太阳高能粒子的电荷态和粒子强度间的相关性

本文发表了在太阳高能粒子事件中,元素氦、碳、氮、氧、氖、镁、硅、硫和铁的离子电荷态的分布。研究结果表明,除氦之外上述元素的电荷态分布的不同离子价的数目是随元素的质量而增大。核子能量在2—3MeV范围内,这些元素的平均粒子强度相对于碳的平均粒子强度之间的相关性能够用离子价的数目随元素质量的增加来解释,而不能用日冕温度确定的电荷态平衡模型来解释。且得出结论,太阳高能粒子的离子电荷是在太阳耀斑区而不是在星际激波区产生。      

近月空间带电粒子环境——“嫦娥1号”“嫦娥2号”观测结果

“嫦娥1号”（CE-1）、“嫦娥2号”（CE-2）都安装了1台太阳高能粒子探测器（High-energetic ParticlesDetectors,HPD）和2台太阳风离子探测器（Solar Wind Ion Detectors,SWIDs）,进行了月球轨道200 km和100 km空间环境探测,获得了月球轨道空间高能带电粒子（质子、电子和重离子）能谱随时间的演化特征、等离子体与月球相互作用特征以及太阳风离子速度、密度和温度参量。空间环境探测数据分析结果表明：太阳活动低年、空间环境扰动水平相对较低、月球处于太阳风中时,近月空间带电粒子环境的基本特征与行星际空间相比变化不大。CE-1、CE-2在轨运行期间,发现了多起0.1～2 MeV能量电子急剧增加事件,这些事件发生在月球从太阳风运动到磁尾的所有空间区域,其中20%的事件伴随着卫星周围等离子体离子加速。模拟和统计研究表明：能量电子急剧增加使得绕月卫星和月球表面电位大幅下降导致了离子加速现象的发生;能量电子总流量大于10¹¹ cm^-2时,绕月卫星和月球表面充电电位可达负的上千伏。此外,月表溅射与反射太阳风离子、太阳风“拾起”离子等空间环境事件的发现,揭示了太阳风离子和月球存在复杂的相互作用过程。     

史汪彗星的彗尾

史汪彗星彗尾里的纹纹路是怎么产生的?2006年11月,史汪彗星意外增亮到肉眼可见的程度,而离子尾也出现了幽灵般变幻的细部构造.离子尾是由太阳紫外线游离的体所构成,并在太阳风的推送下离开太阳.太阳风本身就具有很强的结构性,并深受太阳变幻莫测的磁场的挟制.     

回旋波共振加热加速的多重离子流体模型

在回旋波共振准线性理论基础上建立了自恰描述质子和氧离子各向异性温度和整体速度的双离子流体模型,求得数值解,并与UVCS观测相比较.发现在波谱斜率固定的假设下,模型的数值结果虽然与观测有相同趋势,但不能在误差范围之内解释全部观测现象.进一步的研究需要考虑波谱形状的自洽演化.      

暴时极光区热层大气焦耳加热与F区电离耗空的EISCAT雷达观测

利用ＥＩＳＣＡＴ雷达探测数据，分析计算了太阳活动高年夏季发生的一次强磁暴期间，极光区电离层对流电场、电导率以及焦耳加热速率等着重考察了Ｅ区热怪大气焦耳加热和Ｆ区离子摩擦增温与Ｆ区电子密度耗空的关系发现在下午东向极光电集流期间，电子密度最大耗空出现在Ｆ区３００－３２５ｋｍ高度，时间恰在积分的Ｅ区大气焦耳加热量大值和Ｆ区最大离子增温之后５－１０ｍｉｎ，耗空率达７０％。     

太阳软X射线背景水平与X级的增强发射

本文根据1986年1月-1992年12月期间,130个1-8?的X级别的X射线事件与相应背景发射水平所作的分析,发现90%以上的X级X射线事件,都发生在X射线背景发射≥C1(10-6W／m2)水平上,这一统计规律,可从耀斑加速的非热电子对色球等离于体的加热得到合理的解释.      

X射线耀斑的强度指标

本文利用GOES-7卫星的1分钟记录资料研究了1991年3月和6月期间6个大X耀斑伴随的软X射线爆发特性和源强度的关系。结果指出：对X射线耀斑，其射线辐射流量上升快的在日冕中激起的激波速度也较快．数值模拟研究指出，这可能反映爆发能量释放速率是源强度的主要指标．     

太阳风高速流能流分布

根据Ylysses观测,比较完整地计算了高纬行星际空间太阳风能流分布．计算表明,行星际空间的高速流能流密度约为2．1×10-3J·m-2·s-1（日心距离r＝1AU）,主要来自于太阳风离子所携带的动能流（占58％）和克服太阳引力的势能流（占39％）．要驱动高速流,需要在日冕底部高速流源区（日心距离r=1Rs）向外输出到太阳风的能流密度为7．1×102J·m-2·s－1·分析表明,由日冕底部向外可能输出两种形式的能流,其中一种具有较短的耗散长度,被耗散在很短的空间区域（～1—2Rs）,使日冕温度迅速提高。另一种储藏在连续向外传播的太阳风中,不断耗散用以加速太阳风（＞2Rs）．     

低功率氮氢电弧加热发动机非平衡数值模拟

文章对低功率氮氢电弧加热发动机进行了双温度化学非平衡数值模拟研究,模型中包含总的能量方程和电子能量方程,等离子体组分包括分子、原子、离子和电子等7个组分,采用的化学动力学模型中包含了氮氢组分解离、电离等重要的动力学过程,气体的物性根据当地的组分和温度实时计算。通过计算获得了发动机内部气体温度及各组分数密度分布。结果表明,发动机轴线附近等离子体接近热力学平衡,而在发动机阳极壁面电弧贴附区域等离子体明显偏离热力学平衡;计算获得的组分分布表明电弧加热发动机内存在反混合过程,即发动机内各组分分布与入口浓度分布明显不同。氢组分由发动机中心到阳极壁面沿径向呈现先减小后增大的趋势;而氮组分的浓度分布趋势与氢组分相反;进一步的分析表明,发动机内各组分的扩散主要受到气体解离和电离过程引起的浓度梯度所驱动。     

磁暴期间电离层电磁离子回旋波的地方时分布差异

利用Swarm卫星的高精度（50 Hz）磁场观测数据,对2015年3月16—25日磁暴期间中纬度电离层电磁离子回旋（EMIC）波时空分布特征进行了研究.结果表明:晨侧EMIC波事件数与昏侧大致相当,午前时段明显多于子夜前时段.昏侧EMIC波高发生率与等离子体羽状结构有关,晨侧EMIC波高发生率与太阳风动压增强及稠密冷等离子体有关.晨侧-正午前EMIC波频率高于昏侧-子夜前,表明源区位置以及离子成分占比存在地方时差异.昏侧事件大多发生在早期恢复相,晨侧事件大多发生在晚期恢复相,晨-昏两侧的时间差异源于磁暴期间高能离子西向漂移所需时间及等离子体层顶位置的地方时差异.磁暴期间,EMIC波以H+波和He+为主,其中H+波主要分布在06:00 MLT—10:00 MLT（磁地方时）扇区,He+波主要分布在18:00 MLT—22:00 MLT扇区.在磁暴主相期间没有出现H+带波,但是出现He+-O+双波段EMIC波,表明磁暴主相期间环电流高浓度氧离子对H+带EMIC波具有抑制作用.      

Recovering of the thermal band of Landsat 7 SLC-off ETM+ image using CBERS as auxiliary data

The failure of scan-line corrector (SLC-off) has resulted in the limited use of Landsat 7 ETM+ images. Considering its characteristics, many attempts have been conducted to recover the SLC-off ETM+ image. While much attention has been paid to recovering the optically multispectral bands, few researches have been done to reconstruct the thermal band. Main purposes of our study were to evaluate the possibility that using China Brazil Earth Resources Satellite (CBERS) as auxiliary data to recover the thermal band of SLC-off ETM+, and discuss the usage of the recovered one. The adaptive window linear histogram match (AWLHM) method was selected primarily, followed by the modified one. Results illustrated the feasibility of using the modified AWLHM method with the linear combination of CBERS-01 band3 and band4 to reconstruct the SLC-off thermal band. It encourages that further researches should be done to enable more scientific application of SLC-off ETM+, particularly its’ thermal band.     

Polar/TIMAS statistical results on the outflow of molecular ions from earth at solar minimum

Ion composition data from the first 22 months of operation of the Polar/TIMAS instrument, covering the 15-eV/e to 33-keV/e energy range, have been surveyed to determine the typical abundance, at solar minimum, of N₂⁺, NO⁺ and O₂⁺ ions in the auroral ion outflow, as compared to that of the better known O⁺ ions. The results indicate that molecular ions have roughly the same energy distribution as the O⁺ ions, with maximum differential flux occurring below 400 eV, but are far less abundant, by two orders of magnitude. The molecular ions also differ from the O⁺ ions in that they seem more specifically associated with enhanced geomagnetic activity.     

Auroral signatures of transient processes in the outer magnetosphere

We present an analysis of sporadic and recurrent injections of magnetospheric ions in the midnight auroral oval during substorms and of the associated ionospheric ion outflows. The source of plasma sheet precipitating ions is determined using a simple method, based on the measured relation between the ion inverse velocity and time (l = v × t). This method is applied here to two typical passes of the Interball-Auroral (IA) satellite at distances of 3 R_E above the auroral regions. Substorm related ion injections are shown to be mainly due to time of flight effects. In contrast with particle trajectory computations (Sauvaud et al., 1999), the inverse velocity method does not require magnetic and electric field models and can thus be used systematically for the detection of time of flight dispersed ion structures (TDIS). This allowed us to build a large database of TDIS events and to perform a statistical analysis of their spatial distribution. For the cases presented here the source region of the injected ions is found at radial distances from 18 to 30 R_E near the equatorial magnetosphere. At Interball altitudes ( 3 R_E), ion injections detected at the poleward boundary of the nighside auroral oval are associated with shear Alfvén waves superimposed over large-scale quasi-static current structures. We show that the most poleward TDIS are collocated with a large outflow of ionospheric H⁺ and O⁺ displaying pitch-angle distributions peaked in the pitch-angle range 90°–120°. These ions are thus accelerated perpendicularly to the magnetic field not only in the main auroral acceleration region but also up to at least 3 R_E. The expanding auroral bulge thus constitutes a significant source of H⁺ and O⁺ ions for the mid-tail magnetosphere.     

Polycyclic aromatic hydrocarbon ions and the diffuse interstellar bands.

Neutral naphthalene (C10H8), phenanthrene (C14H10), and pyrene (C16H10) absorb strongly in the ultraviolet and may contribute to the extinction curve. High abundances are required to produce detectable structures. The cations of these PAHs absorb in the visible. C10H8+ has 12 discrete absorption bands which fall between 6800 and 5000 angstroms. The strongest band at 6741 angstroms falls close to the weak 6742 angstroms diffuse interstellar band (DIB). Five other weaker bands also match DIBs. The possibility that C10H8+ is responsible for some of the DIBs can be tested by searching for new DIBs at 6520, 6151, and 5965 angstroms, other moderately strong naphthalene cation band positions. If C10H8+ is indeed responsible for the 6742 angstroms feature, it accounts for 0.3% of the cosmic carbon. The spectrum of C16H10+ is dominated by a strong band at 4435 angstroms in an Ar matrix and 4395 angstroms in a Ne matrix, a position which falls very close to the strongest DIB, that at 4430 angstroms. If C16H10+, or a closely related pyrene-like ion is indeed responsible for the 4430 angstroms feature, it accounts for 0.2% of the cosmic carbon. We also report an intense, very broad UV-to-visible continuum which is associated with both ions and could explain how PAHs convert interstellar UV and visible radiation into IR.     

AUSM系列算法对比研究及背景太阳风初步应用

磁流体力学数值模拟是研究日地物理学现象的一个重要手段. 对比三种AUSM算法, 即AUSM, AUSM+和AUSMPW+, 结合HDC磁场散度消去方法计算多维MHD问题的性能. 通过分析三种算法计算Rotor算例和Orszag-Tang vortex算例的结果发现, AUSM+算法的性能最好. 进一步使用AUSM+算法基于6片网格构造模拟了日冕结构, 计算结果表明这种算法能够正确计算出日冕的大尺度结构. 对于日冕结构模拟块, HDC方法能够较好 地控制磁场散度误差.      

多离子空间等离子体中快磁声波与粒子的回旋共振特性

快磁声波是空间等离子体中一种接近垂直传播的右旋极化电磁波,能够在等离子体层内外传播.快磁声波与带电粒子的回旋共振相互作用能够导致高能电子随机加速和投掷角扩散、能量质子投掷角扩散等,从而影响辐射带高能带电粒子的动态过程.分别基于完整的色散关系和高密度近似的色散关系,在不同空间等离子体条件下研究多离子空间等离子体中不同传播角的快磁声波色散曲线,并计算了快磁声波与H+,He+和O+离子的最小共振能量.结果表明,当传播角较小时,采用高密度近似与采用完整色散关系计算的离子最小共振能量没有太大差别.在中低密度中强磁场空间等离子体中,传播角≥ 88°时高密度近似色散关系会带来很大的误差,因此应利用完整色散关系计算最小共振能量.      

On the line ratio diagnostics for NeV, MgV, SiVII and MgVII solar ions

We present NeV/MgV and MgVII/SiVII theoretical line intensity ratios as a function of electron density and temperature for physical conditions within the solar chromosphere-corona transition region. The electron pressure within the emission regions has been assumed to be a constant parameter. These line intensity ratios in addition could be useful for estimating relative element abundances Ne/Mg and Mg/Si. Line intensities of these ions have been computed using a model solar atmosphere and these have been compared with the available observed values for the quiet -Sun conditions. The analysis suggests the need for observations at higher spectral resolution. The successful launch of the SOHO satellite recently should provide such spectra.     

Comparison of ion composition from the goddard comprehensive ionosphere database with the international reference ionosphere model

We compared the IRI values of T_e, N_e, T_i, O⁺, H⁺, He⁺, O₂₊, and NO⁺ with AE-C values, obtained from the Goddard Comprehensive Ionosphere Database (GCID), composed of data from the satellites, AE-B, OGO-6, ISIS-2, AE-C, AE-D, and AE-E. O⁺ - H⁺ transition levels were derived from the IRI and AE-C altitude profiles. Some discrepancies were found between IRI and the AE-C data. The IRI electron density was found to be about a factor of 2 higher than the data. The H⁺ composition agreed best among the IRI ions, with an average AE-C/IRI ratio of 1.05. The temperatures of both electrons and ions agreed quite well: the average ratios of AE-C/IRI was found to be .99 for electrons and 1.17 for ions.     

碘工质射频离子推力器栅极系统束流特性仿真

为分析碘工质射频离子推力器束流特性,应用粒子云网格算法（PIC）,对碘工质射频离子推力器栅极系统进行三维数值仿真。碘工质电离产物中除了大量存在的I⁺,还包含少量I₂⁺、I²⁺、I³⁺几种多价离子。对添加多价离子前后束流特性的仿真结果进行对比,得出该栅极系统离子空间分布、电势分布、离子相空间分布以及束流、束流发散角,并对变密度工况下束流大小进行统计。计算结果表明,程序能较好地模拟离子在栅极系统中的运动情况：添加多价离子后,等离子体悬浮电势有所上升,鞍点电势有所下降,但整体电势分布的变化幅度较小;添加多价离子后束流大小略有增加,束流发散角略有减小,通过理论分析可知仿真所得理论推力及理论比冲均有小幅度增加;放电室等离子体数密度增加到约2.4×10¹⁷m^-3时,该栅极系统达到了束流引出的极限,后续增大等离子体密度引出束流不增反降。模拟结果可以为碘工质射频离子推力器栅极系统的设计提供参考。     

Low energy ions in the heavy ions in space (HIIS) experiment on LDEF.

We present data from the Lexan top stacks in the Heavy Ions In Space (HIIS) experiment which was flown for six years (April 1984-Jan 1990) onboard the LDEF spacecraft in 28.5 degrees orbit at about 476 km altitude. HIIS was built of passive (i.e. no timing resolution) plastic track detectors which collected particles continuously over the entire mission. In this paper we present data on low energy heavy ions (10 < or = Z, 20MeV/nuc < E < 200 MeV/nuc). These ions are far below the geomagnetic cutoff for fully ionized ions in the LDEF orbit even after taking into account the severe cutoff suppression caused by occasional large geomagnetic storms during the LDEF mission. Our preliminary results indicate an unusual elemental composition of trapped particles in the inner magnetosphere during the LDEF mission, including both trapped anomalous cosmic ray species (Ne, Ar) and other elements (such as Mg and Fe) which are not found in the anomalous component of cosmic rays. The origin of the non-anomalous species is not understood, but they may be associated with the solar energetic particle events and geomagnetic disturbances of 1989.