Interior Evolution of Mercury

The interior evolution of Mercury—the innermost planet in the solar system, with its exceptional high density—is poorly known. Our current knowledge of Mercury is based on observations from Mariner 10’s three flybys. That knowledge includes the important discoveries of a weak, active magnetic field and a system of lobate scarps that suggests limited radial contraction of the planet during the last 4 billion years. We review existing models of Mercury’s interior evolution and further present new 2D and 3D convection models that consider both a strongly temperature-dependent viscosity and core cooling. These studies provide a framework for understanding the basic characteristics of the planet’s internal evolution as well as the role of the amount and distribution of radiogenic heat production, mantle viscosity, and sulfur content of the core have had on the history of Mercury’s interior. The existence of a dynamo-generated magnetic field suggests a growing inner core, as model calculations show that a thermally driven dynamo for Mercury is unlikely. Thermal evolution models suggest a range of possible upper limits for the sulfur content in the core. For large sulfur contents the model cores would be entirely fluid. The observation of limited planetary contraction (∼1–2 km)—if confirmed by future missions—may provide a lower limit for the core sulfur content. For smaller sulfur contents, the planetary contraction obtained after the end of the heavy bombardment due to inner core growth is larger than the observed value. Due to the present poor knowledge of various parameters, for example, the mantle rheology, the thermal conductivity of mantle and crust, and the amount and distribution of radiogenic heat production, it is not possible to constrain the core sulfur content nor the present state of the mantle. Therefore, it is difficult to robustly predict whether or not the mantle is conductive or in the convective regime. For instance, in the case of very inefficient planetary cooling—for example, as a consequence of a strong thermal insulation by a low conductivity crust and a stiff Newtonian mantle rheology—the predicted sulfur content can be as low as 1 wt% to match current estimates of planetary contraction, making deep mantle convection likely. Efficient cooling—for example, caused by the growth of a crust strongly in enriched in radiogenic elements—requires more than 6.5 wt% S. These latter models also predict a transition from a convective to a conductive mantle during the planet’s history. Data from future missions to Mercury will aid considerably our understanding of the evolution of its interior.     

低温加压条件下EVA手套的力量分析

为了研究航天员舱外活动时的手套压力和太空低温复合效应对操作力量的影响,选取最大握力和握力疲劳两个指标评价手动作业力量,其中握力疲劳采用做功能力评价.操作力量抓握试验所需的不同温度和压力是通过在低温模拟舱中利用液氮降温以及真空泵抽气实现.结果表明:戴手套对最大握力和握力疲劳的影响都非常显著;与常温常压戴手套相比,压力(29.6 kPa,39.2 kPa)单独作用对最大握力的影响显著,低温单独作用对最大握力的影响并不显著,而二者对握力疲劳的影响都非常显著;在加压和低温复合作用下,最大握力和握力疲劳会进一步受到显著影响.可见手套压力和太空低温复合效应严重降低了航天员手部力量的发挥,航天员舱外作业人-手套系统的研究需考虑复合因素的影响.     

基于细胞吸引子选择机制的网络选择算法

随着无线通信技术的发展,物联网、车联网和体联网等同类型的无线网络之间共存、相互补充和异构融合。任何单一的通信技术不能完全满足人们对网络服务的多样化需求。如何在移动过程中选择可靠高效的网络连接成为学术和工业界的研究热点。基于细胞吸引子选择模型,提出了一种面向群体终端网络选择的决策方法,并通过车联网环境数值实验比较了该生物启发式决策方法与基于效用函数方法的性能,结果表明:基于细胞吸引子选择机制的生物启发式决策方法在网络选择决策中具有较好的性能。      

磁场影响葡萄糖氧化酶活性的研究

以尼龙网作载体，用戊二醛交联将区区糖氧化酶（ＧＯＤ）固定装成酶柱并联结于流动体系中，采用流动注射分光光度法研究磁场对固定化ＧＯＤ催化活性的影响。结果表明，在０℃、５℃、４５℃下以１．０×１０＾－２ｍｏｌ．Ｌ＾－１的葡萄糖为底物及５５℃下以０．１ｍｏｌ＾－１的葡萄糖为底物时，０．２２Ｔ静有显著提高固定化ＧＯＤ的反应速度，且磁场效应与底物浓度及磁场作用时间有关。用动力学方法考察了不同强度的磁场对溶解Ｇ     

电液伺服加载的神经网络内部反馈控制

 针对电液伺服加载系统多余力问题,提出了一种反馈加载系统内部力差信号减少多余力的控制方法。为了消除液压非线性及参数变化等影响,进一步提出基于神经网络内部参考模型调节方法。该参考模型为无舵机扰动时的液压油缸负载压力方程,在加载过程中,将油缸的负载压力与参考模型输出比较,利用神经网络自适应调节能力,消除加载中舵机运动的速度和加速度干扰,同时也克服液压系统非线性,时变参数和扰动的影响,该方法有较好的适用性。     

KM6水平舱改造测控系统研制

宇航员出舱活动是我国载人航天发展战略的第二步——空间实验室工程的一项基本任务。为满足完成“SZ-7人-船-服”出舱活动联合试验任务的需要,必须需要对原有KM6水平舱进行适应性的功能改造。为了确保宇航员的生命安全,必须尽可能的提高整个控制系统的可靠性,。测控系统在总体结构上采用SIEMENS PCS7冗余集散控制系统的方式,对所有关键测控环节（包括控制计算机、CPU、电源、网络、I/O模块等）都进行了冗余备份,以确保宇航员出舱活动试验流程的顺利进行,并对重要操作中关键参数互联、互锁,杜绝误操作,确保有完善的系统监控和故障报警功能,。改造后通过多次调试和多种试验模式演练,各分系统和总控系统测控功能均达到设计指标要求。为人-舱-服联合试验提供了坚强的后盾。     

550～600 km高度上热层大气密度的中长期变化

选用了2005年8月20日至2006年7月28日高度550～600 km附近的热层大气密度探测数据,对表征太阳活动的F10.7值和表征地磁活动强度的Ap指数进行了相关特性的统计.分析结果表明,在无明显地磁扰动时热层大气密度日平均值的涨落呈现27日和准半年的周期性变化,但在地磁扰动期间这种变化的周期性会被削弱,且大气密度的周日变化幅度与F10.7值呈正相关关系.      

日地L5太阳探测工程概述

南京大学联合中国气象局、上海航天技术研究院等单位共同建议的日地L5太阳探测工程——“羲和二号”,将在国际上首次发射一颗人造探测器至日地系统第5个拉格朗日点,通过精测矢量磁场、揭示三维爆发和精准预警预报,解答“活动区磁场的产生演化及其与太阳爆发的物理联系”和“太阳爆发的传播规律及其与灾害性空间天气的关系”这2个太阳物理和空间天气领域亟待解决的重大科学和应用问题。本文重点阐述“羲和二号”的科学与应用目标,简要介绍其科学载荷和初步方案。联合日地连线方向上的太阳探测,“羲和二号”的实施将开启我国太阳立体探测时代,拓展人类对太阳爆发机制的理解,为空间天气预警预报带来革命性突破。     

The longitudinal and hemispherical variation of the IRI’s foF2 estimates at ±40° dip angle around 95°E and 130°E sector under fluctuating solar flux conditions

The deviation of the IRI estimates of the monthly mean foF2 in the low mid latitude of 95°E–130°E longitude sector is investigated using simultaneous ground measurements at four stations during 2010–2014. The stations form two conjugate pairs of the same geo-magnetic latitude at two fixed longitudes enabling direct longitudinal and hemispheric comparison. The temporal, spatial, seasonal and solar activity variations of the deviations are discussed with reference to the longitudinal density variation in the transition region between low and midlatitudes. Cases of underestimation/overestimation as well as good estimate are noted. Underestimation (overestimation) in the daytime and overestimation (underestimation) in the nighttime of 95°E (130°E) are common. The longitudinal difference in the measurements suggests negative (positive) foF2 gradient from west to east in daytime (nighttime). In contrast, the IRI predicts flatter or increasing longitudinal profiles from 95°E to 130°E. The local time and longitudinal variation of the IRI deviations can be attributed to the combined role of the longitudinal EIA structure as well as midlatitude zonal wind-magnetic declination effect. The station/season independent deviations relate the role of solar activity representation in the IRI. These deviations may be attributed to the weak IRI response to rapid solar flux fluctuations.