Modeling the solar cosmic ray event of 13 December 2006 using ground level neutron monitor data

In order to understand the physics under extreme solar conditions such as those producing ground level enhancements of solar cosmic rays, it is important to use accurate and reliable models. The NM-BANGLE Model is a new cosmic ray model which couples primary solar cosmic rays at the top of the Earth’s atmosphere with the secondary ones detected at ground level by neutron monitors during GLEs. This model calculates the evolution of several GLE parameters such as the solar cosmic ray spectrum, anisotropy and particle flux distribution, revealing crucial information on the energetic particle propagation and distribution. The total output of the NM-BANGLE Model is a multi-dimensional GLE picture that gives an important contribution to revealing the characteristics of solar energetic particle events recorded at ground level. In this work, the results of the NM-BANGLE Model application to the recent GLE of 13 December 2006 are presented and discussed. Moreover, a comparison with the extreme event of 20 January 2005 (GLE69) has been realized.     

Ion production and ionization effect in the atmosphere during the Bastille day GLE 59 due to high energy SEPs

The influence of high energy particles, specifically cosmic rays, on atmospheric physics and chemistry is highly discussed. In most of the proposed models the role of ionization in the atmosphere due to cosmic rays is not negligible. Moreover, effect(s) on minor constituents and aerosols are recently observed, specifically over the polar regions during strong solar particle events. According to the recent findings for such effects it is necessary an essential increase of ion production, specifically during the winter period. The galactic cosmic rays are the main source of ionization in the Earth’s stratosphere and troposphere. Occasionally, the atmospheric ionization is significantly enhanced during strong solar energetic particles events, specifically over the polar caps. During the solar cycle 23 several strong ground level enhancements were observed. One of the strongest was the Bastille day event occurred on 14 July 2000. Using a full Monte Carlo 3-D model, we compute the atmospheric ionization, considering explicitly the contribution of cosmic rays with galactic and solar origin, focusing on high energy particles. The model is based on atmospheric cascade simulation with the PLANETOCOSMICS code. The ion production rate is computed as a function of the altitude above the sea level. The ion production rate is computed on a step ranging from 10 to 30?min throughout the event, considering explicitly the spectral and angular characteristics of the high energy part of solar protons as well as their time evolution. The corresponding event averaged ionization effect relative to the average due to galactic cosmic rays is computed in lower stratosphere and upper troposphere at various altitudes, namely 20?km, 15?km, 12?km and 8?km above the sea level in a sub-polar and polar regions. The 24^h and the weekly ionization effects are also computed in the troposphere and low stratosphere. Several applications are discussed.     

双补燃室固冲凝聚相颗粒分布对比试验研究

针对固冲发动机燃烧效率较低以及凝相粒子分布规律不清楚的现状,本文建立了一套评价固冲发动机燃烧效率的双补燃室试验装置和研究凝相颗粒分布的取样装置。对比研究了结构相同的补燃室内的参数,其误差小于0.5%,说明该装置可以用于精确对比不同补燃室的燃烧效率。然后应用该装置完成了补燃室长度分别为600mm、800mm、1000mm,进气角度分别为30°、45°、60°的对比试验,分析了粒子的粒度分布规律和化学成分变化规律,该规律与数值分析的规律相同。试验结果表明：在进气角度不变情况下,补燃室长度增加有利于提高燃烧效率,燃烧室压强提高,凝相粒子直径明显减小,B粒子燃烧更充分;在补燃室长度为1000mm的情况下,进气角度增加有利于燃烧效率增加,燃烧室压强提高,粒子直径减小,B粒子燃烧更充分。双补燃室发动机是评价补燃室燃烧效率的有效装置,粒度分布和燃烧产物的化学成分有助于补燃室结构设计。     

小型回流燃烧室燃烧特性数值研究

某科研样机采用蒸发管回流燃烧室,其燃烧室结构复杂,燃烧机理和气流流动情况尚不清楚。在实验过程中发现,蒸发管及附近的火焰筒壁面上出现了较严重的积碳现象,影响燃烧室的性能。为了探究该型燃烧室的工作过程、分析积碳现象的原因,采用k-ε湍流模型、旋涡耗散概念燃烧模型(EDC)以及颗粒随机轨道模型对该燃烧室工作流场进行流固热耦合数值计算。结果表明,燃烧室性能参数计算值与台架试车数据较吻合,各项参数相对误差均小于1.7%。计算得到了燃烧室工作时流动和燃烧情况,同时分析出了各气孔流动情况及发挥的作用,并得出了产生积碳现象的原因,为该型燃烧室优化设计提供依据。     

Evidence for a Two-Stage Acceleration Process in Large Solar Energetic Particle Events

Using high-resolution mass spectrometers on board the Advanced Composition Explorer (ACE), we surveyed the event-averaged ∼0.1–60 MeV/nuc heavy ion elemental composition in 64 large solar energetic particle (LSEP) events of cycle 23. Our results show the following: (1) The Fe/O ratio decreases with increasing energy up to ∼10 MeV/nuc in ∼92% of the events and up to ∼60 MeV/nuc in ∼64% of the events. (2) The rare isotope ³He is greatly enhanced over the corona or the solar wind values in 46% of the events. (3) The heavy ion abundances are not systematically organized by the ion’s M/Q ratio when compared with the solar wind values. (4) Heavy ion abundances from C–Fe exhibit systematic M/Q-dependent enhancements that are remarkably similar to those seen in ³He-rich SEP events and CME-driven interplanetary (IP) shock events. Taken together, these results confirm the role of shocks in energizing particles up to ∼60 MeV/nuc in the majority of large SEP events of cycle 23, but also show that the seed population is not dominated by ions originating from the ambient corona or the thermal solar wind, as previously believed. Rather, it appears that the source material for CME-associated large SEP events originates predominantly from a suprathermal population with a heavy ion enrichment pattern that is organized according to the ion’s mass-per-charge ratio. These new results indicate that current LSEP models must include the routine production of this dynamic suprathermal seed population as a critical pre-cursor to the CME shock acceleration process.     

Solar Energetic Particle Events: Phenomenology and Prediction

Space Science Reviews - Solar energetic particle events can cause major disruptions to the operation of spacecraft in earth orbit and outside the earth's magnetosphere and have to be considered...     

气固两相管道流中柱状粒子取向的数值研究

本文对管道悬浮流中柱状粒子的取向分布进行研究。首先对柱状粒子在流场内的运动进行数值模拟，然后运用统计方法得出大量柱状粒子的取向分布；得到了粒子长径比、St数和流场区域对粒子取向分布的影响。计算结果表明，柱状粒子长径比和St数的变化对粒子取向分布的影响并不明显，而流场区域所造成的流场横向速度梯度对粒子取向分布有重要的影响。随着流场横向速度梯度的增大，粒子有明显的占优取向，且当流场横向速度梯度增大到一定程度时，粒子取向都趋向于流动方向。文中部分结果与实验进行了比较，两者吻合较好。     

纳米锑颗粒的制备及其分散性研究

采用电化学方法电沉积制得不同形貌及粒径的纳米锑颗粒,并在制备过程中使用OP-10对纳米锑颗粒表面进行了原位改性.通过TEM、XRD、FTIR等方法对纳米锑颗粒的形态、物相和包覆效果进行表征.结果显示,纳米锑颗粒的制备具有时间效应和电流效应.随着反应时间的加长,纳米锑颗粒粒径变大,且在某种程度上存在着团聚现象;电流密度在一定范围内,适当增大电流密度有利于纳米锑颗粒的形成.纳米锑颗粒的表面改性,主要是通过OP-10的长链分子结构与纳米锑颗粒之间的化学吸附以及OP-10的长链烷基分子之间的氢键、范德华力相互作用,分子链相互缠结,部分通过C-H键互相渗入,最终有效地包覆在纳米锑颗粒表面来达到其表面改性效果,同时在反应过程中醚键也起了一定作用.纳米锑颗粒在纯液体石蜡油中的分散稳定性能与其添加量有关,其最佳添加量为0.5％.     

Simulation of ASTROD I test mass charging due to solar energetic particles and interplanetary electrons

As ASTROD I travels through space, its test mass will accrue charge due to exposure of the spacecraft to high-energy particles. This test mass charge will result in Coulomb forces between the test mass and the surrounding electrodes. In earlier work, we have used the GEANT 4 toolkit to simulate charging of the ASTROD test mass due to cosmic-ray protons of energies between 0.1 and 1000 GeV at solar maximum and at solar minimum. Here we use GEANT 4 to simulate the charging process due to solar energetic particle events and interplanetary electrons. We then estimate the test mass acceleration noise due to these fluxes. The predicted charging rates range from 2247 e⁺/s to 47,055 e⁺/s, at peak intensity, for the four largest SEP events in September and October 1989. Although the noise due to charging exceeds the ASTROD I budget for the two larger events, it can be suppressed through continuous discharging. The acceleration noise during the two small events is well below the design target. The charging rate of the ASTROD I test mass due to interplanetary electrons in this simulation is about −11% of the cosmic-ray protons at solar minimum, and over −37% at solar maximum. In addition to the Monte Carlo uncertainty, an error of ±30% in the net charging rates should be added to account for uncertainties in the spectra, physics models and geometry implementations.     

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.