镁粉与二氧化碳动态点火燃烧特性数值研究

Mg粉/CO₂粉末发动机是火星探测中较为理想的原位资源利用方案，为了掌握Mg/CO₂粉末发动机稳定点火燃烧特性，在考虑氧化层厚度对Mg颗粒熄火影响的基础上，基于涡耗散/有限速率模型建立了点火燃烧模型，并应用数值计算方法研究了Mg粉颗粒粒径（5μm， 10μm， 15μm， 20μm和25μm）、入口预混气流雷诺数（1500， 2000， 2500， 3000和3500）和CO₂/Mg氧燃比（0.5， 1， 1.5， 2和2.5）对Mg粉/CO₂动态点火燃烧的影响。计算结果表明：雷诺数和氧燃比恒定时，随着粒径从5μm增加到10μm，平均温度升高，平均点火时间延长，燃烧效率增加；随着粒径从10μm增加到25μm，平均温度降低，平均点火时间延长，燃烧效率减少。粒径和氧燃比恒定时，平均温度随雷诺数增加而下降；平均点火时间和燃烧效率随雷诺数增加基本不变。粒径和雷诺数恒定，随着氧燃比从0.5增大到1.5，平均温度升高；随着氧燃比从1.5增大到2.5，平均温度下降；平均点火时间和燃烧效率随氧燃比增大基本不变。     

A numerical study of segmented cooling-stream injection in supersonic film cooling

The present study proposes a segmented cooling-stream injection structure based on a certain coolant mass flow rate, and numerically investigates the effect of segmented cooling-stream injection on supersonic film cooling. The results indicate that without shock-wave impingement and with helium as the coolant, segmented cooling-stream injection can reduce the mixing between the mainstream and the cooling stream to produce better cooling performance than single injection, especially at larger coo...     

Statistical analysis of the occurrence rate of geomagnetic storms during solar cycles 20–24

This study examines the occurrences rate of geomagnetic storms during the solar cycles (SCs) 20–24. It also investigates the solar sources at SCs 23 and 24. The Disturbed storm time (Dst) and Sunspot Number (SSN) data were used in the study. The study establishes that the magnitude of the rate of occurrences of geomagnetic storms is higher (lower) at the descending phases (minimum phases) of solar cycle. It as well reveals that severe and extreme geomagnetic storms (Dst < -250 nT) seldom occur at low solar activity but at very high solar activity and are mostly associated with coronal mass ejections (CMEs) when occurred. Storms caused by CME + CH-HSSW are more prominent during the descending phase than any other phase of the solar cycle. Solar minimum features more CH-HSSW- associated storms than any other phase. It was also revealed that all high intensity geomagnetic storms (strong, severe and extreme) are mostly associated with CMEs. However, CH-HSSW can occasionally generate strong storms during solar minimum. The results have proven that CMEs are the leading cause of geomagnetic storms at the ascending, maximum and the descending phases of the cycles 23 and 24 followed by CME + CH-HSSW. The results from this study indicate that the rate of occurrence of geomagnetic storms could be predicted in SC phases.