整体级发动机用含硼BAMO／THF推进剂的探索研究

采用最小自由能法（ｗｈｉｔｅ法），计算研究了增塑剂与粘合剂质量比（Ｐ１、Ｐ０）、固体含量、硼含量、ＨＭＸ含量对用于整体级发动机的含硼ＢＡＭＯ／ＴＨＦ（１：１）推进剂能量的影响。实验研究制得的６５％固体含量的ＢＡＭＯ／ＴＨＦ（１：１）含硼固体推进剂的基础燃速、压强指数较低；φ６５ｍｍ发动机的试车结果表明：实验制得的６５％固体含量的含硼ＢＡＭＯ／ＴＨＦ（１：１）推进剂的比冲效率为８４．４５％。     

喷气推进系统的用能分析

应用工程热力学中技术功的概念和exergy分析的方法，以简单涡轮喷气推进系统为例，用一种新的观点对这类移动的开口系统进行了用能效率的分析。所得到的能流图和exeryy流图能够非常清晰地显示出系统各个部件中能量转化的情况，为部件性能的改进和整个系统效率的提高提供了有用的信息。这种分析方法摆脱了传统的脱离实际的循环分析，能够方便地处理诸如内外函发动机以及火箭发动机等各种复杂循环的系统。exergy分析能够更清楚地显示不可逆损失在各部件中的分配，从而更明确地指示改进的方向。     

含新型含能材料的 XLDB 推进剂能量及特征信号的预估

通过几种新型含能材料及常规材料对固体推进剂能量性能和特征信号影响的对比、分析,预估了几种新型高能量密度材料的应用前景。     

稳态等离子体推力器低功率工作模式实验研究

稳态等离子体动力器（SPT）是技术性能和空间适应性良好的电推力器,是小卫星空间动力的理想选择。从实验的角度研究了额定功率为660W的SPT在低于其额定功率下运行,推力器的放电特性、推车特性、推力效率、比冲等性能随推力器工作参数的变化。实验结果表明：660W的SPT推力器在低于其额定功率下工作,具有稳定的放电特性和确定的推力性能,可以将较大尺寸的SPT推力器在低功率模式下运行来替代小尺寸SPT推力器的作用。     

高能推进剂燃烧效率研究和实测比冲预估

采用燃烧残渣中活性铝含量分析、真空爆热和发动机试验等方法，研究了高能推进剂中主要组分对推进剂燃烧效率的影响。研究结果表明：增塑剂的种类和含量是影响效率的主要因素，AP的含量及固体组分的粒度级配也有明显影响；BSF－φ315发动机试车结果证明高能推进剂的的实测比冲效率大于0．94。采用软件计算发动机的实测比中，可预估高能推进剂配方在不同压强及燃速条件下标准试验发动机（BSF－φ165和BSF－φ315）试车的实测比冲值。     

Interplanetary Physics Research in China： 2006-2008

This brief report summarized the latest advances of the interplanetary physics research in China during the period of 2006-2007,made independently by Chinese space physicists and through international collaboration.The report covers all aspects of the interplanetary physics,including theoretical studies,numerical simulation and data analysis.     

Relativistic solar protons in the ground level event of 23 February 1956: New study

In this study we applied again to the outstanding solar particle event of 23 February 1956, the largest one in the entire history of observations of solar cosmic rays. Due to significant improvement of the analysis/modeling techniques and new understanding of physical processes in the solar atmosphere and interplanetary space, a possibility arises to interpret the old data in the light of modern concept of multiple particle acceleration at/near the Sun. In our new analysis the data of available then neutron monitors and muon telescopes are used. The technique of the analysis includes: (a) calculation of asymptotic cones of ground-based detectors; (b) modeling of cosmic ray detector responses at variable parameters of the flux of solar relativistic protons; (c) determination of primary solar proton parameters outside magnetosphere by comparison of computed responses with observations. Certain evidence was obtained that the flux of relativistic solar protons consisted of two distinct components: prompt and delayed ones. The prompt component with exponential energy spectrum caused a giant impulse-like increase at a number of European cosmic ray stations. The delayed component had a power-law spectrum and was a cause of gradual increase at cosmic ray stations in the North American region. A numerical simulation of the proton acceleration in the vicinity of the magnetic reconnection region brings to the proton spectrum with exponential dependence on energy. This agrees with observational data for the prompt component. It is also shown that the huge increase in ∼5000% on neutron monitors was due to the prompt component only with the exponential proton spectrum. The power-law spectrum of comparable intensity gave considerably smaller effect.     

Model of energetic populations at Ganymede,implications for an orbiter

A model is developed to study the energetic particle populations in Ganymede’s magnetosphere. The main objective is to estimate to what extent the moon could protect an orbiter from radiations. Using Liouville’s theorem, the phase space density of particles coming from Jupiter’s magnetosphere is calculated at any point of Ganymede’s environment. Up to energies of ∼50–100 keV for ions and ∼10–20 MeV for electrons, Ganymede’s magnetic field appears to be able to form distinctive populations as loss-cones over the polar caps and radiation belts. At larger energies, these features are blurred by Larmor radius effects; the moon absorption simply creates a quasi-isotropic layer of ∼500 km thickness where the flux is reduced by ∼40–50%. The predictions are compared to Galileo measurements. In particular, we demonstrate the importance of the moon sweeping in reducing the flux over the polar caps. Interestingly, this can be accounted for by assuming that the particles bouncing between Jupiter and Ganymede are ideally scattered in pitch angle and permanently re-fill the loss-cone, which increases the precipitation on Ganymede’s polar cap. In overall, it is estimated that the radiation dose received by an orbiter of Ganymede will be reduced by more than 50–60% compared to the expected dose at Jupiter/Ganymede distance. This should have a positive impact on the design of a future orbiter of Ganymede.     

Energetic neutral atom (ENA) and charged particle periodicities in Saturn’s magnetosphere

The Magnetospheric Imaging Instrument (MIMI) on the Cassini spacecraft has observed energetic neutral atoms (ENA) and charged particles at Saturn from mid-2004 to the present. The particles often but not always reveal striking periodic behavior that seems to depend on the type of particle and spacecraft location. When subjected to a Lomb periodogram analysis, energetic electrons (>150 keV) exhibited strong frequency peaks near 10.80 h (the nominal or “base” period of Saturn kilometric radiation) during 2006–2008, but essentially no periodicity during 2005. The electron periodograms also show pronounced “double” frequency peaks in 2007 and 2008. Energetic protons (3–26 keV) show strong peaks near the same period for 2005–2007, but none for 2008. Oxygen ions at the same energies display strong peaks for 2005 and 2006, but not for 2007 and 2008. By projecting the ENA images onto Saturn’s equatorial plane or onto a plane perpendicular to the equatorial plane and then summing the data in the appropriate dimension, “strip” images can be constructed from which a time history can be derived. These time histories of ENA emissions are also subjected to a Lomb periodogram analyses. The energetic hydrogen neutrals (20–50 keV) exhibited periodic behavior only during 2007, while energetic oxygen neutrals (64–144 keV) displayed a strong SKR-like period in 2005 and 2006 but not for 2007 or 2008. Some of this behavior may be due to changing spacecraft aspect relative to the ENA emissions, and some of it may be real. This periodic behavior may be consistent with a rotating anomaly that “flashes” brightly in the midnight-to-dawn sector once per 10.8 h, with the flash parameters depending on particle species and energy.     

Research Advances of Solar Corona and Interplanetary Physics in China: 2012–2014

Solar transients and their related interplanetary counterparts have severe effects on the space environments of the Earth. Therefore, the research of solar corona and interplanetary physics has become the focus of study for both solar and space scientists. Considerable progress has been achieved in these aspects by the solar and space physics community of China during 2012–2014, which will be given in this report. The brief report summarizes the research advances of solar corona and interplanetary physics into the following parts: solar wind origin and turbulence, coronal waves and seismology, solar eruptions, solar energetic particle and galactic cosmic ray, magnetic reconnection,Magnetohydrodynamic(MHD) models and their applications, waves and structures in solar wind,propagation of ICMEs/shocks and their arrival time predictions. These research achievements have been achieved by Chinese solar and space scientists independently or via international collaborations.