A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.     

Galactic Wind: Mass Fractionation and Cosmic Ray Acceleration

The dynamical and chemical effects of the Galactic Wind are discussed. This wind is primarily driven by the pressure gradient of the Cosmic Rays. Assuming the latter to be accelerated in the Supernova Remnants of the disk which at the same time produce the Hot Interstellar Medium, it is argued that the gas removed by the wind is enriched in the nucleosynthesis products of Supernova explosions. Therefore the moderate mass loss through this wind should still be able to remove a substantial amount of metals, opening the way for stars to produce more metals than observed in the disk, by e.g. assuming a Salpeter-type stellar initial mass function beyond a few Solar masses. The wind also allows a global, physically appealing interpretation of Cosmic Ray propagation and escape from the Galaxy. In addition the spiral structure of the disk induces periodic pressure waves in the expanding wind that become a sawtooth shock wave train at large distances which can re-accelerate “knee” particles coming from the disk sources. This new Galactic Cosmic Ray component can reach energies of a few×10¹⁸ eV and may contribute to the juncture between the particles of Galactic and extragalactic origin in the observed overall Cosmic Ray spectrum.     

基于模块的飞机产品结构管理研究

飞机研发是一项大型的系统性工程,传统的飞机产品结构由于零组件数据集包含有二维图纸、三维模型、临时更改单等大量文档且更改较频繁,同时制造、维修等部门在工程数据重构中存在工作量大和转换易脱节等特点,导致产品数据管理异常复杂和困难,效率也较低。为了简化飞机产品结构管理方式,在借鉴国际主流飞机制造商经验的基础上,通过结合模块化理论和全三维设计手段。以某一型号的民用飞机为例,重点从产品结构的组织模式、数据集的构成、产品数据的更改规则对该管理方案进行了阐述。从而保证了构型数据管理的便捷性和准确性,也符合未来飞机产品研发全数字化的发展方向。     

大涵道比涡扇发动机循环参数优化算法研究及应用

针对多约束条件与多优化变量的大涵道比涡扇发动机循环参数优化问题,提出了自适应三次变异差分进化算法,运用多个Benchmarks多峰函数对算法进行验证,并将该算法与大涵道比涡扇发动机性能计算程序相结合,对多约束条件下的循环参数进行了优化.计算结果表明:自适应三次变异差分进化算法比传统差分进化算法收敛精度更高、收敛速度更快,大幅度提高了大涵道比涡扇发动机循环参数优化效果,适合解决大涵道比涡扇发动机循环参数优化问题.      

基于SPN的跑道利用率模型分析与研究

采用随机Petri网(SPN)建立了跑道系统运行约束方程;通过构造同构马尔科夫链建立了系统处于各种状态时的稳态概率表达式;改变变迁的触发速率,分析跑道利用率的变化情况。证明了模型的可达性、有界性,且不存在死点。     

基于自适应差分进化算法的变循环发动机模型求解方法研究

为了降低传统迭代算法在求解变循环发动机非线性模型时对初值的依赖性,将模型的求解问题转换为求最小值的优化问题,引入差分进化算法进行模型的求解,并提出一种自适应差分进化算法(ADE)。ADE借助轮盘赌选择法,利用种群的进化经验可以自适应的选择最适合当前种群的差分策略与算法控制参数。针对变循环发动机四个典型工作点的模型求解问题,研究了标准差分进化算法(SDE)的控制参数对其性能的影响,获取了SDE在求解四个典型工作点时的最优控制参数组合,对比分析了ADE与SDE的性能差异,最后研究了种群规模对ADE性能的影响。结果表明：SDE在求解发动机模型时具有较好的鲁棒性,在求解不同工作点时算法的最优控制参数并不完全相同;相比于使用最优控制参数的SDE,ADE可以在不影响算法鲁棒性的情况下提升效率50%以上;减少ADE的种群规模会在提升算法效率的同时破坏鲁棒性。     

可压缩多介质流动问题的高精度数值模拟方法

在可压缩流动问题的数值模拟领域,激波的高分辨率计算已取得重要进展.但是包含物质界面的可压缩多介质流动的数值模拟还存在诸多数值挑战,主要表现为界面处数值耗散过大和非物理振荡等问题.界面处流体性质的不连续性是造成可压缩多介质流动问题物理建模与数值方法困难的主要原因.为了建立一套高效的可压缩多介质流动问题的高精度数值模拟方案...     

高温吸波涂层的多目标优化模型设计

大多数高温吸波材料都属于非磁损耗型,单层往往很难达到理想的吸波性能.为解决此问题并优化涂层厚度,通过差分进化算法建立了多层高温吸波涂层的多目标优化模型,重点以8.2～12.4 GHz内反射率RL＜-10 dB频率带宽和涂层总厚度d为优化目标.设定三种高温吸波材料,研究表明,单层涂层很难达到理想的吸波性能;在单目标优化中...     

变循环发动机模态转换建模及控制规律设计方法研究

为了实现变循环发动机快速可靠的模态转换,本文发展了变循环发动机模态转换过渡态模型及控制规律设计方法。在变循环发动机动态数值仿真程序的基础上,针对模态选择阀与涵道引射器这两个模态转换过程中的关键变几何部件,建立了高精度的气流突扩局部损失模型。首次提出了可考虑模态选择阀堵塞对发动机性能影响的模态选择阀堵塞模型,消除了由于模型不精确造成的模态转换参数波动。在建立的变循环发动机数学模型的基础上,提出了基于直接推力控制技术的模态转换控制规律设计方法,考虑了变循环发动机的8个可调参数,采用差分进化算法对模态转换过程进行了优化。结果表明,本文提出的模态转换控制规律设计方法可以实现变循环发动机快速平稳的模态转换,双外涵转单外涵的参数变化规律与单外涵转双外涵的参数变化规律基本类似,推力在0.6秒就稳定在目标推力值,其余参数大多在1.4秒之后才趋于稳定。本文提出的变循环发动机模态转换控制规律设计方法还可应用于常规航空发动机的加/减速过渡态控制规律设计中。     

基于产品结构的飞机客户化管理研究

航空公司因市场定位、品牌建设、拟飞航线和所选设备不同,导致客户对不同架次或批次商用飞机的 客户化需求存在较大差异,因此灵活高效的客户化管理是实现客户飞机有效构型配置的第一个关键步骤,也是 飞机采购合同签署的基础。提出一种基于产品结构的需求管理方案,构建三层数据管理结构和各种表单对客 户需求进行全流程管控,对某型号飞机信息系统开发的案例进行分析。该管理方案能够支撑不同航空公司客 户化构型的定义,保证客户需求传递的便捷性和实现的准确性,符合产品全寿命周期管理的发展需求。