Coronal radio-sounding detection of a CME during the 1997 Galileo solar conjunction

Frequency fluctuations of the Galileo S-band radio signal were recorded nearly continuously during the spacecraft’s solar conjunction from December 1996 to February 1997. A strong propagating disturbance, most probably associated with a coronal mass ejection (CME), was detected on 7 February when the radio ray path proximate point was on the west solar limb at about 54 solar radii from the Sun. The CME passage through the line of sight is characterized by a significant increase in the fluctuation intensity of the recorded frequency and by an increase in the plasma speed from about 234 km s⁻¹ up to about 755 km s⁻¹. These velocity estimates are obtained from a correlation analysis of frequency fluctuations recorded simultaneously at two widely-separated ground stations. The density turbulence power spectrum is found to steepen behind the CME front. The Galileo radio-sounding data are compared with SOHO/LASCO observations of the CME in the corona and with WIND spacecraft data near the Earth’s orbit.     

Interplanetary Physics Research in China:2006—2008

This brief report summarized the latest advances of the interplanetary physics research in China during the period of 2006—2007,made independently by Chinese space physicists and through international collaboration.The report covers all aspects of the interplanetary physics,including theoretical studies,numerical simulation and data analysis.     

Solar Sources of Heliospheric Energetic Electron Events—Shocks or Flares?

Electrons with near-relativistic (E≳30 keV, NrR) and relativistic (E≳0.3 MeV) energies are often observed as discrete events in the inner heliosphere following solar transient activity. Several acceleration mechanisms have been proposed for the production of those electrons. One candidate is acceleration at MHD shocks driven by coronal mass ejections (CMEs) with speeds ≳1000 km s⁻¹. Many NrR electron events are temporally associated only with flares while others are associated with flares as well as with CMEs or with radio type II shock waves. Since CME onsets and associated flares are roughly simultaneous, distinguishing the sources of electron events is a serious challenge. On a phenomenological basis two classes of solar electron events were known several decades ago, but recent observations have presented a more complex picture. We review early and recent observational results to deduce different electron event classes and their viable acceleration mechanisms, defined broadly as shocks versus flares. The NrR and relativistic electrons are treated separately. Topics covered are: solar electron injection delays from flare impulsive phases; comparisons of electron intensities and spectra with flares, CMEs and accompanying solar energetic proton (SEP) events; multiple spacecraft observations; two-phase electron events; coronal flares; shock-associated (SA) events; electron spectral invariance; and solar electron intensity size distributions. This evidence suggests that CME-driven shocks are statistically the dominant acceleration mechanism of relativistic events, but most NrR electron events result from flares. Determining the solar origin of a given NrR or relativistic electron event remains a difficult proposition, and suggestions for future work are given.     

带迎角钨杆斜侵彻铝板数值仿真研究

为研究迎角对钨杆斜侵过程的影响,开展了带迎角钨杆斜侵彻铝板数值仿真研究。仿真中采用SPH方法,Shock状态方程和Steinberg本构模型。钨杆共有两种尺寸,分别为Φ10mm×23mm和Φ10mm×46mm。铝板厚10mm,撞击速度为2km/s,撞击角度为60°。为简化分析,将迎角分解为俯仰角和偏航角,其中俯仰角范围为-90°～90°,偏航角范围为0°～90°。对钨杆侵彻过程的分析结果表明：斜侵彻存在临界迎角,在临界迎角范围内钨杆所受力矩可忽略不计;在临界迎角范围外,钨杆将发生弯曲甚至折断。对钨杆的剩余质量分析结果表明：当偏航角为0°且钨杆未折断时,剩余质量只在较小的范围内变化;当俯仰角为0°时,剩余质量随迎角增加线性减小。对钨杆的剩余速度分析结果表明：偏航角对剩余速度的影响与俯仰角对剩余速度的影响基本一致,剩余速度曲线关于0°迎角基本对称。根据仿真结果,采用曲线拟合的方法给出了钨杆斜侵彻铝板的剩余速度经验公式。     

一种直升机自旋训练过程涡轴发动机控制规律设计与仿真

针对直升机自旋训练过程中涡轴发动机快速响应要求,提出了一种以燃油流量和导叶角为控制量的鲁棒控制规律抑制自由涡轮转速瞬态下垂.首先,通过改进UH-60直升机/T700发动机综合模型,使之能够模拟自旋进入及自旋恢复过程动态变化.其次,提出并设计一种基于燃油流量和导叶调节的涡轴发动机鲁棒控制规律,并通过典型的自旋训练过程仿真,验证了该控制规律相比仅以燃油流量为变量的控制规律,自由涡轮转速瞬态下垂量降低至3%以下,且燃油流量变化更加平缓,改善了执行机构的工作条件.     

基于氦质谱检漏仪的飞机机翼整体油箱检漏技术

介绍了氦质谱检漏的原理,基于氦质谱检漏技术,提出面向机翼整体油箱的检漏方案,包括粗漏检测方法和细漏检测方法,在此基础上,开展氦气-航空煤油泄漏对比试验,确定了能够应用于生产的初步标准。     

质量基准研究的最新进展

质量基准是迄今唯一保留人工制品的SI单位.近年来,计量学家通过国际合作,试图基于自然的不变性质、阿佛加德罗常数和普朗克常数的概念重新定义质量基准.     

Space storm measurements of the July 2005 solar extreme events from the low corona to the Earth

The Athens Neutron Monitor Data Processing (ANMODAP) Center recorded an unusual Forbush decrease with a sharp enhancement of cosmic ray intensity right after the main phase of the Forbush decrease on 16 July 2005, followed by a second decrease within less than 12 h. This exceptional event is neither a ground level enhancement nor a geomagnetic effect in cosmic rays. It rather appears as the effect of a special structure of interplanetary disturbances originating from a group of coronal mass ejections (CMEs) in the 13–14 July 2005 period. The initiation of the CMEs was accompanied by type IV radio bursts and intense solar flares (SFs) on the west solar limb (AR 786); this group of energetic phenomena appears under the label of Solar Extreme Events of July 2005. We study the characteristics of these events using combined data from Earth (the ARTEMIS IV radioheliograph, the Athens Neutron Monitor (ANMODAP)), space (WIND/WAVES) and data archives. We propose an interpretation of the unusual Forbush profile in terms of a magnetic structure and a succession of interplanetary shocks interacting with the magnetosphere.     

Modelling and observations of photospheric magnetic helicity

Mounting observational evidence of the emergence of twisted magnetic flux tubes through the photosphere have now been published. Such flux tubes, formed by the solar dynamo and transported through the convection zone, eventually reach the solar atmosphere. Their accumulation in the solar corona leads to flares and coronal mass ejections. Since reconnections occur during the evolution of the flux tubes, the concepts of twist and magnetic stress become inappropriate. Magnetic helicity, as a well preserved quantity, in particular in plasma with high magnetic Reynolds number, is a more suitable physical quantity to use, even if reconnection is involved.     

Viewing radiation signatures of solar energetic particles in interplanetary space

A current serious limitation on the studies of solar energetic particle (SEP) events is that their properties in the inner heliosphere are studied only through in situ spacecraft observations. Our understanding of spatial distributions and temporal variations of SEP events has come through statistical studies of many such events over several solar cycles. In contrast, flare SEPs in the solar corona can be imaged through their radiative and collisional interactions with solar fields and particles. We suggest that the heliospheric SEPs may also interact with heliospheric particles and fields to produce signatures which can be remotely observed and imaged. A challenge with any such candidate signature is to separate it from that of flare SEPs. The optimum case for imaging high-energy (E > 100 MeV) heliospheric protons may be the emission of π⁰-decay γ-rays following proton collisions with solar wind (SW) ions. In the case of E > 1 MeV electrons, gyrosynchrotron radio emission may be the most readily detectible remote signal. In both cases we may already have observed one or two such events. Another radiative signature from nonthermal particles may be resonant transition radiation, which has likely already been observed from solar flare electrons. We discuss energetic neutrons as another possible remote signature, but we rule out γ-ray line and 0.511 MeV positron annihilation emission as observable signatures of heliospheric energetic ions. We are already acquiring global signatures of large inner-heliospheric SW density features and of heliosheath interactions between the SW and interstellar neutral ions. By finding an appropriate observable signature of remote heliospheric SEPs, we could supplement the in situ observations with global maps of energetic SEP events to provide a comprehensive view of SEP events.