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.     

Energetic Hydrogen and Oxygen Atoms Observed on the Nightside of Mars

We present measurements of energetic hydrogen and oxygen atoms (ENAs) on the nightside of Mars detected by the neutral particle detector (NPD) of ASPERA-3 on Mars Express. We focus on the observations for which the field-of-view of NPD was directed at the nightside of Mars or at the region around the limb, thus monitoring the flow of ENAs towards the nightside of the planet. We derive energy spectra and total fluxes, and have compiled maps of hydrogen ENA outflow. The hydrogen ENA intensities reach 10⁵ cm⁻² sr⁻¹ s⁻¹, but no oxygen ENA signals above the detection threshold of 10⁴ cm⁻² sr⁻¹ s⁻¹ are observed. These intensities are considerably lower than most theoretical predictions. We explain the discrepancy as due to an overestimation of the charge-exchange processes in the models for which too high an exospheric density was assumed. Recent UV limb emission measurements (Galli et al., this issue) point to a hydrogen exobase density of 10¹⁰ m⁻³ and a very hot hydrogen component, whereas the models were based on a hydrogen exobase density of 10¹² m⁻³ and a temperature of 200 K predicted by Krasnopolsky and Gladstone (1996). Finally, we estimate the global atmospheric loss rate of hydrogen and oxygen due to the production of ENAs.     

非金属电热膜材料及工艺分析

本文论述了制作电热膜的工艺过程.对电热膜的材料、烧结工艺及使用寿命进行了试验,获得了有价值的结论.并论述了提高电热膜产品寿命应注意的问题.     

楔—后掠柱激波干扰流场和热流的工程算法

本文针对航天飞机机翼前缘的简化模型,即楔-后掠柱模型,在大后掠、高超声速条件下,提供了一种计算柱体前缘激波干扰流场和热流的工程计算方法。在中国科技大学流体力学实验室的激波风洞中取得了激波干扰的流场显示结果。计算的结果与国内外实验数据的比较表明,这是一种有效的方法。     

局地热源上大气边界层及其与自由大气相互作用的理论研究

本文利用二维高阶矩湍流闭合的中尺度数值模式,模拟了局地加热源上大气边界层的湍流结构,讨论了大气边界层与自由大气之间的相互作用,并由此亦使人们在海风消失时常常观测到的“风通（ｂｏｒｅ）”现象得到解释。     

铜川新区采暖期PM_(2.5)浓度与气象条件关系探究

利用铜川市新区2013年11月至2014年3月PM2.5逐时浓度和距离最近的耀县气象观测站同步气象观测资料,分析了PM2.5与环境气象条件的关系,表明本区域采暖期环境气象条件对PM2.5浓度影响显著。能见度越好、日照时间越长、气温越高,PM2.5浓度越小;风速越大、混合层高度越高,大气水平和垂直扩散能力越强,PM2.5浓度亦越小;而空气相对湿度越高、云量越多,PM2.5浓度越大。风速较大时一般混合层高度也较高,大气水平和垂直扩散能力均较强,PM2.5浓度较低。5mm以上连续性降水过程对PM2.5的净化效果明显,持续多日平均风速2.3m/s以上的较大风速过程也有很好的净化效果。2.0mm以下的单日降水在风速较小时净化效果不明显,1.0mm以下的微量降水在风速较小时还会使PM2.5浓度不降反升。     

“中青年教育研究基金”管理初探

中青年教育研究基金课题,是民航学院科研工作普遍展开的一个侧重面。简要地分析了中青年教育研究基金设立后的现状和存在的问题;重点探讨了科学选题与充分论证是提高课题申报水平和完成率的关键;提出了在加深认识的同时,应采取措施从管理上增大工作保障的力度。通过提高申报水平,加强管理,保证中青年教育研究基金课题的质量和圆满完成,使中青年教育研究基金课题走上一条健康发展的研究道路。