RBCC-RKT两级入轨飞行器起飞质量估算方法

针对液体火箭发动机真空比冲基本不变,火箭基循环组合发动机(RBCC)比冲随着飞行条件不断变化的特点,提出了将增广拉格朗日遗传算法优化第一级飞行弹道与传统液体火箭质量估算方法估算第二级起飞质量相结合,获得水平起飞两级入轨RBCC-RKT飞行器第一级起飞质量的估算方法,为总体方案初步设计论证提供参考.通过算例,分析了一级RBCC飞行器惰性质量比、最高动压,气动特性与起飞质量之间的关系.计算表明,降低RBCC飞行器惰性质量比、提高一级飞行器最大飞行动压、提高飞行器升阻比,都能有效地降低一级起飞质量.     

Multi-scale reconnections in a complex CME

A series of three flares of GOES class M, M and C, and a CME were observed on 20 January 2004 occurring in close succession in NOAA 10540. Types II, III, and N radio bursts were associated. We use the combined observations from TRACE, EIT, Hα images from Kwasan Observatory, MDI magnetograms, GOES, and radio observations from Culgoora and Wind/ WAVES to understand the complex development of this event. We reach three main conclusions. First, we link the first two impulsive flares to tether-cutting reconnections and the launch of the CME. This complex observation shows that impulsive quadrupolar flares can be eruptive. Second, we relate the last of the flares, an LDE, to the relaxation phase following forced reconnections between the erupting flux rope and neighbouring magnetic field lines, when reconnection reverses and restores some of the pre-eruption magnetic connectivities. Finally, we show that reconnection with the magnetic structure of a previous CME launched about 8 h earlier injects electrons into open field lines having a local dip and apex (located at about six solar radii height). This is observed as an N-burst at decametre radio wavelengths. The dipped shape of these field lines is due to large-scale magnetic reconnection between expanding magnetic loops and open field lines of a neighbouring streamer. This particular situation explains why this is the first N-burst ever observed at long radio wavelengths.     

对接仿真试验台杠铃式质量惯量模拟技术研究

针对地面航天器对接动力学全物理仿真试验台,提出采用质量惯量模拟技术模拟航天器的质量、惯量特性,以便灵活的适应不同吨位航天器对接试验。设计了杠铃式质量惯量模拟结构。介绍了杠铃式模拟件的结构特点,确定调整参数,调整范围,对模拟误差进行了分析。结果表明杠铃式质量惯量模拟件模拟准确,调整简单、方便。     

In-Situ Solar Wind and Magnetic Field Signatures of Interplanetary Coronal Mass Ejections

The heliospheric counterparts of coronal mass ejections (CMEs) at the Sun, interplanetary coronal mass ejections (ICMEs), can be identified in situ based on a number of magnetic field, plasma, compositional and energetic particle signatures as well as combinations thereof. We summarize these signatures and their implications for understanding the nature of these structures and the physical properties of coronal mass ejections. We conclude that our understanding of ICMEs is far from complete and formulate several challenges that, if addressed, would substantially improve our knowledge of the relationship between CMEs at the Sun and in the heliosphere.     

Solar Wind Sources and Their Variations Over the Solar Cycle

In this paper I will briefly summarize the present status of our knowledge on the four different sorts of solar wind, their sources and their short- and long-term variations. First: the fast solar wind in high-speed streams that emerges from coronal hole regions. Second: the slow solar wind emerging from the non-active Sun near the global heliospheric current sheet above helmet streamers and underlying active regions. Third: the slow solar wind filling most of the heliosphere during high solar activity, emerging above active regions in a highly turbulent state, and fourth: the plasma expelled from the Sun during coronal mass ejections. The coronal sources of these different flows vary dramatically with the solar activity cycle.     

Two energy release processes for CMEs: MHD catastrophe and magnetic reconnection

It remains an open question how magnetic energy is rapidly released in the solar corona so as to create solar explosions such as solar flares and coronal mass ejections (CMEs). Recent studies have confirmed that a system consisting of a flux rope embedded in a background field exhibits a catastrophic behavior, and the energy threshold at the catastrophic point may exceed the associated open field energy. The accumulated free energy in the corona is abruptly released when the catastrophe takes place, and it probably serves as the main means of energy release for CMEs at least in the initial phase. Such a release proceeds via an ideal MHD process in contrast with nonideal ones such as magnetic reconnection. The catastrophe results in a sudden formation of electric current sheets, which naturally provide proper sites for fast magnetic reconnection. The reconnection may be identified with a solar flare associated with the CME on one hand, and produces a further acceleration of the CME on the other. On this basis, several preliminary suggestions are made for future observational investigations, especially with the proposed Kuafa satellites, on the roles of the MHD catastrophe and magnetic reconnection in the magnetic energy release associated with CMEs and flares.     

稠密气固两相流颗粒质量流量测量方法研究

为解决粉末火箭发动机和粉末冲压发动机供粉系统冷流标定过程中颗粒质量流量的测量问题,提出了一种稠密气固两相流中颗粒质量流量的测量方法,并基于旋风分离器和电子天平运用该方法设计了一套气固两相流中固体质量流量的测量装置,同时运用粉末火箭发动机的供粉系统对该测量方法和装置的测试性能进行了实验验证研究。结果表明:测量装置的粉末收集效率可高达98.5%以上,为固体颗粒的质量流量测量提供了保障;测量方法具有较好的可靠性和测量精度,其测量结果相对误差低于3%;测量方法具有较好的测量稳定性,重复性实验中测量结果相对误差低于2%;通过改变旋风分离器结构设计等参数,可拓宽测量方法的适用范围。     

跨介质运动物体的附加质量

跨介质运动物体具备能够适应多种流体介质环境的突出优势,但由于受自由面及流体影响,力学环境复杂,其运动特性难以预测。附加质量法是工程上解决物体与流体耦合问题的常用方法,但现有的附加质量结论无法直接推广到带自由面问题的跨介质过程。针对跨介质过程的时变附加质量问题,提出了一种新的求解方法,研究了不同浸深时某柱体外形跨介质过程中出水阶段和入水阶段的附加质量变化规律。结论表明:出水阶段和入水阶段的附加质量随浸深的变化趋势一致,曲线相似;相同浸深状态时出水阶段和入水阶段的法向附加质量相近,线性特征明显;相同浸深状态时出水阶段和入水阶段的轴向附加质量、附加转动惯量和附加静距差距明显,2个过程不可逆。本文所提出的方法可为各类跨介质结构体设计提供技术支持,也可推广至其他带自由面问题的附加质量求解中。      

Flux emergence,flux imbalance,magnetic free energy and solar flares

Emergence of complex magnetic flux in the solar active regions lead to several observational effects such as a change in sunspot area and flux embalance in photospheric magnetograms. The flux emergence also results in twisted magnetic field lines that add to free energy content. The magnetic field configuration of these active regions relax to near potential-field configuration after energy release through solar flares and coronal mass ejections. In this paper, we study the relation of flare productivity of active regions with their evolution of magnetic flux emergence, flux imbalance and free energy content. We use the sunspot area and number for flux emergence study as they contain most of the concentrated magnetic flux in the active region. The magnetic flux imbalance and the free energy are estimated using the HMI/SDO magnetograms and Virial theorem method. We find that the active regions that undergo large changes in sunspot area are most flare productive. The active regions become flary when the free energy content exceeds 50% of the total energy. Although, the flary active regions show magnetic flux imbalance, it is hard to predict flare activity based on this parameter alone.     

Solar energetic particle events during the rise phases of solar cycles 23 and 24

We present a comparative study of the properties of coronal mass ejections (CMEs) and flares associated with the solar energetic particle (SEP) events in the rising phases of solar cycles (SC) 23 (1996–1998) (22 events) and 24 (2009–2011) (20 events), which are associated with type II radio bursts. Based on the SEP intensity, we divided the events into three categories, i.e. weak (intensity < 1 pfu), minor (1 pfu < intensity < 10 pfu) and major (intensity ? 10 pfu) events. We used the GOES data for the minor and major SEP events and SOHO/ERNE data for the weak SEP event. We examine the correlation of SEP intensity with flare size and CME properties. We find that most of the major SEP events are associated with halo or partial halo CMEs originating close to the sun center and western-hemisphere. The fraction of halo CMEs in SC 24 is larger than the SC 23. For the minor SEP events one event in SC23 and one event in SC24 have widths < 120° and all other events are associated with halo or partial halo CMEs as in the case of major SEP events. In case of weak SEP events, majority (more than 60%) of events are associated with CME width < 120°. For both the SC the average CMEs speeds are similar. For major SEP events, average CME speeds are higher in comparison to minor and weak events. The SEP event intensity and GOES X-ray flare size are poorly correlated. During the rise phase of solar cycle 23 and 24, we find north–south asymmetry in the SEP event source locations: in cycle 23 most sources are located in the south, whereas during cycle 24 most sources are located in the north. This result is consistent with the asymmetry found with sunspot area and intense flares.