Cosmic ray impact on extrasolar earth-like planets in close-in habitable zones

Because of their different origins, cosmic rays can be subdivided into galactic cosmic rays and solar/stellar cosmic rays. The flux of cosmic rays to planetary surfaces is mainly determined by two planetary parameters: the atmospheric density and the strength of the internal magnetic moment. If a planet exhibits an extended magnetosphere, its surface will be protected from high-energy cosmic ray particles. We show that close-in extrasolar planets in the habitable zone of M stars are synchronously rotating with their host star because of the tidal interaction. For gravitationally locked planets the rotation period is equal to the orbital period, which is much longer than the rotation period expected for planets not subject to tidal locking. This results in a relatively small magnetic moment. We found that an Earth-like extrasolar planet, tidally locked in an orbit of 0.2 AU around an M star of 0.5 solar masses, has a rotation rate of 2% of that of the Earth. This results in a magnetic moment of less than 15% of the Earth's current magnetic moment. Therefore, close-in extrasolar planets seem not to be protected by extended Earth-like magnetospheres, and cosmic rays can reach almost the whole surface area of the upper atmosphere. Primary cosmic ray particles that interact with the atmosphere generate secondary energetic particles, a so-called cosmic ray shower. Some of the secondary particles can reach the surface of terrestrial planets when the surface pressure of the atmosphere is on the order of 1 bar or less. We propose that, depending on atmospheric pressure, biological systems on the surface of Earth-like extrasolar planets at close-in orbital distances can be strongly influenced by secondary cosmic rays.     

Venus, Mars, and the ices on Mercury and the moon: astrobiological implications and proposed mission designs

Venus and Mars likely had liquid water bodies on their surface early in the Solar System history. The surfaces of Venus and Mars are presently not a suitable habitat for life, but reservoirs of liquid water remain in the atmosphere of Venus and the subsurface of Mars, and with it also the possibility of microbial life. Microbial organisms may have adapted to live in these ecological niches by the evolutionary force of directional selection. Missions to our neighboring planets should therefore be planned to explore these potentially life-containing refuges and return samples for analysis. Sample return missions should also include ice samples from Mercury and the Moon, which may contain information about the biogenic material that catalyzed the early evolution of life on Earth (or elsewhere). To obtain such information, science-driven exploration is necessary through varying degrees of mission operation autonomy. A hierarchical mission design is envisioned that includes spaceborne (orbital), atmosphere (airborne), surface (mobile such as rover and stationary such as lander or sensor), and subsurface (e.g., ground-penetrating radar, drilling, etc.) agents working in concert to allow for sufficient mission safety and redundancy, to perform extensive and challenging reconnaissance, and to lead to a thorough search for evidence of life and habitability.     

法向发身率测量仪

本文给出了在大气温度下测量物质表面法向发射率的原理、装置结构及测试结果。这个装置是由黑体,样品腔和辐射计(接收元件)构成。法向发射率是由在相同温度下样品产生的热电势EMF与黑体产生的热电势EMFo之比来度量的。最后,对误差进行了讨论。     

大间隙高强度胶粘剂在粘接石英陶瓷与低膨胀合金中的应用

论述了使用硅凝胶粘接石英陶瓷材料与低膨胀合金，并通过采取减小内应力的方法，以使其能提高强度且耐高温。结果表明：在石英陶瓷与低膨胀合金的粘接过程中，该硅凝胶涂布方便。在常温下，压剪强度为5．18MPa；在200℃的高温下，保温5min，压剪强度仍可达3．22MPa。它的强度及耐高温性能完全符合应用要求。     

小型空天飞行器制导导航与控制系统方案

针对地面垂直发射、可长时间在轨运行和轨道机动、再入稠密大气层并水平着陆在机场跑道上的小型空天飞行器,研究其制导导航与控制系统方案.分析其在轨运行、离轨、再入、末端能量管理、自主进场着陆、地面滑跑等各阶段的制导、导航与控制系统任务需求,根据任务需求提出相应的制导导航与控制系统组成方案,并阐述制导导航与控制系统的工作原理.理论分析结果表明,提出的制导导航与控制系统方案满足飞行器各阶段的任务需求,合理可行.     

利用非GEO卫星进行地面站时间同步研究

根据地球静止轨道（GEO）卫星转发同步信号的双向时间比对法实现站间时间同步的基本原理,提出了利用拟合非GEO卫星转发信号的伪距实现时间同步的新方法。拟合伪距法消除了传播路径延迟和只能使用GEO卫星作为信号转发器的限制,扩大了双向时间比对的应用范围。仿真结果表明：该法有较高的精度,满足工程要求。     

Astrobiology through the ages of Mars: the study of terrestrial analogues to understand the habitability of Mars

Mars has undergone three main climatic stages throughout its geological history, beginning with a water-rich epoch, followed by a cold and semi-arid era, and transitioning into present-day arid and very cold desert conditions. These global climatic eras also represent three different stages of planetary habitability: an early, potentially habitable stage when the basic requisites for life as we know it were present (liquid water and energy); an intermediate extreme stage, when liquid solutions became scarce or very challenging for life; and the most recent stage during which conditions on the surface have been largely uninhabitable, except perhaps in some isolated niches. Our understanding of the evolution of Mars is now sufficient to assign specific terrestrial environments to each of these periods. Through the study of Mars terrestrial analogues, we have assessed and constrained the habitability conditions for each of these stages, the geochemistry of the surface, and the likelihood for the preservation of organic and inorganic biosignatures. The study of these analog environments provides important information to better understand past and current mission results as well as to support the design and selection of instruments and the planning for future exploratory missions to Mars.