratio =(4.7^+1.0 _–0.8)×10^–10 and a baryon mass fraction _b h ² ₁₀₀=0.017±0.005 (2), consistent with the values obtained from deuterium and Cosmic Microwave Background measurements. Correcting Y _p upward by 2–4% would make the agreement even better.     

Helium-3: Status and Prospects

We report on our continuing efforts to determine 3He abundances in H II regions and planetary nebulae. Our detections of 3He in some PNe show that some stars produce large amounts of 3He. However the H II region abundances show no evidence for this production. From our sample of > 40 H II regions, the subsample which should yield the most reliable abundances has 3He/H abundances which scatter between 1-2 × 10-5. There is no trend with either galactocentric distance or metallicity. Even if we do not understand the underlying mechanisms, we see empirically that stars neither produce nor destroy 3He in a major way. We thus suggest that the level of the "3He Plateau" (3He/H = 1.5 _-0.5 ^+1.0 × 10^-5) is a reasonable estimate for the primordial 3He.     

用准稳态方法建立碳氢燃料点火燃烧的简化化学反应动力学模型

基于“准稳态”方法建立了一套碳氢燃料点火燃烧的化学反应动力学模型简化方法和相应的软件SPARCK,并从甲烷点火燃烧的GRI2.11详细基元反应动力学模型出发简化得出了包含16个组分12步总包反应形式的简化化学反应动力学模型,从庚烷点火燃烧的详细基元反应动力学模型出发简化得出了包含25个组分21步总包反应形式的简化化学反应动力学模型。通过其计算结果与CARM软件导出简化模型的计算结果和典型激波管试验结果的对比可以看出,本文简化得到的简化反应动力学模型能较为有效地再现详细基元反应模型的反应机理,简化模型的计算精度与CARM软件导出简化模型的计算精度相当。与详细基元反应动力学模型相比,简化模型有效地减少了反应组分,在工程计算中有比较好的应用前景。     

基于预测的计算网格负载平衡研究

计算网格中负载平衡有着重要的作用和显著的效果.预测节点性能是实现动态负载平衡的关键,本文首先引入预测网格节点性能的指数平滑算法,讨论了平滑系数的选取方法.然后设计一个负载平衡实验,实验证明使用基于该预测算法的动态负载平衡与静态负载平衡和不使用负载平衡时任务执行效率有明显的提高.     

单循环脉冲爆轰发动机内外流场的动力学结构

对脉冲爆轰发动机由高温火团引发的甲烷-空气混合气体爆轰过程和管内、外轴对称流场分布进行数值模拟,考虑了CH4-O2-N2的19个基元反应和14种组份。计算结果反映了爆轰管出口端附近区域的激波衍射,涡环及复杂的涡与激波相互作用情况等,描绘了管内、外流场的动力学结构。     

RDX－CMDB推进剂铅－铜－炭催化燃速模型

分析了ＲＤＸ在平台催化中的作用，认为ＲＤＸ对平台催化有正、负两方面的影响。据此提出了ＲＤＸ－ＣＭＤＢ推进剂平台催化燃速模型。导出的燃速公式能够定量地描述平台燃烧现象的各个阶段。在ＭＴＷ－１推进剂基础配方的应用表明，计算值与实测值之间的平均相对误差小于１０％。     

Deep Impact: A Large-Scale Active Experiment on a Cometary Nucleus

The Deep Impact mission will provide the first data on the interior of a cometary nucleus and a comparison of those data with data on the surface. Two spacecraft, an impactor and a flyby spacecraft, will arrive at comet 9P/Tempel 1 on 4 July 2005 to create and observe the formation and final properties of a large crater that is predicted to be approximately 30-m deep with the dimensions of a football stadium. The flyby and impactor instruments will yield images and near infrared spectra (1–5 μm) of the surface at unprecedented spatial resolutions both before and after the impact of a 350-kg spacecraft at 10.2 km/s. These data will provide unique information on the structure of the nucleus near the surface and its chemical composition. They will also used to interpret the evolutionary effects on remote sensing data and will indicate how those data can be used to better constrain conditions in the early solar system.