Nickel Isotopic Composition and Nickel/Iron Ratio in the Solar Wind: Results from SOHO/CELIAS/MTOF

Using the Mass Time-of-Flight Spectrometer (MTOF)—part of the Charge, Elements, Isotope Analysis System (CELIAS)—onboard the Solar Heliospheric Observatory (SOHO) spacecraft, we derive the nickel isotopic composition for the isotopes with mass 58, 60 and 62 in the solar wind. In addition we measure the elemental abundance ratio of nickel to iron. We use data accumulated during ten years of SOHO operation to get sufficiently high counting statistics and compare periods of different solar wind velocities. We compare our values with the meteoritic ratios, which are believed to be a reliable reference for the solar system and also for the solar outer convective zone, since neither element is volatile and no isotopic fractionation is expected in meteorites. Meteoritic isotopic abundances agree with the terrestrial values and can thus be considered to be a reliable reference for the solar isotopic composition. The measurements show that the solar wind elemental Ni/Fe-ratio and the isotopic composition of solar wind nickel are consistent with the meteoritic values. This supports the concept that low-FIP elements are fed without relative fractionation into the solar wind. Our result also confirms the absence of substantial isotopic fractionation processes for medium and heavy ions acting in the solar wind.     

Highlights of the Brazilian Solar Spectroscope

The digital, decimetric (950–2500 MHz) Brazilian Solar Spectroscope (BSS, Sawant, H.S., Subramanian, K.R., Faria, C., et al. Brazilian Solar Spectroscope (BSS). Solar Phys. 200, 167–176, 2001) with high time (10–1000 ms) and frequency (1–10 MHz) resolution is in regular operation since April, 1998, at the National Space Research Institute (INPE) at São José dos Campos, Brazil. The BSS has now been upgraded with a new digital data acquisition and data processing system. The new version of the BSS has improved the observational possibilities with the capability to record up to 200 frequency channels available in the selectable frequency range 950–2500 MHz. The GPS receiver permits the acquisition of data with time accuracy in the order of 0.1 ms. The software system of the BSS is composed by two distinct modules: the first, data acquisition system provides a flexible Graphical User Interface (GUI) that allows one to choose the observational parameters. The second module is the real time visualization system that permits real time visualization of the observed dynamic spectrum and additionally allows procedures for visualization and preliminary analysis of the recorded solar spectra. Using the new visualization system, we have realized two new types of dm-radio fine structures: narrow band type III bursts with positive as well as negative group frequency drift and dots emissions arranged in zebra-like and fiber-like chains. Furthermore, we have found flare generated fast wave trains according to their tadpole signature in wavelet power spectra for a decimetric type IV radio event (June 6, 2000 flare).     

双体卫星对日定向姿态机动控制

研究了双体卫星(DFP)对日定向姿态机动控制问题。首先分析双体卫星工作机理,建立载荷舱与平台舱姿态模型,推导磁浮机构线圈和磁钢相对距离的数学表达式。提出基于PD控制的载荷舱对日姿态机动、平台舱姿态跟踪以及两舱避碰等控制策略。在此基础上,为提高平台舱姿态跟踪速度,设计反步控制器对平台舱飞轮的动态特性进行补偿。进一步,为提高两舱协同控制性能,对传统PD控制进行改进,提出基于变增益PD控制的载荷舱姿态机动控制律,将两舱相对姿态信息包含在载荷舱对日姿态机动控制律中,有效降低了两舱碰撞风险,提高了两舱姿态机动速度。仿真结果表明,本文控制算法能有效实现双体卫星对日定向,且能避免两舱碰撞。     

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.      

太阳微波爆发与高能质子的共生过程

本文根据近年来对太阳射电爆发与高能质子／γ射线谱线辐射等观测资料的统计分析,得出不同型别的太阳射电爆发中以微波爆发与γ射线辐射／质子事件发生过程中的高能质子共生率最高,趋近100％,这一结果,否定了以前认为米波Ⅱ型或米波Ⅳ型爆发拥有产生高能质子必要条件的看法;指出：上述微波爆发可以细分为脉冲型和微波Ⅳ型（Ⅳμ型）,它们的物理条件不同,共生关系的表现特征也不尽相同;并且对上述共生现象的物理过程作了初步的解释和探讨．     

基于MATLAB间断照射雷达信号仿真技术

针对间断照射雷达信号质量分析过程中没有实际雷达的问题,根据复杂间断照射雷达信号产生原理,提出了用任意波形发生器和微波信号源模拟雷达波形的方法,基于软件无线电技术,给出了用MATLAB软件仿真复杂基带调制信号并导入任意波形发生器的具体实施方案。采用该方案设计的信号模拟方法,产生的信号涵盖调制副载波参数、脉冲同步信号、编码信息等丰富的内容,可以解决实验室环境中复杂间断照射雷达信号的获取问题。经过试验验证,该仿真信号的方案具有通用性好、易于实现等特点,可以为相同体制复杂调制信号的产生提供方法和手段,减少试验成本。     

空间站对日定向装置试验台的控制器设计与精度考核

针对太阳电池帆板大挠性、大惯量等特性,导致对对日定向装置施加的大幅值、高频响的变负载力矩难以模拟和模拟精度不足的问题,设计了以电动负载模拟器为核心装置的地面半物理仿真试验台。首先建立了电动负载模拟器（加载单元）模型,采用递推最小二乘法对加载单元各参数进行辨识,并分析各参数对加载单元响应特性的影响。提出一种超前校正与模糊自适应PID相结合的复合控制算法,该方法有效地拓宽了加载单元带宽、改善了力矩跟随性能和抑制了力矩误差。用不同信号对试验台响应速度、加载带宽和加载精度进行分析和考核。实验结果表明：该复合控制算法使加载力矩较好地复现了太阳电池帆板模型的期望输出力矩,为对日定向装置对太阳电池帆板的驱动性能考核实验模拟出较为精确的期望模型的负载（测试）力矩。     

Coronal magnetic field evolution under reconnective relaxation

The nonlinear evolution of a partially open coronal magnetic configuration is considered, assuming that corona responds to photospheric footpoint motions by small-scale reconnection events that produce a relaxed lower-energy state while conserving the global magnetic helicity of the system. The results of numerical calculations for such a relaxed equilibrium show an essential role of the amount of helicity injected to the closed-field region. If photospheric perturbations are incoherent (small-scale shearing with inefficient helicity injection), the relaxed state becomes close to an initial potential field. In this case reconnective relaxation does not result in a substantial global evolution, just providing heating of the corona (Vekstein et al, 1993). On the contrary, sufficient injection of the magnetic helicity can lead to a considerable restructuring of the coronal magnetic configuration, with possible change of its topology (formation of magnetic islands), and even catastrophic loss of equilibrium (Wolfson et al, 1994)     

Solar mass flow in fine-scale structures

Observations of transient and steady velocities at chromospheric, transition region and coronal temperatures in the quiet Sun and coronal holes are reviewed. The relevance of fine-scale structures in governing the mass balance of the solar atmosphere is stressed. At present, a coherent picture of these mass flows does not exist. However, the current observational base of transition region and coronal velocity information is limited but should greatly improve with measurements from the SOHO satellite.     

Analysis of a long-duration AR throughout five solar rotations: Magnetic properties and ejective events

Coronal mass ejections (CMEs), which are among the most magnificent solar eruptions, are a major driver of space weather and can thus affect diverse human technologies. Different processes have been proposed to explain the initiation and release of CMEs from solar active regions (ARs), without reaching consensus on which is the predominant scenario, and thus rendering impossible to accurately predict when a CME is going to erupt from a given AR. To investigate AR magnetic properties that favor CMEs production, we employ multi-spacecraft data to analyze a long duration AR (NOAA 11089, 11100, 11106, 11112 and 11121) throughout its complete lifetime, spanning five Carrington rotations from July to November 2010. We use data from the Solar Dynamics Observatory to study the evolution of the AR magnetic properties during the five near-side passages, and a proxy to follow the magnetic flux changes when no magnetograms are available, i.e. during far-side transits. The ejectivity is studied by characterizing the angular widths, speeds and masses of 108 CMEs that we associated to the AR, when examining a 124-day period. Such an ejectivity tracking was possible thanks to the multi-viewpoint images provided by the Solar-Terrestrial Relations Observatory and Solar and Heliospheric Observatory in a quasi-quadrature configuration. We also inspected the X-ray flares registered by the GOES satellite and found 162 to be associated to the AR under study. Given the substantial number of ejections studied, we use a statistical approach instead of a single-event analysis. We found three well defined periods of very high CMEs activity and two periods with no mass ejections that are preceded or accompanied by characteristic changes in the AR magnetic flux, free magnetic energy and/or presence of electric currents. Our large sample of CMEs and long term study of a single AR, provide further evidence relating AR magnetic activity to CME and Flare production.