XMM-Newton observations of the field of γ-ray burst 980425

The error box of GRB980425 has been observed by XMM-Newton in March 2002, with the aim of measuring the late epoch X-ray emission of the supernova 1998bw and of clarifying its supposed association with the GRB itself. We present here the preliminary results obtained with the EPIC PN camera. Our observations confirm the association between SN 1998bw and GRB980425. The EPIC PN measurement of the SN 1998bw flux is significantly below the extrapolation of the power-law temporal trend fitted to the BeppoSAX points and implies a faster temporal decay. We propose different physical interpretations of the SN X-ray light curve, according to whether it is produced by one or more radiation components.     

The statistical features of radio bursts with fine structure at 1.1–7.6 GHz

This work presents the spectral and temporal features of radio bursts with fine structures (FSs) at broad band from 1.1 to 7.6 GHz. Fifteen burst events are studied with high frequency and temporal cadence observation from the Solar Broadband Radio Spectrometer at three frequency bands. It is found that the amount and species of radio FS decrease with increasing frequency band; the pulsation, type III burst and continuum are most frequently recorded; almost in all the burst events, more radio FSs occur before the soft X-ray (SXR) maximum than after; at 1.1–2.06 GHz, all types of radio FSs have more before the SXR peak except fiber; at 2.6–3.8 GHz, pulsation, fiber and spike prefer to appear after the peak; the separation between neighboring emission lines of zebra pattern increases with increasing frequency and the magnetic field deduced from the whistler model is 29–86 G at 1.1–2.06 GHz and 89–268 G at 2.6–3.8 GHz.     

Multi-scale reconnections in a complex CME

A series of three flares of GOES class M, M and C, and a CME were observed on 20 January 2004 occurring in close succession in NOAA 10540. Types II, III, and N radio bursts were associated. We use the combined observations from TRACE, EIT, Hα images from Kwasan Observatory, MDI magnetograms, GOES, and radio observations from Culgoora and Wind/ WAVES to understand the complex development of this event. We reach three main conclusions. First, we link the first two impulsive flares to tether-cutting reconnections and the launch of the CME. This complex observation shows that impulsive quadrupolar flares can be eruptive. Second, we relate the last of the flares, an LDE, to the relaxation phase following forced reconnections between the erupting flux rope and neighbouring magnetic field lines, when reconnection reverses and restores some of the pre-eruption magnetic connectivities. Finally, we show that reconnection with the magnetic structure of a previous CME launched about 8 h earlier injects electrons into open field lines having a local dip and apex (located at about six solar radii height). This is observed as an N-burst at decametre radio wavelengths. The dipped shape of these field lines is due to large-scale magnetic reconnection between expanding magnetic loops and open field lines of a neighbouring streamer. This particular situation explains why this is the first N-burst ever observed at long radio wavelengths.     

Fast spectroscopy of the 4 November 1978 gamma-ray burst

The Franco-Soviet Signe experiments on Venera 11 and Venera 12 allow a spectral analysis of gamma-ray bursts with a time resolution of 250 ms. Evidence is presented for i) short annihilation flashes of up to 20 photons cm⁻²s⁻¹ and ii) rapid variations of the continuum, from a study of the intense 4 November 1978 event.     

缠绕复合材料壳体爆破压强的预测

针对缠绕复合材料壳体在内压作用下的破坏问题,基于连续损伤介质力学方法,建立了一种缠绕复合材料渐进损伤破坏分析模型。模型中考虑了纤维破坏、基体损伤和纤维/基体开裂3种破坏模式,并针对缠绕复合材料面内剪切非线性的实际,建立了面内剪切非线性模型。通过子程序UMAT将模型嵌入ABAQUS/Standard中,对含缺口缠绕复合材料试件拉伸过程进行了仿真计算,验证了模型的正确性。采用该模型对缠绕复合材料壳体的水压破坏过程进行了仿真分析,结果表明:内压作用下缠绕复合材料的最终破坏是由于纤维断裂导致的,且纤维破坏主要出现在环向层,基体破坏主要出现在纵向层。      

轴流式轮盘破裂转速的数值计算方法

对3种轴流式轮盘在常温和高温下进行了非线性有限元计算,提出了一种应用有限元法计算轮盘破裂转速的破裂准则,得出了3种轮盘的破裂转速;并将计算结果与大变形解析法及试验值作了对比分析。      

AGATE: A high energy gamma-ray telescope using drift chambers

The exciting results from the highly successful Energetic Gamma-Ray Experiment Telescope (EGRET) instrument on the Compton Gamma-Ray Observatory (CGRO) has contributed significantly to increasing our understanding of high energy gamma-ray astronomy. A follow-on mission to EGRET is needed to continue these scientific advances as well as to address the several new scientific questions raised by EGRET. Here we describe the work being done on the development of the Advanced Gamma-Ray Astronomy Telescope Experiment (AGATE), visualized as the successor to EGRET. In order to achieve the scientific goals, AGATE will have higher sensitivity than EGRET in the energy range 30 MeV to 30 GeV, larger effective area, better angular resolution, and an extended low and high energy range. In its design, AGATE will follow the tradition of the earlier gamma-ray telescopes, SAS-2, COS B, and EGRET, and will have the same four basic components of an anticoincidence system, directional coincidence system, track imaging, and energy measurement systems. However, due to its much larger size, AGATE will use drift chambers as its track imaging system rather than the spark chambers used by EGRET. Drift chambers are an obvious choice as they have less deadtime per event, better spatial resolution, and are relatively easy and inexpensive to build. Drift chambers have low power requirements, so that many layers of drift chambers can be included. To test the feasibility of using drift chambers, we have constructed a prototype instrument consisting of a stack of sixteen 1/2m × 1/2m drift chambers and have measured the spatial resolution using atmospheric muons. The results on the drift chamber performance in the laboratory are presented here.     

轮盘径向破裂转速计算方法分析及修正

分析了轮盘径向破裂转速理论计算方法及常用平均径向应力计算方法的含义及其特点.且依据理论计算方法的含义,提出了基于有限元计算结果的轮盘径向破裂转速计算修正方法.通过实例应用,证明了相对于理论方法计算结果,修正方法较常用平均径向应力方法计算精度更高,其计算精度由6.6%提高到0.5%以内,且修正方法较理论方法使用更方便、工程适用性更强.      

Mu-level法的湍流猝发频率检测技巧

针对mu-level法分析结果易受试验及检测参数影响的问题,详细探讨了该方法用于湍流猝发频率检测的适应性和提高其检测精度的技巧.通过对不同法向检测位置、采样频率、采样时间、门限值L及附加判定条件下湍流猝发频率的检测和对比分析,获取了各因素对湍流猝发频率检测的影响规律,探讨了提高湍流猝发频率检测准确性的可行途径,并总结了一套基于mu-level法的湍流猝发频率四步测试方法(试采样、试分析、采样、检测分析).      

What we knew,what we know and what we will know about cosmic gamma-ray bursts

The paper is devoted to the present crisis in the field of cosmic gamma-ray bursts. There are two different paradigms of the phenomenon, which have practically equal numbers of supporters. The cosmological one associates bursts with collisions of compact objects at distances up to those with red-shifts of about 1–2. The galactic paradigm assumes that bursts are generated by neutron stars in the extended galactic halo. The present situation is shown to be very close to the ultimate establishment of the paradigm of the origin of cosmic gamma-ray bursts.