The γ-ray bursts as a result of the proper activity of the neutron star

The model of the Γ-ray burst is developed which is based on the nuclear explosion in the neutron star envelope because of the chain fission reaction of the superheavy nuclei. It is shown, that the main part of the Γ-ray burst radiation must have thermal origin, but the nonthermal component and Γ-ray lines may be present. The parameters of the strong burst of 5 March 1979 are evaluated on the basis of its radiation spectra and the present model. The distance to this burst is about 100 pc and the total energy of this Γ-ray burst is about 2.1039 ergs.     

X射线耀斑的强度指标

本文利用GOES-7卫星的1分钟记录资料研究了1991年3月和6月期间6个大X耀斑伴随的软X射线爆发特性和源强度的关系。结果指出：对X射线耀斑，其射线辐射流量上升快的在日冕中激起的激波速度也较快．数值模拟研究指出，这可能反映爆发能量释放速率是源强度的主要指标．     

磁云边界层内朗缪尔波活动现象的初步研究

对35例磁云边界层内朗缪尔波活动现象进行了初步分析, 发现两类磁云边界层内特有的朗缪尔波活动现象. 一类是相对于邻近鞘区和磁云本体, 整个边界层内朗缪尔波活动增强; 另一类是短时间的朗缪尔波爆发现象, 同时伴随着宽频带的多普勒频移离子声波活动. 考察了其中一例朗缪尔波爆发事件对应的高分辨率电子分布函数数据, 发现速度约为7×103 km/s的电子束流形成尾峰分布不稳定性导致了朗缪尔波的爆发.      

微波爆发前太阳射电发射的周期振荡

本文分析了1979年1月一12月紫台3.2cm、10cm波段上的爆发资料,峰值流量增量ΔS/S≥50%的爆发共计25个,发现所有25个爆发的爆前记录曲线上都存在着周期从几秒一10几秒、振幅约为太阳非扰动分量l%的振荡。这种振荡一般先于爆发几小时或几天。但对于特大爆发,如47GB型爆发,在长时间持续振荡以后,往往在爆前几十分钟或几小时突归宁静,呈平滑记录;对于较小的爆发,脉冲爆或持续期较短的复杂爆,如3S型、20GRF型以及45C型,在振荡同爆发之间不存在记录曲线的宁静时段,而往往由振荡直接延续到爆发。因此微波辐射的这种振荡特性可能是耀斑区域储能过程的一种反映。      

一个日面边缘大爆发的射电观测特性

本文详细列出1981年4月27日0808UT发生的日面边缘大爆发的射电观测特征,并作了有关射电爆发形态及微波频谱、非热电子能谱的初步分析。      

2006年12月13日太阳射电暴对GPS观测的影响

日地空间环境不仅影响航天器运行和安全, 也是导航、定位和通信等无线 电应用系统主要的误差源. 其中来自太阳L波段的射电暴被认为是全球导航卫星 系统(GNSS)稳定和性能的潜在威胁因素, 当L波段射电爆发达到一定阈值时, 将给用户带来不同程度的射电噪声干扰, 严重时会引起接收机失锁和定位服务 中断. 本文对2006年12月13日太阳射电暴对GPS造成的影响进行了研究, 利用太阳射电 观测数据、L波段闪烁观测数据和向阳面不同区域的GPS观测网数据, 分析 GPS观测对射电暴的响应. 结果表明, 此次事件对GPS观测产生了明显的影响, 射 电暴期间GPS发生幅度闪烁事件和明显失锁现象, 多个台站上空的多颗GPS 卫星 信号完全中断长达6min左右, 且多个台站上空锁定的卫星数目小于4颗, 使 得GPS定位完全失效. 相对而言, 射电暴期间日下点附近的GPS台站受到的影响 比远离日下点的大.      

Determination of confidence contours for gamma ray burst source locations

The method for determining gamma-ray burst source regions which has produced the best results until now is long-baseline wavefront triangulation. The direction of the source of the gamma rays is derived from the delay in the arrival time of the burst at widely spaced detectors on at least three spacecraft. An exact method to compute confidence contours for the source error boxes is given in the present paper.     

太阳射电微波爆发的频谱分析

1981年4月1日太阳发生一个4N级Hα耀斑并伴随出现强烈的IV型射电爆发.本文对北京天文台,西澳大利亚站等射电资料进行分析.分析表明:(1)该事件的微波源状态相对稳定,米波源位置存在移动,因此产生微波辐射与米波辐射是两组不同的电子群体,在爆发频谱指数的时变曲线上表现出明显的形态差异.还由于两者辐射源的位置不同,微波与米波的爆发在峰值时刻上也不完全符合.(2)4月1日微波大爆发是由三个主爆发组成的,它们的峰值时刻分别为0135.1,0146.1,0153.6UT.由射电高频端谱指数算出的非热电子能谱指数表明,在射电爆发的三个峰值时刻电子能谱都变硬.本文还得出该活动区的非热电子平均速度(以光速c为单位)β为0.9左右,磁场强度B为430G.并由回旋同步辐射阻尼算得,非热电子的寿命为829秒,这个数值与三个主峰的持续时间相吻合.     

THE PROGRESS ON SPACE ASTRONOMY IN CHINA DURING 2000-2002

In this paper main achievements in the area of space astronomy are summarized.During the flight of cosmic Gamma-Ray Burst Spectrometer(GRBS) onboard spacecraft Shenzhou-2(launched on 2001-01-10), much observational results of cosmic γ-ray burst and solar X, γ-ray burst are obtained. The preliminary analysis on space data has lead to some interesting results. Besides it, some other long-term space astronomy programs are briefly described here.     

Investigating gamma-ray burst data reduction techniques with Swift’s instruments

The amount of data on gamma-ray bursts (GRBs) and the detected afterglows observed by the Swift satellite contributed significantly to the understanding of the phenomenon. The behavior of the early afterglow rises some interesting questions. With the early afterglow localizations of gamma-ray burst positions made by Swift, the clear delimitation of the prompt phase and the afterglow is not so obvious any more. There are hints of a canonical X-ray afterglow lightcurve with segments of different slopes. Not all bursts necessarily show all the segments. It is important to see if the prompt phase and the afterglow has the same origin or they stem from different parts of the progenitor system. We will combine the of gamma-ray burst data from BAT and XRT and compare the extrapolated gamma-ray flux to the X-ray in a sample of bursts and find that there is a good agreement between the two measurements. This indicates that the physical process shaping burst and the early afterglow are the same.     

Developments in high-precision gamma-ray burst source studies

The first interplanetary gamma-ray burst spacecraft network is making possible the precise determination of gamma-ray burst source locations. This network is an international cooperation involving the Helios-2, Pioneer Venus, Venera-11, Venera-12, ISEE-3 and Prognoz-7 spacecraft. The celestial regions that have been defined, with one exception, have no correlations either to known x-ray emitters or to steady optical counterparts, to ～ 22nd mag. The event of 1979 March 5 has a very small source field located within the contour of the supernova remnant N49 in the LMC; the possibility of this measurement as a source identification, the 55 kpc distance of N49 as opposed to the nearby source distances assumed for typical bursts, and the very different characteristics of this event, however, are three arguments for its separate classification. The recent identification of an archived, 50-year old, optical transient within the high-precision source field of a typical burst [1] suggests both that events may repeat and that sources may be localized with even greater accuracy optically.This review outlines the precise source location data being produced by the first and the second spacecraft networks, the possibilities of additional networks and of related studies in other disciplines, and the prospects both for real-time optical transient observations and for the definition of gamma-ray burst sources by optical transient astronomy.     

Limit cycles of accretion disks in the Rapid Burster and GRS 1915+105

The Rapid Burster is known to show rapidly repetitive bursts (Type II bursts). An interesting feature of the Type II burst is an approximate proportionality of the burst duration to the time to the next burst. The time sequence from a burst to the following quiescent phase can be said to be a time-scale invariant high (burst phase)–low (quiescent phase) transition. The Galactic superluminal source, GRS 1915+105 exhibits a variety of the time variation of the X-ray flux and often repeats transitions between a high-flux level and a low-flux level. In such high–low transitions, Belloni et al. (1997b) found an approximate proportionality between the duration of the low-flux phase and that of the following high-flux phase, over a wide range of the time scale. This low–high transition can again be said to be time-scale invariant. However, an interesting difference between the two time scale invariant transitions is an opposite order of the high and low-flux phase in the time-scale invariant sequence. In the case of the Rapid Burster, the high-flux (burst) phase is the first, while the low-flux phase is the first in the case of GRS1915+105. A limit cycle between an accretion disk in a state of the standard-disk and that in a state of the ADAF (advection dominated accretion flow) is discussed to explain the time-scale invariant high–low (or low–high) transition as well as the difference between the neutron star system and the black-hole system, qualitatively. A phenomenological relation of the accretion disk change with mass ejections from the central part of the disk is also discussed.     

FC-AE-1553网络的“并发交换式”动态带宽调度机制

为提高航天航空网络传输性能,针对低轨空间舱内有效载荷系统的特点及有效载荷系统数据传输的要求,将空间有效载荷系统的数据分为周期性业务、突发性业务及强时效性业务3种业务类型,并综合分析3种业务特征,提出了一种可应用于FC-AE-1553网络的“并发交换式”动态带宽调度（DBA）机制,即突发性业务传输采用“并发交换式”的动态带宽分配,周期性业务采用静态固定带宽分配,强时效性业务采用抢占式带宽分配的方案。采用理论分析和仿真验证的方式分析了该调度机制的可行性,并通过OPNET仿真软件建立了FC-AE-1553网络仿真平台。结果表明,相比FC-AE-1553网络传统的“总线式”调度机制,所提机制可将FC-AE-1553网络的吞吐量提高10倍以上,且当网络节点数为32时,FC-AE-1553网络的吞吐量可从2.8 Gb/s提高到46 Gb/s,突发性业务的平均时延可降低1个数量级。      

Collaborative VLA,SOHO and RHESSI observations of evolving sources of energy release in the corona above active regions

Very Large Array (VLA) observations at 20 and 91 cm wavelength are compared with data from the SOHO (EIT and MDI) and RHESSI solar missions to investigate the evolution of decimetric Type I noise storms and Type III bursts and related magnetic activity in the photosphere and corona. The combined data sets provide clues about the mechanisms that initiate and sustain the decimetric bursts and about interactions between thermal and nonthermal plasmas at different locations in the solar atmosphere. On one day, frequent, low-level hard X-ray flaring observed by RHESSI appears to have had no clear affect on the evolution of two closely-spaced Type I noise storm sources lying above the target active region. EIT images however, indicate nearly continuous restructuring of the underlying EUV loops which, through accompanying low-level magnetic reconnection, might give rise to nonthermal particles and plasma turbulence that sustain the long-lasting Type I burst emission. On another day, the onset of an impulsive hard X-ray burst and subsequent decimetric burst emission followed the gradual displacement and coalescence of a small patch of magnetic magnetic polarity with a pre-existing area of mixed magnetic polarity. The time delay of the impulsive 20 and 91 cm bursts by up to 20 min suggests that these events were unlikely to represent the main sites of flare electron acceleration, but instead are related to the rearrangement of the coronal magnetic field after the main flare at lower altitude. Although the X-ray flare is associated with the decimetric burst, the brightness and structure of a long-lasting Type I noise storm from the same region was not affected by the flare. This suggests that the reconfiguration of the coronal magnetic fields and the subsequent energy release that gave rise to the impulsive burst emission did not significantly perturb that part of the corona where the noise storm emission was located.     

A model of the rapid burster

A new burst mode of MXB 1730 - 335, the rapid burster, as discovered by Hakucho in August 1979, is characterized by a train of long X-ray bursts whose behaviour is dictated by the accretion rate. In this mode the burst luminosity reaches the Eddington limit, so that the X-ray pressure controls the accretion from a reservoir in the magnetopause and accretion columns in the polar regions explain general features of the rapid burster observed in August 1979.     

Optical bursts from X-ray irradiated accretion disk

A new burst mode of MXB 1730 - 335, the rapid burster, as discovered by Hakucho in August 1979, is characterized by a train of long X-ray bursts whose behaviour is dictated by the accretion rate. In this mode the burst luminosity reaches the Eddington limit, so that the X-ray pressure controls the accretion from a reservoir in the magnetopause and accretion columns in the polar regions explain general features of the rapid burster observed in August 1979.     

Noise in wireless systems from solar radio bursts

Solar radio bursts were first discovered as result of their interference in early defensive radar systems during the Second World War (1942). Such bursts can still affect radar systems, as well as new wireless technologies. We have investigated a forty-year record of solar radio burst data (1960–1999) as well as several individual radio events in the 23rd solar cycle. This paper reviews the results of a portion of this research. Statistically, for frequencies f  1 GHz (near current wireless bands), there can be a burst with amplitudes >10³ solar flux units (SFU; 1 SFU = 10⁻²² W/m²) every few days during solar maximum conditions, and such burst levels can produce problems in contemporary wireless systems.     

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.     

Gradient pattern analysis of short solar radio bursts

We analyze the weak component of the localized temporal pattern variability of 3 GHz solar burst observed by the Ondrejov radiospectrograph. A complex, short and weak impulsive sample from the time series was analyzed by applying a method based on the gradient pattern analysis and discrete wavelet decomposition. By analyzing canonical temporal variability patterns we show that the new method can reliably characterize the phenomenological dynamical process of short time series (N ? 10³ measurements) as the radio burst addressed here. In the narrowest sense, by estimating the mutual information distance in the gradient spectra, we show that the fluctuation pattern of the short and weak 3 GHz impulsive solar burst, with energetic amplitudes <350 SFU, is closer to the intermittent and strong MHD turbulent variability pattern.     

A solar type U burst in the decimetric range

This paper analyzes a Type U burst at 1.0 – 2.8 GHz which occurred between 12:36:26 – 12:36:32 UT on 1992 August 22, observed by Ond ejov Observatory, Czech Republic. This may be the first example of Type U bursts in the decimetric range, as far as we know. From analysis we came to the following conclusion: (1) The frequency drift rates of the ascending and descending branches are 1.25 and 0.225 GHz/s, respectively, and the velocities of the electron beam are 0.38 c and 0.26 c, respectively; (2) The burst decay of the ascending branch is larger than that of the descending branch; (3) The variations of the maximum frequencies of instantaneous spectra with time appear as from the highest (1.92 GHz) to the lowest (1.0 GHz), then toward higher frequency (1.53 GHz) (this is consistent with that predicted by plasma emission theory); (4) The bandwidths of the ascending branch are about twice that of the descending branch (this may be caused by the larger drift rates of the ascending branch); (5) The temperature of the coronal loop apex is 6.3 × 10⁶ K; (6) The magnetic field at the top of the loop is greater than 9.2 G; (7) This U burst emission is plasma radiation at the second harmonic.