Spectroscopic Measurement of Coronal Compositions

Although the elemental composition in all parts of the solar photosphere appears to be the same this is clearly not the case with the solar upper atmosphere (SUA). Spectroscopic studies show that in the corona elemental composition along solar equatorial regions is usually different from polar regions; composition in quiet Sun regions is often different from coronal hole and active region compositions and the transition region composition is frequently different from the coronal composition along the same line of sight. In the following two issues are discussed. The first involves abundance ratios between the high-FIP O and Ne and the low-FIP Mg and Fe that are important for meaningful comparisons between photospheric and SUA compositions and the second involves a review of composition and time variability of SUA plasmas at heights of 1.0≤h≤1.5R _⊙.     

30CrMnSiA钢连接座超塑性等温精锻技术的研究

 <正> 超塑性等温锻造作为新工艺自70年代以来,已在航空航天、机械电子、轻工行业等得到推广应用。长时间内,国内主要在钛合金、铝合金等工业材料上开展了成形研究和应用。本文则对高强度30CrMnSiA钢连接座件进行了超塑性等温成形工艺试验,并在钢的超细化预处理和变形中组织结构变化等研究的基础上进行成形工艺的研究。     

Effect of areal expansion and coronal heating on the solar wind

Empirical studies have shown that the solar wind speed at Earth is inversely correlated with the areal expansion rate of magnetic flux tubes near the Sun. Recent model calculations that include a self-consistent determination of the coronal temperature allow one to understand the physical basis of this relationship; they also suggest why the solar wind mass flux is relatively constant.     

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.     

液体火箭爆炸后有毒气体扩散研究

提出了液体推进剂火箭爆炸后残余推进剂蒸发形成的有毒气体在大气中扩散的解析模型,并数值模拟了地面有毒气体浓度场在不同的环境,天气情况下的分布情况及环境参数对毒气扩散过程影响的分析,能为工程应用提供实用的数据。     

Small scale structures in the solar corona

The observational characteristics of the small scale magnetic structures are summarized. The temperature structure and temporal variability of the emission from coronal bright points, that pervade the source region of the solar wind in coronal holes and the quiet sun, and from active regions are shown to be remarkably similar. Particular emphasis is given to observations, potentially feasible with SOHO, that could resolve some of the outstanding issues regarding the role of the small scale magnetic structures in the energy balance and properties of the solar wind.     

对气液二相流音速的进一步研究

测量小药量电雷管爆炸压力波的传播速度,再修正到音速。结果表明:气液二相流音速比单相液体或空气介质低得多,流动机构对音速变化有显著影响。对低气泡率泡状流,音速与均匀流模型导出的结论相一致。随气泡率增加,流动机构改变时,音速值变化很大。     

Solar Models with Non-Standard Chemical Composition

The OPAL monochromatic opacity tables are used to evaluate the impact of a non-standard chemical composition on solar models. A calibrated solar model with consistent diffusion including the effect of radiative forces and ionization on drift velocities is presented. It is shown that surface abundances are predicted to change slightly more than in traditional solar models where these refinements are not included. All elements included in the model settle at similar rates which is reflected in the relative variation in surface abundances ranging from 7.5% for calcium to 8.8% for argon. The structural difference between the consistent model and the traditional model is small, with a maximum effect of 0.3% for the isothermal sound speed at the base of the convection zone. The settling of CNO is only marginally affected. Opacity profiles have also been calculated with varying abundances for volatile elements, for which the abundances are poorly known, and other selected elements. It is shown that if one allows a 10% variation of these elements individually one can expect a peak Rosseland mean opacity variation of 3% for oxygen, a little less 2% for Si and Ne, and around 1% for Mg and S in the radiative zone. Other light metals and volatile elements have no significant impact on the opacity. This revised version was published online in June 2006 with corrections to the Cover Date.     

Coronal Heating by Magnetic Explosions

From magnetic fields and coronal heating observed in flares, active regions, quiet regions, and coronal holes, we propose that exploding sheared core magnetic fields are the drivers of most of the dynamics and heating of the solar atmosphere, ranging from the largest and most powerful coronal mass ejections and flares, to the vigorous microflaring and coronal heating in active regions, to a multitude of fine-scale explosive events in the magnetic network, driving microflares, spicules, global coronal heating, and, consequently, the solar wind. This revised version was published online in June 2006 with corrections to the Cover Date.     

The scientific payload of the space-based Solar and Heliospheric Observatory (SOHO)

The space-based Solar and Heliospheric Observatory (SOHO) is a joint venture of ESA and NASA within the frame of the Solar Terrestrial Science Programme (STSP), the first Cornerstone of ESA's long-term programme Space Science — Horizon 2000. The principal scientific objectives of the SOHO mission are: a) a better understanding of the structure and dynamics of the solar interior using techniques of helioseismology, and b) a better insight into the physical processes that form and heat the Sun's corona, maintain it and give rise to its acceleration into the solar wind. To achieve these goals, SOHO carries a payload consisting of 12 sets of complementary instruments which are briefly described here.     

采用线膨胀系数可控ZrO2-TiO2陶瓷模具的钛合金高精度超塑成形

对线膨胀系数可控的ZrO2-TiO2陶瓷模具及钛合金高精度超塑成形进行了系统研究。探讨了TiO2体积分数和相对密度对ZrO2-TiO2陶瓷的线膨胀系数的影响规律,并引入相对密度修正模型——Turner模型来准确预测复合陶瓷材料的线膨胀系数。采用压痕法检测了与TC4钛合金等膨胀系数的ZrO2-TiO2陶瓷模具的超塑成形精度。在925℃下,利用ZrO2-TiO2陶瓷模具进行超塑成形,其使用性能良好。结果表明:ZrO2-TiO2陶瓷的线膨胀系数随TiO2体积分数的增加而减小,随相对密度的增加而增加。采用线膨胀系数优化的ZrO2-TiO2陶瓷模具,成形精度误差大幅降低,不超过0.1%,且陶瓷模具具有足够的热机械性能进行超塑成形,使用性能优良。     

FIP Effect in the Solar Upper Atmosphere: Spectroscopic Results

Recent spectroscopic measurements from instruments on the Solar and Heliospheric Observatory (SOHO) find that the coronal composition above a polar coronal hole is nearly photospheric. However, similar SOHO observations show that in coronal plasmas above quiet equatorial regions low-FIP elements are enhanced by a factor of ≈ 4. In addition, the process of elemental settling in coronal plasmas high above the solar surface was shown to exist. Measurements by the Ulysses spacecraft, which are based on non-spectroscopic particle counting techniques, show that, with the exception of He, the elemental composition of the fast speed solar wind is similar to within a factor of 1.5 to the composition of the photosphere. In contrast, similar measurements in the slow speed wind show that elements with low first ionization potential (FIP < 10 eV) are enhanced, relative to the photosphere, by a factor of 4-5. By combining the SOHO and Ulysses results, ideas related to the origin of the slow speed solar wind are presented. Using spectroscopic measurements by the Solar Ultraviolet Measurement of Emitted Radiation (SUMER) instrument on SOHO the photospheric abundance of He was determined as 8.5 ± 1.3% (Y = 0.248). This revised version was published online in June 2006 with corrections to the Cover Date.     

Radio Emissions from Solar Active Regions

Solar active region coronae are known for strong magnetic fields permeating tenuous plasma, which makes them an ideal astronomical laboratory for magnetohydrodynamics research. It is, however, relatively less known that this physical condition also permits a very efficient radiation mechanism, gyro-resonant emission, produced by hot electrons gyrating in the coronal magnetic field. As a resonant mechanism, gyro-emission produces high enough opacity to fully reveal the coronal temperature, and is concentrated at a few harmonics of the local gyrofrequency to serve as an excellent indicator of the magnetic field. In addition, the polarization of the ubiquitous free–free emission and a phenomenon of depolarization due to mode coupling extend the magnetic field diagnostic to a wide range of coronal heights. The ability to measure the coronal temperature and magnetic field without the complications that arise in other radiative inversion problems is a particular advantage for the active region radio emissions available only at these wavelengths. This article reviews the efforts to understand these radiative processes, and use them as diagnostic tools to address a number of critical issues involved with active regions.     

Coronal plumes and fine scale structure in high speed solar wind streams

We present a solar wind model which takes into account the possible origin of fast solar wind streams in coronal plumes. We treat coronal holes as being made up of essentially 2 plasma species, denser, warmer coronal plumes embedded in a surrounding less dense and cooler medium. Pressure balance at the coronal base implies a smaller magnetic field within coronal plumes than without. Considering the total coronal hole areal expansion as given, we calculate the relative expansion of plumes and the ambient medium subject to transverse pressure balance as the wind accelerates. The magnetic flux is assumed to be conserved independently both within plumes and the surrounding coronal hole. Magnetic field curvature terms are neglected so the model is essentially one dimensional along the coronal plumes, which are treated as thin flux-tubes. We compare the results from this model with white-light photographs of the solar corona and in-situ measurements of the spaghetti-like fine-structure of high-speed winds.     

Artificial equilibrium points and bi-impulsive maneuvers to observe 243 Ida

In the restricted three-body problem, the traditional Lagrange points L₁ and L₂ are the only equilibrium points near the asteroid 243 Ida. The thrust generated by a solar sail over a spacecraft enables the existence of new artificial equilibrium points, which depend on the position of the spacecraft with respect to the asteroid and the attitude of the solar sail. Such equilibrium points generate new spots to observe the body from above or below the plane of motion. Such points are very good observational locations due to their stationary condition. This work provides a preliminary analysis to observe Ida through the use of artificial equilibrium points as spots combined with transfer maneuvers between them. Such combination can be used to observe the asteroid from more different points of view in comparison to fixed ones. The analyses are made for a spacecraft equipped with a solar sail and capable of performing bi-impulsive maneuvers. The solar radiation pressure is used both to maintain the equilibrium condition and to reduce the costs of the transfers and/or to create transfers with longer duration. This is a new aspect of the present research, because it combines the continuous thrust with initial and final small impulses, which are feasible for most of the spacecraft, because the magnitudes of the impulses are very low. These combined maneuvers may reduce the transfer times of the maneuvers in most of the cases, compared with the maneuvers based only on continuous thrust. Several options involved in these transfers are shown, like to minimize the fuel spent ($\mathrm{\Delta }\mathit{v}$) as a function of the transfer time or to extend the duration of the travel between the points. Extended transfer times can be useful when observations are required during the transfers.     

基于MATLAB某型飞机航空直流供电保护研究

在机载直流供电系统保护中,广泛使用的保护装置有熔断器（保险丝）和热断路器（双金属自动开关）,其原因是它们结构简单,且满足航空输配电保护的要求。但是它们本身具有诸多不可克服的缺点,例如熔断器缺乏较集中的过载保护特性且特性不稳定,影响到过载保护的可靠性、熔断时有因过热而爆炸的可能性、部分熔断器因安装位置导致不能目视检查熔断情况及熔断器熔断后在飞行时更新难于操作等等。鉴于这些问题,在过流大、易短路的供电主干线路中使用高可靠性、高稳定性、操作简便、自动化程度高的保护装置对提高飞机供电系统可靠性具有重要意义。提出了某型飞机供电保护方案,在MATLAB平台上实现了模拟仿真,结果表明能够有效地解决线路的短路、过载等故障。     

基于APDL的ABS材料FDM-3D打印温度场有限元分析

通过编写APDL命令流,结合ANSYS系统中的"单元生死"技术,动态模拟并仿真了ABS材料在打印过程中温度场的分布,经分析后可以明显看出在不同时刻整体温度场的分布情况,确定温度变化波动范围,温差较大的位置,并结合温度场的云图分析结果确定应力分布不平稳位置,明确Z向不能作为精基准平面。     

反应等离子喷涂Fe-Ti-C复合粉末制备金属陶瓷涂层的组织形成机理

以蔗糖为碳的前驱体、TiFe粉为原料制备Fe-Ti-C系反应热喷涂复合粉末,通过等离子喷涂沉积TiC/Fe金属陶瓷涂层,利用"淬熄试验"研究涂层组织形成机理.采用XRD和SEM分析喷涂粉末、涂层以及淬熄粒子的组织结构.结果表明:每个复合粉末团粒构成独立的反应单元,在喷涂飞行过程中首先出现Ti-Fe液相,然后整个团粒发生球化;熔化的团粒内部生成大量细小TiC颗粒,表层有少量TiC聚集,与基板碰撞后形成复合强化片层与TiC聚集片层交替叠加的涂层结构;随飞行距离增大,团粒外部TiC聚集层增厚,内部TiC颗粒减少,碰撞扁平化程度降低;最终涂层由TiC和Fe两相组成,大量亚微米级TiC颗粒呈内晶型均匀分布于Fe基体中.     

Isotopic Composition of the Solar Wind Inferred from In-Situ Spacecraft Measurements

The Sun is the largest reservoir of matter in the solar system, which formed 4.6 Gyr ago from the protosolar nebula. Data from space missions and theoretical models indicate that the solar wind carries a nearly unfractionated sample of heavy isotopes at energies of about 1 keV/amu from the Sun into interplanetary space. In anticipation of results from the Genesis mission’s solar-wind implanted samples, we revisit solar wind isotopic abundance data from the high-resolution CELIAS/MTOF spectrometer on board SOHO. In particular, we evaluate the isotopic abundance ratios ¹⁵N/¹⁴N, ¹⁷O/¹⁶O, and ¹⁸O/¹⁶O in the solar wind, which are reference values for isotopic fractionation processes during the formation of terrestrial planets as well as for the Galactic chemical evolution. We also give isotopic abundance ratios for He, Ne, Ar, Mg, Si, Ca, and Fe measured in situ in the solar wind.