Fractionation of SI, NE, and MG Isotopes in the Solar Wind as Measured by Soho/Celias/MTOF

Using the high-resolution mass spectrometer CELIAS/MTOF on board SOHO we have measured the solar wind isotope abundance ratios of Si, Ne, and Mg and their variations in different solar wind regimes with bulk velocities ranging from 330 km/s to 650 km/s. Data indicate a small systematic depletion of the heavier isotopes in the slow solar wind on the order of (1.4±1.3)% per amu (2σ-error) compared to their abundances in the fast solar wind from coronal holes. These variations in the solar wind isotopic composition represent a pure mass-dependent effect because the different isotopes of an element pass the inner corona with the same charge state distribution. The influence of particle mass on the acceleration of minor solar wind ions is discussed in the context of theoretical models and recent optical observations with other SOHO instruments. This revised version was published online in June 2006 with corrections to the Cover Date.     

利用TDLAS技术评估火箭基组合循环发动机试验性能

针对宽范围工作的火箭基组合循环（RBCC）发动机推力、比冲和燃烧效率等性能难以通过关键参数的实时测量直接计算的问题,提出利用可调谐二极管激光器吸收光谱（TDLAS）技术实现发动机燃气温度、H2O组分浓度和速度多参数同时实时在线非接触式激光光谱测量方法,搭建用于RBCC地面试验性能分析的时分复用-扫描波长TDLAS系统。通过试验获得的(7444.352+7444.371)/7185.597cm -1 谱线附近吸收光谱,从而得到燃气温度、H2O组分浓度和速度参数,并结合数值模拟方法确定的流场参数纵向分布,实现基于关键参数在线测量的发动机性能直接计算。该方法有助于评判燃烧组织和结构改变对发动机性能的影响。     

空间环境对漫反射板的影响

光学系统在空间环境条件下的衰变对卫星遥感仪器探测精度有重要影响.漫反射板是星载光学遥感仪器辐射定标的重要工具.本文通过对ADEOS/TOMS和Earth Probe/TOMS仪器馒反射板漫反射率衰变特性的比较,分析研究了原子氧和太阳紫外辐射对漫反射板的影晌.结果表明,太阳紫外辐照和原子氧剥蚀引起的漫反射板反射率衰变系数分别为0.00049/h和1.2 × 10^-17cm²,但在卫星入轨初期,太阳紫外辐照的影响可增加约4倍.     

碳纤维-环氧树脂波纹梁吸能能力的试验研究

 用试验研究了碳纤维 -环氧树脂圆弧型波纹梁在轴向准静态载荷下的损毁过程、峰值载荷和能量吸收能力。通过 3组不同尺寸的波纹梁在轴向准静态载荷下的压缩试验,研究了波纹梁的缓冲吸能机理,并对波纹梁的峰值载荷和吸能能力做了定量分析,讨论了不同结构尺寸对波纹梁在轴向准静态载荷下的峰值载荷和吸能能力的影响。     

Relativistic proton production at the Sun in the 20 January 2005 solar event

Based on the concept of multiple acceleration of solar energetic particles (SEP) we analyzed the super-event of 20 January 2005 by the data of ground level, balloon and spacecraft observations. The main characteristics of relativistic solar protons (energy spectra, anisotropy directions and pitch-angle distributions) are derived and their dynamics during the event is studied. It is shown that the flux of relativistic solar protons may consist of two distinct components, the so-called prompt and delayed ones. Within a two-source model of particle generation, one of which is associated with an expanding magnetic loop, we solved the transport equation in energy phase space, including adiabatic losses simultaneously with the stochastic acceleration process, and calculate the expected spectra of the delayed component at the source. The confrontation of experimental spectra with theoretical ones shows that the delayed component may be correctly described by stochastic acceleration, but not the prompt component. The required acceleration efficiencies turned out to be rather high, so that, for this particular event, adiabatic cooling is practically negligible. Our results provide a new support to the existence of two populations of relativistic solar protons in some SEP events.     

Dynamic processes in the outer heliosphere: voyager observations and models

We review recent Voyager 2 observations in the vicinity of 70 AU. The character of the solar wind plasma data between 2002 and 2003 changed to a regime in which the speed, density and magnetic field magnitude are positively correlated. The average speed of the solar wind at Voyager 2 increased between early 2003 and mid-2004, which we attribute to a return of fast coronal hole flow. We use solar wind data at Earth as input to numerical models which include the effect of pickup ions to model the radial evolution of the solar wind. The model reproduces the basic features of the observations. As a specific example, we investigate the propagation of the Halloween (Oct.–Nov.), 2003 storms in the outer heliosphere. The model predictions are in reasonable agreement with Voyager 2 observations.     

Estimation of the bias of the Minimum Variance technique in the determination of magnetic clouds global quantities and orientation

Magnetic clouds (MCs) are highly magnetized plasma structures that have a low proton temperature and a magnetic field vector that rotates when seen by a heliospheric observer. More than 25 years of observations of magnetic and plasma properties of MCs at 1 AU have provided significant knowledge of their magnetic structure. However, because in situ observations only give information along the trajectory of the spacecraft, their real 3D magnetic configuration remains still partially unknown. We generate a set of synthetic clouds, exploring the space of parameters that represents the possible orientations and minimum distances of the satellite trajectory to the cloud axis, p. The synthetic clouds have a local cylindrical symmetry and a linear force-free magnetic configuration. From the analysis of synthetic clouds, we quantify the errors introduced in the determination of the orientation/size (and, consequently, of the global magnetohydrodynamic quantities) by the Minimum Variance method when p is not zero.     

太阳微波射电快速精细结构亚类型的观测分析

通过分析"云南天文台4波段太阳射电快速同步观测系统"1990-01-1994－01取得的103个射电爆发,发现其中29个存在不同类型的快速精细结构（FFS）.尤其是发现了几个少见的亚类FFS现象.本文仅介绍两个亚类型：窄带变周期脉动和宽带慢漂移长周期脉动.这些现象表明太阳射电FFS的多样性,它们发生在射电爆发的不同阶段（耀斑不同相）,从而说明在耀斑演化中日冕非热电子的加速或注入可能贯穿于整个耀斑发展过程.由于耀斑后相FFS的发生,可验证耀斑后相存在磁重联和似环结构（耀斑后环）的重新形成.由于不同的亚类FFS反映日冕中存奇特别的环境条件,从而推测日冕中可能存在更复杂的多重类型的磁结构.     

Applications and usage of the real-time Neutron Monitor Database

A high-time resolution Neutron Monitor Database (NMDB) has started to be realized in the frame of the Seventh Framework Programme of the European Commission. This database will include cosmic ray data from at least 18 neutron monitors distributed around the world and operated in real-time. The implementation of the NMDB will provide the opportunity for several research applications most of which will be realized in real-time mode. An important one will be the establishment of an Alert signal when dangerous solar cosmic ray particles are heading to the Earth, resulting into ground level enhancements effects registered by neutron monitors. Furthermore, on the basis of these events analysis, the mapping of all ground level enhancement features in near real-time mode will provide an overall picture of these phenomena and will be used as an input for the calculation of the ionization of the atmosphere. The latter will be useful together with other contributions to radiation dose calculations within the atmosphere at several altitudes and will reveal the absorbed doses during flights. Moreover, special algorithms for anisotropy and pitch angle distribution of solar cosmic rays, which have been developed over the years, will also be set online offering the advantage to give information about the conditions of the interplanetary space. All of the applications will serve the needs of the modern world which relies at space environment and will use the extensive network of neutron monitors as a multi-directional spectrographic detector. On top of which, the decreases of the cosmic ray intensity – known as Forbush decreases – will also be analyzed and a number of important parameters such as galactic cosmic ray anisotropy will be made available to the users of NMDB. A part of the NMDB project is also dedicated to the creation of a public outreach website with the scope to inform about cosmic rays and their possible effects on humans, technological systems and space-terrestrial environment. Therefore, NMDB will also stand as an informative gate on space research through neutron monitor’s data usage.     

Identification of high energy solar particle signals on the Mexico City neutron monitor database

We performed a search for ground level solar cosmic ray enhancements on the full five minute database of the Mexico City neutron monitor using wavelet filters and two different statistical tests. We present a detailed analysis of the time series of November 2, 1992, where we found a previously unreported increment matching the onset time of the impulsive phase of GLE 54, thus providing evidence of an effective detection of high energy solar cosmic rays.