New evidence for strong non-thermal effects in Tycho’s supernova remnant

For the case of Tycho’s supernova remnant (SNR), we present the relation between the blast wave and contact discontinuity radii calculated within the nonlinear kinetic theory of cosmic ray (CR) acceleration in SNRs. It is demonstrated that these radii are confirmed by recently published Chandra measurements which show that the observed contact discontinuity radius is very close to the shock radius. Therefore a consistent explanation of these observations can be given in terms of efficient CR acceleration which makes the medium more compressible.     

Oxygen line mapping of SN 1006 with Suzaku

SN 1006 is one of the supernova remnants (SNRs) with relatively low-temperature electrons, considering the young age of just 1000 years. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) and the Hard X-ray Detector (HXD) onboard Suzaku, the fifth Japanese X-ray satellite. Thanks to the excellent spectral resolution of XIS in the soft X-ray band, H-like and He-like oxygen emission lines were clearly detected, and we could make a map of the line intensity, and as well as a flux and the photon index of nonthermal component. We found that these parameters have spatial dependences from region to region in the SNR; the north region is bright in nonthermal, while dim in thermal; the east region is bright in both nonthermal and thermal; the inner region shows dim nonthermal and bright thermal emission. The photon index is the smallest in the north region.     

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.     

Fe/O Ratios in Interplanetary Shock Accelerated Particles

It is widely accepted that diffusive shock acceleration is an important process in the heliosphere, in particular in producing the energetic particles associated with interplanetary shocks driven by coronal mass ejections. In its simplest formulation shock acceleration is expected to accelerate ions with higher mass to charge ratios less efficiently than those with lower mass to charge. Thus it is anticipated that the Fe/O ratio in shock-accelerated ion populations will decrease with increasing energy above some energy. We examine the circumstances of five interplanetary shocks that have been reported to have associated populations in which Fe/O increases with increasing energy. In each event, the situation is complex, with particle contributions from other sources in addition to the shock. Furthermore, we show that the Fe/O ratio in shock-accelerated ions can decrease even when the shock is traveling through an Fe-rich ambient ion population. Thus, although shock acceleration of an Fe-rich suprathermal population has been proposed to explain large Fe-rich solar particle events, we find no support for this proposal in these observations.     

Theory of fragmented energy release in the Sun

The magnetic energy released inside an active region is closely related to its formation and evolution. Following the evolution of a collection of flux tubes inside the convection zone and above the photosphere we can show that many nonlinear structures (current sheets, shock waves, double layers etc.) are formed. We propose in this review that coronal heating, flares and particle acceleration are due to the interaction of the plasma with these nonlinear structures. Approaching active regions as a driven complex dynamical system we can show that several coherent ensembles of the nonlinear structures will appear spontaneously. The statistical analysis of these structures is a major problem in solar physics. We can also show that many observed large scale structures are the result of the convolution of non-observable fragmentation in the energy release process.     

Acceleration of interplanetary pick-up ions and anomalous cosmic rays

It may not be doubted anymore that anomalous cosmic rays (ACRs) are produced in the heliosphere from interplanetary pick-up ions through their acceleration at the solar wind termination shock. However, there is no general agreement in the community of heliospheric researchers concerning the mechanism of injection of the pick-up ions into the shock acceleration. We discuss here three possible ways for pick-up ions to be involved into the acceleration process at the termination shock: (1) preacceleration of pick-up ions in the whole region from the Sun up to the termination shock by solar wind turbulences and interplanetary shock waves, (2) local preacceleration of pick-up ions in a vicinity of the termination shock by shock surfing, and (3) formation of high-velocity tails in pick-up ion spectra consisting of secondary pick-up ions which are produced in the supersonic solar wind due to ionization of energetic neutral atoms entering from the inner heliosheath.     

加速度对含铝复合推进剂瞬时燃速的影响

本文研究了加速度向量对含铝复合推进剂瞬时燃速的影响.其中包括加速度大小和方向对推进剂瞬时燃速增加率的影响和在同一加速度条件下铝粉粒径、铝粉含量和铝粉形状对瞬时燃速增加率的影响.此外,还对研究结果进行了分析和讨论.     

基于遗传算法的涡扇发动机多变量加速寻优控制

研究了变几何涡扇发动机不等式约束下的遗传算法最优加速控制规律，在全飞行包线内进行了仿真计算。通过分析多变量变几何涡扇发动机加速过程的特点和性能要求，用离散化加速模型结合遗传算法，使得加速过程最优。仿真计算表明该控制律可以保证变几何涡扇发动机在全飞行包线内稳定工作，且加速时间最短。     

惯导平台式重力测量技术实现及应用

详细阐述了解析方位双轴惯导平台式重力测量的工作原理,并通过基于方位余弦积的惯导力学编排解决了极区工作问题。在常规平台式重力测量数据处理方法的基础上,针对高动态环境提出了基于Kalman滤波的运动扰动修正方法。在此基础上研制了ZL11-1A型国产惯导平台式海洋重力仪。通过与国外主流重力仪产品海上同船作业比对,结果表明,该型重力仪在高海况下测量精度依然优于1mGal,满足重力测量作业要求。     

涡扇发动机全包线加速控制计划改进方法研究

加速控制计划直接影响了发动机的响应速度以及运行安全。为了提高发动机响应能力,提出了一种基于等温度线的发动机全包线加速控制计划。分别针对稳态和动态过程开展相似换算误差分析,证明并验证了关键参数在等风扇进口温度时,具有较高相似换算精度的规律。基于此换算误差理论,提出全包线加速控制计划改进方法,该方法在不同等风扇进口温度下设计多条加速控制计划,再通过线性插值得到包线内不同等温线下的加速控制计划。结果表明,改进后的加速控制计划相比于传统单点优化得到的加速控制计划,发动机加速至最大转速的98%所需的时间减少了7.2%,最大转速提升了1%,且风扇、压气机喘振裕度和涡轮前温度等均未超出限制值。因此,该方法相比于传统单点优化方法既提升了在包线内获取的加速控制计划的精度,又确保了发动机在包线内安全稳定工作的前提下更好的发挥加速性能。