The evolution of a complex solar radio burst corresponding to special configuration of microwave sources

A complex radio burst associated with periodic (∼1 and 6 min) pulsations and several kinds fine structures, e.g., normal- and reverse-drifting type III bursts, zebra patterns, and slowly drifting structure was observed with the radio spectrometers (1.0–2.0, 2.6–3.8, 5.2–7.6, and 0.65–1.5 GHz) at the National Astronomical Observatories of China (NAOC) in Beijing and Yunnan on 19 October 2001. In combination with the images of 17 and 34 GHz from NoRH and the magnetograms from MDI we reveal the existence and evolution of preexisting and new emerging sources, and find the horseshoe-shaped structure of microwave sources intensity during the late phase of the burst. Through the detailed comparison of the evolution of each source with the time profiles of radio bursts corresponding to these sources we indicate that the intimate correlation between the microwave sources evolution and the generation of the radio burst associated fine structures. Some fine structures can be considered as the MHD turbulence and plasma emission mechanism, based on the anisotropic beam instability and hybrid waves generations. From the characteristics of observations we may presume that the coronal magnetic structures should contain an extended coronal loop system and multiple discrete electrons acceleration/injection sites. The mechanisms of this complex radio burst are deal with the incoherent gyrosynchrotron emission from the trapped electrons and the coherent plasma emission from the non trapped electrons.     

Multiple wavelength observations of flaring active regions

We present observations of flaring active regions with the Very Large Array (V.L.A. at 6 cm and 20 cm wavelengths) and the Westerbork Synthesis Radio Telescope (W.S.R.T. at 6 cm wavelength). These are compared with photospheric magnetograms (Meudon) and with Hα and offband Hα photographs (Big Bear and Ottawa River Solar Observatories). The 6 cm radiation of these active regions marks the legs of dipolar loops which have their footpoints in lower-lying sunspots. The intense, million degree radiation at 6 cm lies above sunspot umbrae in coronal regions where the longitudinal magnetic field strength H_? = 600 Gauss and the height above the sunspot umbrae h = 3.5±0.5 × 10⁹ cm. Circularly polarized horseshoe structures at 6 cm ring the sunspot umbrae. The high degree of circular polarization (?_c = 95%) of the horseshoes is attributed to gyroresonant emission above sunspot^? penumbrae. The 20 cm radiation of these active regions exhibits looplike coronal structures which extend across regions of opposite magnetic polarity in the underlying photosphere. The 20 cm loops are the radio wavelength counterparts of the X-ray coronal loops. We infer semilengths L = 5 × 10⁹ cm, maximum electron temperatures T_e(max) = 3 × 10⁶ K, emission measures ∫N_e²d$\text{l}$ = 10²⁸ cm^?5, and electron densities N_e = 10⁹ cm^?3 (or pressures p = 1 dyn cm^?2) for the 20 cm bremsstrahlung. A total of eight solar bursts were observed at 6 cm or 20 cm wavelength with second-of-arc angular resolution. The regions of burst energy were all resolved with angular sizes between 5″ and 30″, brightness temperatures between 2 × 10⁷ K and 2 × 10⁸ K, and degrees of circular polarization between 10% and 90%. The impulsive phase of the radio bursts are located near the magnetic neutral lines of the active regions, and between the flaring Hα kernels which mark the footpoints of magnetic loops. In one case there was preburst heating in the coronal loop in which a burst occurred. Snapshot maps at 10 s intervals reveal interesting burst evolution including rapid changes of circular polarization and an impulsive burst which was physically separated from both the preburst radio emission and the gradual decay phase of the burst.     

On the impulsiveness of the Hα emission from a flaring atmosphere

Emissions from solar flares may reveal fast fluctuations, which can be attributed to small-scale injections of energetic electrons. In this paper, we perform numerical calculations of the Hα emission from a flaring atmosphere bombarded by a pulsating electron beam. We assume that the variation of the electron beam flux consists of two components: a fluctuation component and a background component. The results show that the amplitude of Hα fluctuations varies depending on the magnitude of the background flux of the electron beam. In the case of a higher background flux, the Hα fluctuations are more significant than in the case of a lower background flux. This result is compatible with the observations in which the Hα fluctuations appear preferentially near the hard X-ray maximum.     

The spatial distributions of the sources of UV solar Explosive Events at different velocities

We analyze five solar Explosive Events observed in the Si iv emission line at 139.37 nm during SUMER/SoHO raster scans near disk center. The Doppler velocities from −45 km s⁻¹ to +45 km s⁻¹ were sorted into eleven symmetrically organized velocity bins, five equally-sized bins on each side and one bin for the line at rest. The radiance values along the NS oriented slit around the maximum of each EE are used to build one-dimensional distributions. We study these distributions and their development in space and time for different velocity bins to unveil the 3D-structure and evolution of Explosive Events. The spatial radiance distributions for the EE maximum and around it were made. For some Explosive Events the dispersion direction is not oriented orthogonally to the slit direction; consequently, the blueshifted emission is in a linear way offset from the redshifted emission by several pixels. The largest offset (∼5″) is observed between distributions whose velocities differ by ∼36 km s⁻¹. The linear relation agrees with an scenario of flows inside magnetic arcs.     

X-ray flaring activity of flare stars and RS CVn binaries

In recent times, X-ray flares have been observed in several flare stars and RS CVn binaries. From an analysis of the X-ray flare observations we find a correlation between the average energy emitted in the X-ray band in flares and the bolometric luminosity of the stars. This relation is similar to the relation obtained in the optical band specifically for the flare stars and hence we suggest a similarity in the flaring nature of the flare stars and the RS CVn binaries. Further, a correlation is also found between the X-ray flare decay time and the peak X-ray luminosity for the flare stars and the RS CVn binaries. We show that this relation can be explained by the solar flare loop models.     

Exosat observations of quiescent and flaring emission from active late-type stars

We present the highlights of several Guest Investigator programs carried out with the EXOSAT satellite. We discuss quiescent as well as flaring emission from normal F to M dwarfs, from dMe flare stars and from RS CVn binaries.     

Converging motion of conjugate flaring kernels during two large solar flares

In this paper, we analyze the footpoint motion of two large solar flares using observations made by the Transition Region and Coronal Explorer (TRACE) and Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). The two flares are the M5.7 flare of March 14, 2002 and the X10 flare of October 29, 2003. They are both classical two-ribbon flares as observed in TRACE 1600 or 171 Å images and have long-duration conjugate hard X-ray (HXR) footpoint emission. We use the ‘center-of-mass’ method to locate the centroids of the UV/EUV flare ribbons. The results are: (1) The conjugate UV/EUV ribbons and HXR footpoints of the two flares show a converging (inward) motion during the impulsive phase. For the two flares, the converging motion lasts about 3 and 10 min, respectively. The usual separation (outward) motion for the flare ribbons and footpoints take place only after the converging motion. (2) During the inward and the outward motion, the conjugate ribbons and footpoints of the two events exhibit a strong unshear motion. In obtaining above results, TRACE UV/EUV and RHESSI HXR data show an overall agreement. The two events demonstrate that the magnetic reconnection for the flares occurs in highly sheared magnetic field. Furthermore, the results support the magnetic model constructed by Ji et al. [Ji, H., Huang, G., Wang, H. Astrophys. J. 660, 893–900, 2007], who proposed that the contracting motion of flaring loops is the signature of the relaxation of sheared magnetic fields.     

Energy sources for the ionosphere—a survey

An outline is given of early aeronomical ideas about the formation of the ionosphere by solar wave radiation, and its development under the impetus of increasing basic knowledge. In particular, the development concerning solar radiation in the far ultraviolet and X-ray ranges is discussed (Sect. 1). General considerations on the relation with observable ionospheric parameters are given in Sect. 2 while the individual layers are discussed in Sect. 3. It is found that elder investigations, with wrong assumptions came to the right densities while their estimates of production rates were far too low. Since two years only satellite and laboratory data allow satisfying estimates.     

Conditions for the onset of temperature oscillations in a simulated floating-zone configuration

The floating-zone method for crystal growth is studied in simulated low-gravity conditions by suspending a drop of fluid vertically between two circular rods and heating the upper rod with a heater. Flow and temperature oscillations are observed under certain conditions. The temperature oscillation level and the oscillation frequency are measured against the Marangoni number for several aspect ratios using hexadecane and Fluorinert as the test fluids. It is observed that, contrary to what has been believed, the Marangoni number is not the proper parameter to describe the onset of oscillation.     

Evaluation of a combined electrostatic and magnetostatic configuration for active space-radiation shielding

Developing successful and optimal solutions to mitigating the hazards of severe space radiation in deep space long duration missions is critical for the success of deep-space explorations. A recent report (Tripathi et al., 2008) had explored the feasibility of using electrostatic shielding. Here, we continue to extend the electrostatic shielding strategy and examine a hybrid configuration that utilizes both electrostatic and magnetostatic fields. The main advantages of this system are shown to be: (i) a much better shielding and repulsion of incident ions from both solar particle events (SPE) and galactic cosmic rays (GCR), (ii) reductions in the power requirement for re-charging the electrostatic sub-system, and (iii) low requirements of the magnetic fields that are well below the thresholds set for health and safety for long-term exposures. Furthermore, our results show transmission levels reduced to levels as low as 30% for energies around 1000 MeV, and near total elimination of SPE radiation by these hybrid configurations. It is also shown that the power needed to replenish the electrostatic charges due to particle hits from the GCR and SPE radiation is minimal.     

Transient growth effects during space solidification experiments in a Bridgman configuration

This paper reviews the different mechanisms involved during a Bridgman solidification. It is demonstrated that during a space experiment, due to the lack of time it is not possible to wait for steady states for all the phenomena considered. So a non steady state analysis is needed. Mass and heat transfers are considered as well as kinetics effects. Different coupling effects are emphasized. It is shown that fine measurements during space experiments are needed in order to verify these important transient stages. One kind of possible experiments is proposed to enable us a better understanding of the solidification laws.     

Multi-wavelength study of the short term TeV flaring activity from the blazar Mrk 501 observed in June 2014

In this work, we study the short term flaring activity from the high synchrotron peaked blazar Mrk 501 detected by the FACT and H.E.S.S. telescopes in the energy range 2–20 TeV during June 23–24, 2014 (MJD 56831.86–56831.94). We revisit this major TeV flare of the source in the context of near simultaneous multi-wavelength observations of $\gamma$–rays in MeV-GeV regime with Fermi-LAT, soft X-rays in 0.3–10 keV range with Swift-XRT, hard X-rays in 10–20 keV and 15–50 keV bands with MAXI and Swift-BAT respectively, UV-Optical with Swift-UVOT and 15 GHz radio with OVRO telescope. We have performed a detailed temporal and spectral analysis of the data from Fermi-LAT, Swift-XRT and Swift-UVOT during the period June 15–30, 2014 (MJD 56823–56838). Near simultaneous archival data available from Swift-BAT, MAXI and OVRO telescope along with the V-band optical polarization measurements from SPOL observatory are also used in the study of giant TeV flare of Mrk 501 detected by the FACT and H.E.S.S. telescopes. No significant change in the multi-wavelength emission from radio to high energy $\gamma$–rays during the TeV flaring activity of Mrk 501 is observed except variation in soft X-rays. The varying soft X-ray emission is found to be correlated with the $\gamma$–ray emission at TeV energies during the flaring activity of the source. The soft X-ray photon spectral index is observed to be anti-correlated with the integral flux showing harder-when-brighter behavior. An average value of 4.5$\%$ for V-band optical polarization is obtained during the above period whereas the corresponding electric vector position angle changes significantly. We have used the minimum variability timescale from the H.E.S.S. observations to estimate the Doppler factor of the emission region which is found to be consistent with the previous studies of the source.     

基于一种匹配函数的ATS资源自动配置方法

提出采用匹配函数描述测试点与仪器端口的匹配程度,用来指导自动测试系统仪器选型和资源配置.匹配函数采用面向信号的方法构建,综合了测点信号属性与仪器性能参数、仪器可靠性、仪器成本、仪器操作复杂度等因素,使得仪器选型和资源配置策略的制定更符合工程需要.给出了资源配置策略和算法,并对资源配置进行了并行测试优化.通过给出一个典型实例,证明该方法能有效降低测试成本,增强系统可靠性,提高测试效率和吞吐量,并为自动测试系统硬件设计的自动化奠定了基础.      

飞机构型管理研究与应用

为了满足现代飞机复杂化、多元化和系列化的要求,保证在飞机数字化设计制造过程中产品数据的一致性、完整性和可追踪性,借鉴波音公司简化构型管理的思想,研究了飞机构型管理和控制的过程,强调构型管理技术在飞机研制的整个生命周期过程中的重要性,明确了构型管理的基本定义,区别了物料清单BOM(Bill Of Material)视图--工程BOM、工艺BOM、制造BOM等与构型之间的关系,指出并分析了飞机构型管理和控制的4项关键技术,即将基于图纸的构型管理变为基于零部件的构型管理;模块化组织飞机产品结构单元;简化有效性管理,通过模块有效性控制飞机产品构型;强化版本的控制.并针对这4项关键技术给出实际的应用解决方案.     

雷达与IFF背靠背配置时的关联算法

对于雷达与IFF(Identification Friend or Foe)背靠背配置时的关联问题,提出了关联算法.主要包括雷达航迹与IFF点迹的时间对准、判别函数构造、关联判决准则选择和关联判决门限设置等,并讨论了多义性问题.4种典型情况下的仿真结果表明,目标间隔与目标到雷达距离之比越大时,关联效果越好;目标交叉时,离交叉点越近,关联效果越差;目标机动阶段时间对准采用雷达航迹平滑的关联效果优于航迹预测,其它情况下采用两种时间对准方法的关联效果相近;在NED(North East Down)坐标系和极坐标系下的关联效果相近;n/m逻辑应选择2/3或3/4,以同时保证对友方目标的漏关联概率和不明目标的误关联概率都较低.     

一种非线性鲁棒PID控制器设计方法

针对一类非线性不确定系统,提出了一种基于PID(比例-积分-微分)控制的鲁棒控制方法.整个控制器由PID控制器和一个鲁棒补偿器构成.首先,基于系统的标称模型设计PID控制器;然后在PID控制的基础上,设计一个辅助鲁棒补偿器,用于补偿系统非线性、参数摄动和外界扰动等对系统控制性能的影响.补偿器的设计基于李雅普诺夫(Lyapunov)稳定性理论进行,从而保证了闭环系统的鲁棒稳定.采用该方法对倒立摆跟踪问题进行了仿真控制,仿真结果验证了设计方案的有效性.     

一类非线性时滞系统的采样控制

针对于采样区间具有已知上界的非线性时滞系统,分别考虑了常采样和变采样两种情况下的采样控制问题.目标是设计一个状态反馈采样控制器,使得闭环系统指数稳定,并且满足给定的性能指标.基于输入延迟方法,可以将采样控制系统转化成具有时变延迟的连续系统.引入了新的时间依赖Lyapunov函数,这些Lyapunov函数在下一个采样时间到来之前没有增长.以线性矩阵不等式(LMI, Linear Matrix Inequality)的形式给出了具有时变延迟的非线性扰动系统指数稳定的充分条件.仿真结果说明了所提方法可以提高系统的抗扰能力.     

Constraints on a hadronic model for unidentified off-plane galactic gamma-ray sources

Recently the H.E.S.S. collaboration announced the detection of an unidentified gamma-ray source with an off-set from the galactic plane of 3.5°: HESS J1507-622. If the distance of the object is larger than about one kpc it would be physically located outside the galactic disk. The density profile of the ISM perpendicular to the galactic plane, which acts as target material for hadronic gamma-ray production, drops quite fast with increasing distance. This fact places distance dependent constraints on the energetics and properties of off-plane gamma-ray sources like HESS J1507-622 if a hadronic origin of the gamma-ray emission is assumed. For the case of this source it is found that there seems to be no simple way to link this object to the remnant of a stellar explosions.     

Nature of gamma-ray burst sources

Observational evidence suggests that gamma ray bursts have a local galactic origin involving neutron stars. In this light we make a critical review of physics of the thermonuclear runaway model placing emphasis on self-consistency. We further show that some of the proposed models can be observationally excluded in the light of existing data from the Einstein Observatory. The possibility of gamma bursts arising in low mass binaries is finally discussed in the light of evolutionary scenarios leading to low luminosity systems.