激波后高温高速流场中的传热特性研究

激波后高温、高速流场中的热力学与传热特性分析是直接涉及到飞行器热防护设计与传热分析的关键问题之一,借助于多组分、考虑非平衡态气体的振动以及激波与热化学非平衡态效应的守恒积分型Navier-Stokes方程组,并用高分辨率总变差减小(TVD)格式进行求解,计算与研究了Apollo工程AS-202返回舱再入地球大气层的6个飞行工况(飞行马赫数15.52～22.63)以及Huygens飞行器再入土卫六大气层的6个工况(飞行马赫数17.29～24.47),分析了不同工况下弓形脱体激波后高温高速流场的热力学与传热特性,计算得到了沿壁面的热流密度分布、温度分布以及Stanton数分布,并与国外相关飞行数据进行了比较,两者吻合较好.相关计算可以指导有关飞行器的热防护设计.      

再入滑翔式飞行器轨迹快速优化

为了满足再入滑翔飞行器轨迹实时生成的要求,提出了一种轨迹快速优化方法.在模型处理方面,根据再入飞行器运动的特点,对再入轨迹方程进行了合理的简化处理和无量纲化处理,使其更适合数值优化算法求解;在算法方面,采用乘子法对再入终端约束进行处理,然后采用共轭梯度法求解最优的再入轨迹.仿真结果表明,这样处理只需10s左右的时间便能产生一条满足约束条件的再入优化轨迹,验证了模型     

基于再入轨迹和气动热环境的返回舱烧蚀研究

针对再入全过程合理预测热防护罩表面材料烧蚀深度和温度的动态变化问题,提出融合再入轨迹、气动热以及Newton-Raphson和三对角矩阵算法（TDMA）构建动态烧蚀的方法。该方法建立直入式和跳跃式三自由度再入轨迹,应用修正的牛顿流体理论估算气动参数,以及修正的Fay-Riddell和Sutton-Grave理论计算驻点区域的热流密度,利用一维非线性热传导方程模拟了热防护材料的烧蚀过程。仿真结果表明：此方法实现了再入全过程热防护材料烧蚀深度和温度连续动态变化的预测,同样适用于更为复杂结构飞行器的动态烧蚀预测,与热平衡积分法（HBI）相比其结果可靠合理,为进一步优化热防护系统（TPS）提供了一定的参考依据。     

航天器的再入走廊及其计算方法

首先定义了航天器的再入走廊,根据提出的一种新的Loh模型与再入走廊的定义,详细地推导出了再入走廊各边界的计算公式,并证明了两种侧向走廊的数学描述是等价的。计算了以美国航天飞机为模型的再入走廊。最后还对影响再入走廊宽度的因素(如再入初始参数、飞行器升阻比、飞行器表面的耐热材料,所能忍耐的动力学环境等)作了分析。     

标准轨迹制导中准平衡滑翔条件优化研究

对于可重复使用运载器标准轨迹再入制导,准平衡滑翔条件可以将高度-速度平面内各项再入约束形成的飞行走廊,转换为倾侧角-速度空间内的倾侧角走廊.通过在倾侧角走廊内设计倾侧角曲线,可以生成满足飞行走廊的标准轨迹.通过论证标准轨迹再入制导过程中的准平衡滑翔条件及其物理意义,说明了由倾侧角走廊内的倾侧角曲线生成的标准轨迹,存在突破再入飞行走廊边界的可能性.通过对倾侧角走廊边界设置余度,极大地降低了标准轨迹突破再入飞行走廊边界的可能性,提高了标准轨迹的设计成功率.     

可重复使用运载器再入轨迹与制导控制方法综述

可重复使用运载器（RLV）是未来实现快速、可靠及廉价进出空间的必然趋势，也是当前航空航天领域的研究热点。对RLV再入段的轨迹优化、制导及控制方法进行了综述。在RLV再入轨迹优化方法上，分别从间接法、直接法以及伪谱法等方面进行了综述，在深入分析每类方法特点的基础上，对其未来发展趋势进行了展望；在RLV再入制导方法上，分别从离线标称轨迹制导、在线轨迹重构制导、预测校正制导等方面进行了综述，对每类再入制导方法进行了优缺点分析，并对未来发展方向进行了总结；在RLV再入姿态控制方法上，分别从线性控制方法、非线性控制方法、智能控制方法等方面对其进行了综述，并对其特点和未来发展趋势进行了分析。最后，对RLV再入制导控制一体化方法进行了综述，指出了未来RLV制导控制一体化研究中亟需解决的关键问题。     

飞船再入制导研究

在配平迎角飞行的合理假设下，建立了描述载人飞船再入飞行段弹道的数学仿真模型。在飞船再入标准轨道设计和再入机动边界计算的基础上，研究了基于标准轨道法的飞船再入飞行制导规律。六自由度飞行弹道的数学仿真证明，设计的制导律能满足飞船再入飞行制导和定点着陆的要求，同时还得到了飞船再入飞行的某些运动规律和一些有益的结论。     

欧洲无翼飞船的再入,降落和着陆技术及验证

取消了欧洲有翼载人航天运输系统“赫尔梅斯”计划之后，研究了多种可能的无翼再入飞船方案，用于人员运输，空间站人员救援以及后勤补给任务，悦船结构的复杂性必须在先进性和可能性之间平衡。在欧洲飞船设计中遇到的一项挑战是要求在欧洲大陆精密着陆。本文介绍了无翼再入飞船再入，降落和着陆综合方案的策略。     

充气式再入飞行器柔性热防护系统的发展状况

讨论了充气式再入飞行器对柔性热防护系统的具体要求，归纳了柔性热防护系统设计的一般准则。概述了柔性热防护系统在充气式再入飞行器中的应用现状，并指出在多层隔热毡(MLI)外表敷设耐高温涂层是柔性热防护系统的理想方案。介绍了柔性热防护系统的材料技术，指出轻质、柔性和耐高温是柔性热防护材料的主要特征，并建议在充气式再入飞行器的总体设计过程中采用Nextel312作为主要候选材料来完成相应的热防护设计。     

载人飞船返回舱的再入气动环境

本文介绍了载人飞船返回舱的再入走廊和气动环境。为了确定返回舱的自由流条件和驻我条件，其再入轨迹和再入走廊是十分重要的。     

The Characterisation of Titan's Atmospheric Physical Properties by the Huygens Atmospheric Structure Instrument (Hasi)

The Huygens Atmospheric Structure Instrument (HASI) is a multi-sensor package which has been designed to measure the physical quantities characterising the atmosphere of Titan during the Huygens probe descent on Titan and at the surface. HASI sensors are devoted to the study of Titan's atmospheric structure and electric properties, and to provide information on its surface, whether solid or liquid. This revised version was published online in August 2006 with corrections to the Cover Date.     

The Huygens Probe System Design

Space Science Reviews - The Huygens Probe is the ESA-provided element of the joint NASA/ESA Cassini/Huygens mission to Saturn and its largest moon Titan. Huygens is an entry probe designed to enter...     

The Huygens Doppler Wind Experiment ' Titan Winds Derived from Probe Radio Frequency Measurements

A Doppler Wind Experiment (DWE) will be performed during the Titan atmospheric descent of the ESA Huygens Probe. The direction and strength of Titan's zonal winds will be determined with an accuracy better than 1 m s⁻¹ from the start of mission at an altitude of ∼160 km down to the surface. The Probe's wind-induced horizontal motion will be derived from the residual Doppler shift of its S-band radio link to the Cassini Orbiter, corrected for all known orbit and propagation effects. It is also planned to record the frequency of the Probe signal using large ground-based antennas, thereby providing an additional component of the horizontal drift. In addition to the winds, DWE will obtain valuable information on the rotation, parachute swing and atmospheric buffeting of the Huygens Probe, as well as its position and attitude after Titan touchdown. The DWE measurement strategy relies on experimenter-supplied Ultra-Stable Oscillators to generate the transmitted signal from the Probe and to extract the frequency of the received signal on the Orbiter. Results of the first in-flight checkout, as well as the DWE Doppler calibrations conducted with simulated Huygens signals uplinked from ground (Probe Relay Tests), are described. Ongoing efforts to measure and model Titan's winds using various Earth-based techniques are briefly reviewed. This revised version was published online in August 2006 with corrections to the Cover Date.     

Huygens' Surface Science Package

The design and performance of the Surface Science Package (SSP) on the Huygens probe are discussed. This instrument consists of nine separate sensors that are designed to measure a wide range of physical properties of Titan's lower atmosphere, surface, and sub-surface. By measuring a number of physical properties of the surface it is expected that the SSP will be able to constrain the inferred composition and structure of the moon's near-surface environment. Although the SSP is primarily designed to sense properties of the surface, some of its sensors will also make measurements of the atmosphere along the probe's entry path and will complement the data gathered by other experiments on the Huygens probe. This revised version was published online in August 2006 with corrections to the Cover Date.     

To the surface of Mars via Titan: : Reuse of Huygens software components on Beagle 2

‘Beagle 2’ is a Mars lander, which will be flown in 2003 as part of ESA's Mars Express mission. Like the Huygens probe to Titan, it is critically dependent on the correct functioning of on-board software to control its descent. Beagle 2 is a much lower cost mission and cannot afford to develop all of its software from scratch. How has the Huygens software been given a new lease of life on-board Beagle 2?     

Touring the saturnian system: the atmospheres of titan and saturn

This report follows the presentation originally given in the ESA Phase A Study for the Cassini Huygens Mission. The combination of the Huygens atmospheric probe into Titan's atmosphere with the Cassini orbiter allows for both in-situ and remote-sensing observations of Titan. This not only provides a rich harvest of data about Saturn's famous satellite but will permit a useful calibration of the remote-sensing instruments which will also be used on Saturn itself. Composition, thermal structure, dynamics, aeronomy, magnetosphere interactions and origins will all be investigated for the two atmospheres, and the spacecraft will also deliver information on the interiors of both Titan and Saturn. As the surface of Titan is intimately linked with the atmosphere, we also discuss some of the surface studies that will be carried out by both probe and orbiter. This revised version was published online in August 2006 with corrections to the Cover Date.     

Geology of the Icy Satellites

In the last 25 years, the explorations of the Voyager and Galileo missions have resulted in an entirely new view of the icy worlds orbiting the giant outer planets. These objects show a huge diversity in their characteristics, resulting from their formation histories, internal processes and interactions with their space environments. This paper will review the current state of knowledge about the icy satellites and discuss the exciting prospects for the upcoming Cassini/Huygens mission as it begins a new era of exploration of the Saturn satellite system.