Time-dependent thermal X-ray afterglows from GRBS

Time-dependent thermal X-ray spectra are calculated from physically plausible conditions around GRB. It is shown that account for time-dependent ionization processes strongly affects the observed spectra of hot rarefied plasma. These calculations may provide an alternative explanation to the observed X-ray lines of early GRBs afterglows (such as GRB 011211). Our technique will allow one to obtain independent constraints on the GRB collimation angle and on the clumpiness of circumstellar matter.     

Gamma ray bursts: Short vs. long

Short and long GRBs are thought to be two distinct classes based on their different duration and spectrum. Through the spectral analysis of two similarly selected samples of BATSE short and long GRBs, we show that short GRBs are harder than long events, confirming what found from the comparison of their hardness ratio. However, this spectral diversity seems to be due to a harder low energy spectral component of short GRBs, rather than a (slightly higher) peak energy. Interestingly short GRBs have a spectrum which is similar to the spectrum of the emission of the first 1–2 s of long events. We find evidence that short GRBs are inconsistent with the E_peak–E_iso correlation defined by long bursts while they follow the same E_peak–L_iso correlation of long GRBs. These results, coupled to the similar variability timescale of short events and the first seconds of long ones, suggest that a common (or similar) dissipation mechanism could operate in both classes. The difference in the duration would then be due mainly to the central engine lifetime.     

DD6镍基单晶涡轮转子叶片失效分析

为了排除某航空发动机DD6镍基单晶高温合金涡轮转子叶片在室温振动试验中发生的裂纹故障,对故障叶片进行了外观检查、断口分析、表面检查、解剖检查、化学成分分析、金相检查、应力分布计算及热模拟试验,确定了故障叶片裂纹的性质和产生原因.结果表明:涡轮转子叶片裂纹为高周疲劳裂纹,叶片局部区域存在异常的γ'筏排组织是导致该叶片产生早期疲劳开裂的主要原因,且附近区域腐蚀过重及结构上处于应力集中区,也促进了疲劳裂纹的萌生及扩展.针对这些故障,建议优化叶片结构并对腐蚀检查进行严格监控,防止出现γ’筏排组织及腐蚀过重现象,从而避免此类故障再次发生.     

DC Characteristics of Gamma-ray Irradiated SiGe HBT in Comparison with Si BJT

The changes of DC characteristics of SiGe HBT after being submitted to γ-ray irradiation of 700 krad, 7 000 krad and 10 000 krad were compared to those of Si BJT. Generally speaking, Ib and Ib–Ib0 increase with the doses increasing. For SiGe HBT, with the doses increasing, Ic and Ic–Ic0 as well as the related changes of the current gain (β) will decrease at higher Vbe, while for Si BJT, with the doses increasing, after irradiation, Ib and Ic–Ic0 increase; β and its related changes also decrease with their differences, however, tending to be very small at high doses of 7 000 krad and 10 000 krad. Moreover, given the same doses, the decreases of β are much larger than SiGe HBT, which shows that SiGe HBT’s anti-radiation performance proves to be better than Si BJT. Still, in SiGe HBT, some strange phe-nomena were observed: Ic–Ic0 will increase after the radiation of 7 000 krad in less than 0.65 V and as will β in less than 0.75 V. The mechanism of radiation-induced change in DC characteristics was also discussed.     

Two years of INTEGRAL result on X-ray binaries

INTEGRAL is the ESA lead International Gamma-Ray Astrophysical Laboratory, successfully launched the 17th October 2002 from Baikonur with a Proton vehicle. In view of the high sensitivity of the two γ-ray instruments IBIS and SPI and their capability to provide at the same time image, spectra and time profiles of all the sources in their wide field of view, a key project was approved as “Core Programme” to obtain deep observations of the Galactic Centre (GCDE) and to exploit regular scan of the whole Galaxy Plane since the beginning of the mission. This paper will briefly review the main astrophysical results obtained in the field of high energy Galactic sources with the INTEGRAL/IBIS γ-ray Imager onboard INTEGRAL, and make a comparison with the previous scenario depicted by the BeppoSAX and RXTE results.     

浇注温度对1种新型铸造镍基高温合金组织和拉伸性能的影响

为分析浇注温度与合金的组织结构和力学性能之间的变化关系,通过改变浇注温度获得不同枝晶组织试样,采用金相显微镜和扫描电镜来观察和分析合金的组织结构,结合拉伸性能测试研究了合金的组织结构对拉伸性能的影响。结果表明：降低浇注温度使γ＇相和碳化物得到细化;降低浇注温度提高了合金的拉伸强度,并改善了塑性。     

基于γ-Re_(θt)转捩模型的低雷诺数翼型数值分析

通过综合运用Michel转捩判据和γ-Re_(θt)转捩模型的方法实现对低雷诺数翼型的气动分析。首先通过Michel转捩判据和层流分离位置分别估算转捩动量厚度雷诺数,然后分别用Langtry和Tomac提出的经验关系式计算转捩动量厚度雷诺数和转捩区长度,通过UDF(User-Defined Functions)将不同组的3个经验关联值写入Fluent软件对E387翼型(雷诺数为3×10~5)进行数值分析,并与试验值进行了对比。结果表明:基于Michel转捩判据比基于层流分离更能准确预测转捩位置,基于层流分离预测的转捩位置过于靠前,但是2种方法的气动力计算结果与试验值都比较吻合,Langtry和Tomac的经验关系式计算结果之间差别不大,Tomac方法能够计算出分离泡,且与Selig油流试验吻合较好。     

微通道流动转捩数值模拟

应用CFD计算软件ANSYS CFX对水力直径为0.4mm的矩形截面微尺度通道中的气体流动进行了数值模拟.采用了3种流动模型,即γ-Re_θt转捩模型、层流模型和剪切应力输运（SST）模型,并将模拟结果与实验结果进行了对比.模拟结果表明:层流模型及SST模型不具有预测转捩的能力;γ-Re_θt转捩模型捕捉到了临界雷诺数且摩擦因数相对误差在20%以下.在未达到临界雷诺数之前,通道后部已经出现局部湍流区,且局部湍流区随着雷诺数的增大而增大.壁面摩擦因数的最低点对应的流向位置与通道中前后湍流区的交结位置几乎一致.      

基于Gamma-Theta模型的固定转捩数值模拟研究

采用γ-~Reθt转捩模型,对NACA0012翼型的固定转捩进行数值模拟,计算了不同雷诺数下刚好激发转捩又不引起过大局部压力扰动和附加阻力的最低粗糙带高度,说明了γ-~Reθt模型模拟固定转捩的能力。通过计算低雷诺数下固定转捩来模拟高雷诺数下自然转捩,计算结果表明固定转捩可以较好地模拟自然转捩。这两种计算结果对风洞试验都有重要的指导意义。     

Summary of the workshop on gamma-ray burst afterglows at the 34th COSPAR meeting

A summary is given of the presentations at the COSPAR workshop on γ-ray bursts with some personal commentary on the contributions, the SN/GRB connection, and on the role of magnetic fields in γ-ray bursts and their afterglows. Of special interest were the accumulated arguments for strong collimation and associated reduction in the total required energy for γ-ray bursts. Significant discussion was also devoted to the issues associated with iron and metal lines in X-ray spectra. It is important to note that some of the afterglows seem to require ambient densities 1 g cm⁻³, rather incompatible with a massive star environment. Of associated difficulty is the fact that few, if any, afterglows seem consistent with the r⁻² wind expected for a massive star model. There are reasons to think that if γ-ray bursts are associated with supernovae they are of Type Ic. This suggests that any wind present might be rich in carbon and oxygen, not hydrogen or helium. If γ-ray bursts are narrowly collimated, then the burst is only probing a small portion of any wind, perhaps just that time-dependent and isotropic structure directly along the rotation axis. The characteristics of “hypernovae” may be the result of orientation effects in a mildly inhomogeneous set of progenitors, rather than requiring an excessive total energy or luminosity. The recent event GRB 021004 provided a rich photometric and spectroscopic record and perhaps the most direct evidence yet for the association of a specific γ-ray burst with a massive star progenitor. If the magnetic field plays a significant role in launching a relativistic γ-ray burst jet from within a collapsing star, then the magnetic field may also play a role in the propagation, collimation, and stability of that jet within and beyond the star. The magneto-rotational instability (MRI) can operate under conditions of moderate rotation. This means that the MRI will be at work generating strong fields exponentially rapidly even as the disk of material begins to form and makes a transition from a non-Keplerian to quasi-Keplerian flow in the collapsar and related models.