基于SAMPEX卫星观测的南大西洋异常区高能质子动态分布特征

利用SAMPEX卫星1992年7月至2004年6月19～27MeV高能质子数据对南大西洋异常区的分布特征进行研究, 发现南大西洋异常区高能质子分布随高度及F_10.7的变化十分显著. 在540±25km高度上, 地磁较为平静时期南大西洋异常区高能质子微分通量随着F_10.7的增大而减小, 同时在F_10.7≥115sfu时减小趋势较为平缓. 对中等及以上磁暴进行统计分析发现, 磁暴期间南大西洋异常区高能质子微分通量和SYM-H指数的绝对值存在明显的反相关关系, 且地磁暴对南大西洋异常区高能质子微分通量存在明显的持续影响效应. 磁暴发生期间高能质子微分通量明显减少. 磁暴恢复相及其之后高能质子微分通量呈现较为显著的恢复过程.      

芳纶短纤和浆粕增强聚氨酯泡沫的结构和性能研究

采用芳纶短纤(AF)和芳纶浆粕(AP)对聚氨酯泡沫进行增强,制备了两种增强聚氨酯泡沫,考察了其的泡孔结构、压缩强度以及热稳定性能。结果表明:随着芳纶纤维和浆粕填充量增加,聚氨酯泡沫的密度和压缩强度呈先增加后减小的变化趋势;当AF和AP的填充量为6wt%时,聚氨酯泡沫底部的压缩强度最大,分别为0.394和0.353 MPa,此时发泡过程中黏弹性增加,表面张力减小导致泡孔孔径明显变小且均匀性提高,纤维分布在泡棱上通过与树脂形成良好的结合起到增强效果;AF和AP的加入有助于提高聚氨酯泡沫的热稳定性,AF增强聚氨酯泡沫具有更好的热稳定性。     

Solar wind low-energy energetic ion enhancements: A tool to forecast large geomagnetic storms

Predicting the occurrence of large geomagnetic storms more than an hour in advance is an important, yet difficult task. Energetic ion data show enhancements in flux that herald the approach of interplanetary shocks, usually for many hours before the shock arrival. We present a technique for predicting large geomagnetic storms (Kp  7) following the arrival of interplanetary shocks at 1 AU, using low-energy energetic ions (47–65 keV) and solar wind data measured at the L1 libration point. It is based on a study of the relationship between energetic ion enhancements (EIEs) and large geomagnetic storms by Smith et al. [Smith, Z., Murtagh, W., Smithtro, C. Relationship between solar wind low-energy energetic ion enhancements and large geomagnetic storms. J. Geophys. Res. 109, A01110, 2004. doi:10.1029/ 2003JA010044] using data in the rise and maximum of solar cycle 23 (February 1998–December 2000). An excellent correlation was found between storms with Kp  7 and the peak flux of large energetic ion enhancements that almost always (93% of time in our time period) accompany the arrival of interplanetary shocks at L1. However, as there are many more large EIEs than large geomagnetic storms, other characteristics were investigated to help determine which EIEs are likely to be followed by large storms. An additional parameter, the magnitude of the post-shock total magnetic field at the L1 Lagrangian point, is introduced here. This improves the identification of the EIEs that are likely to be followed by large storms. A forecasting technique is developed and tested on the time period of the original study (the training data set). The lead times, defined as the times from the arrival of the shock to the start of the 3-h interval of maximum Kp, are also presented. They range from minutes to more than a day; the average for large storms is 7 h. These times do not include the extra warning time given when the EI flux cross the high thresholds ahead of the shock. Because the data-stream used in the original study is no longer available, we extended the original study (1998–2000) to 2001, in order to: (a) investigate EIEs in 2001; (b) present a validation of the technique on an independent data set; (c) compare the results based on the original (P1) energy channel to those of the replacement (P1′) and (d), determine new EIE thresholds for forecasting geomagnetic storms using P1′ data. The verification of this P1′ training data set is also presented, together with lead times.     

Solar proton enhancements in different energy channels and coronal mass ejections during the last solar cycle

The main properties of 11622 coronal mass ejections (CMEs) observed by the Solar and Heliospheric Observatory (SOHO) mission’s Large Angle and Spectrometric Coronagraph (LASCO-C2) from January 1996 through December 2006 are considered. Moreover, the extended database of solar proton enhancements (SPEs) with proton flux >0.1 pfu at energy >10 MeV measured at the Earth’s orbit is also studied. A comparison of these databases gives new results concerning the sources and acceleration mechanisms of solar energetic particles. Specifically, coronal mass ejections with width >180° (wide) and linear speed >800 km/s (fast) seem they have the best correlation with solar proton enhancements. The study of some specific solar parameters, such as soft X-ray flares, sunspot numbers, solar flare index etc. has showed that the soft X-ray flares with importance >M5 may provide a reasonable proxy index for the SPE production rate. From this work, it is outlined that the good relation of the fast and wide coronal mass ejections to proton enhancements seems to lead to a similar conclusion. In spite of the fact that in the case of CMEs the statistics cover only the last solar cycle, while the measurements of SXR flares are extended over three solar cycles, it is obvious for the studied period that the coronal mass ejections can also provide a good index for the solar proton production.     

基于CAE仿真的两轴柔性滚弯过程的应变分析

介绍了两轴柔性滚弯的工作原理和技术优势.为便于对滚弯过程中弹性层的受力进行分析,提出了折算弹性模量的概念,来定义柔性滚弯过程中聚氨酯橡胶随成形改变的弹性模量,并推导了聚氨酯橡胶折算弹性模量的计算公式.利用非线性有限元分析软件MARC建立了两轴柔性滚弯过程的有限元模型,模拟了板料滚弯成形加工过程,得出了在不同刚性滚直径和不同压入深度下板料与弹性层的应变分布.基于CAE的仿真分析,可以对柔性滚弯过程工艺参数的选取提供依据.     

Comparing proton fluxes of central meridian SEP events with those predicted by SOLPENCO

We have developed an operational code, SOLPENCO, that can be used for space weather prediction schemes of solar energetic particle (SEP) events. SOLPENCO provides proton differential flux and cumulated fluence profiles from the onset of the event up to the arrival of the associated traveling interplanetary shock at the observer’s position (either 1.0 or 0.4 AU). SOLPENCO considers a variety of interplanetary scenarios where the SEP events develop. These scenarios include solar longitudes of the parent solar event ranging from E75 to W90, transit speeds of the associated shock ranging from 400 to 1700 km s⁻¹, proton energies ranging from 0.125 to 64 MeV, and interplanetary conditions for the energetic particle transport characterized by specific mean free paths. We compare the results of SOLPENCO with flux measurements of a set of SEP events observed at 1 AU that fulfill the following four conditions: (1) the association between the interplanetary shock observed at 1 AU and the parent solar event is well established; (2) the heliolongitude of the active region site is within 30° of the Sun–Earth line; (3) the event shows a significant proton flux increase at energies below 96 MeV; (4) the pre-event intensity background is low. The results are discussed in terms of the transit velocity of the shock and the proton energy. We draw conclusions about both the use of SOLPENCO as a prediction tool and the required improvements to make it useful for space weather purposes.     

To the problem on the reliability of solar energetic proton flux models

This work analyses basic issues of conformity of the most well-known models of solar energetic particles (SEP) fluxes to the experimental data. It is shown, that the postulates on neglecting SEP fluxes in quiet Sun years and on invariability SEP fluxes in active Sun years, underlying some models, contradict the experimental data.     

环氧化端羟基聚丁二烯／H12 MDI型聚氨酯固化工艺的研究

采用环氧化端羟基聚丁二烯(EHTPB)与H12MDI固化交联形成聚氨酯弹性体,利用DSC外推法研究了EHTPB/H12MDI型聚氨酯固化的最佳反应温度,再通过测量固化产物的力学性能研究了其他最佳固化工艺参数,包括反应时间、固化剂H12MDI用量、EHTPB环氧值以及扩链剂BDO用量,并在相同条件下对端羟基聚丁二烯(HTPB)/H12MDI和EHTPB/H12MDI固化产物的力学性能进行了比较。结果表明,EHTPB/H12MDI固化产物具备更好的力学性能,并得到了EHTPB/H12MDI型聚氨酯弹性体的最佳固化工艺条件。     

网状聚氨酯泡沫材料的制备,性能及应用

本文介绍了网络聚氨酯泡沫的多种制备方法、材料的主要特性及应用情况。