A short gamma-ray burst apparently associated with an elliptical galaxy at redshift z = 0.225

Gamma-ray bursts (GRBs) come in two classes: long (> 2 s), soft-spectrum bursts and short, hard events. Most progress has been made on understanding the long GRBs, which are typically observed at high redshift (z approximately 1) and found in subluminous star-forming host galaxies. They are likely to be produced in core-collapse explosions of massive stars. In contrast, no short GRB had been accurately (< 10') and rapidly (minutes) located. Here we report the detection of the X-ray afterglow from--and the localization of--the short burst GRB 050509B. Its position on the sky is near a luminous, non-star-forming elliptical galaxy at a redshift of 0.225, which is the location one would expect if the origin of this GRB is through the merger of neutron-star or black-hole binaries. The X-ray afterglow was weak and faded below the detection limit within a few hours; no optical afterglow was detected to stringent limits, explaining the past difficulty in localizing short GRBs.     

An enigmatic long-lasting gamma-ray burst not accompanied by a bright supernova

Gamma-ray bursts (GRBs) are short, intense flashes of soft gamma-rays coming from the distant Universe. Long-duration GRBs (those lasting more than approximately 2 s) are believed to originate from the deaths of massive stars, mainly on the basis of a handful of solid associations between GRBs and supernovae. GRB 060614, one of the closest GRBs discovered, consisted of a 5-s hard spike followed by softer, brighter emission that lasted for approximately 100 s (refs 8, 9). Here we report deep optical observations of GRB 060614 showing no emerging supernova with absolute visual magnitude brighter than M(V) = -13.7. Any supernova associated with GRB 060614 was therefore at least 100 times fainter, at optical wavelengths, than the other supernovae associated with GRBs. This demonstrates that some long-lasting GRBs can either be associated with a very faint supernova or produced by different phenomena.     

A gamma-ray burst with a high-energy spectral component inconsistent with the synchrotron shock model

Gamma-ray bursts are among the most powerful events in nature. These events release most of their energy as photons with energies in the range from 30 keV to a few MeV, with a smaller fraction of the energy radiated in radio, optical, and soft X-ray afterglows. The data are in general agreement with a relativistic shock model, where the prompt and afterglow emissions correspond to synchrotron radiation from shock-accelerated electrons. Here we report an observation of a high-energy (multi-MeV) spectral component in the burst of 17 October 1994 that is distinct from the previously observed lower-energy gamma-ray component. The flux of the high-energy component decays more slowly and its fluence is greater than the lower-energy component; it is described by a power law of differential photon number index approximately -1 up to about 200 MeV. This observation is difficult to explain with the standard synchrotron shock model, suggesting the presence of new phenomena such as a different non-thermal electron process, or the interaction of relativistic protons with photons at the source.     

A very energetic supernova associated with the gamma-ray burst of 29 March 2003

Over the past five years evidence has mounted that long-duration (>2 s) gamma-ray bursts (GRBs)-the most luminous of all astronomical explosions-signal the collapse of massive stars in our Universe. This evidence was originally based on the probable association of one unusual GRB with a supernova, but now includes the association of GRBs with regions of massive star formation in distant galaxies, the appearance of supernova-like 'bumps' in the optical afterglow light curves of several bursts and lines of freshly synthesized elements in the spectra of a few X-ray afterglows. These observations support, but do not yet conclusively demonstrate, the idea that long-duration GRBs are associated with the deaths of massive stars, presumably arising from core collapse. Here we report evidence that a very energetic supernova (a hypernova) was temporally and spatially coincident with a GRB at redshift z = 0.1685. The timing of the supernova indicates that it exploded within a few days of the GRB, strongly suggesting that core-collapse events can give rise to GRBs, thereby favouring the 'collapsar' model.     

An optical spectrum of the afterglow of a gamma-ray burst at a redshift of z = 6.295

The prompt gamma-ray emission from gamma-ray bursts (GRBs) should be detectable out to distances of z > 10 (ref. 1), and should therefore provide an excellent probe of the evolution of cosmic star formation, reionization of the intergalactic medium, and the metal enrichment history of the Universe. Hitherto, the highest measured redshift for a GRB has been z = 4.50 (ref. 5). Here we report the optical spectrum of the afterglow of GRB 050904 obtained 3.4 days after the burst; the spectrum shows a clear continuum at the long-wavelength end of the spectrum with a sharp cut-off at around 9,000 A due to Lyman alpha absorption at z approximately 6.3 (with a damping wing). A system of absorption lines of heavy elements at z = 6.295 +/- 0.002 was also detected, yielding the precise measurement of the redshift. The Si ii fine-structure lines suggest a dense, metal-enriched environment around the progenitor of the GRB.     

An origin for short gamma-ray bursts unassociated with current star formation

Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized and fading afterglow counterparts detected. The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations. The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 (refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2-3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts--the coalescence of binary systems of neutron stars or a neutron star-black hole pair--are the progenitors of short bursts.     

An improved algorithm for blind carrier frequency estimation with burst MPSK transmissions

This paper presents an improved non-data-aided algo-rithm for carrier frequency estimation for burst M-ary PSK signals when modulation order M and training symbols are unknown. Unlike data-aided estimation, a phase clustering algorithm is used first to estimate M and modulated information is removed by a vari-able interval linear phase unwrapping. Then, a high-order correlation algorithm with proper correction is present, which reduces the probability of phase ambiguity and promotes anti-noise capability of the estimation. Simulations are given to analyze the unbiased esti-mation range, and the asymptotic performance and symbol number are needed to compare with the former algorithms. The new algo-rithm has a large estimation range close to the theoretical maximum value for non-data-aided estimation and has a better performance than earlier non-data-aided techniques for large frequency offset, low signal-to-noise ratio, and limited symbol numbers.     

有限域上的低复杂度正规基及其对偶基

设q为素数的方幂,n为正整数,Fqn为有限域 Fq 的n次扩域。利用 Fq 上多项式分解和Fqn在Fq上正规基N＝｛αqi｜i＝0,1,…,n-1｝的基本性质得出一些低复杂度正规基及其对偶基 B＝｛βqi｜i＝0,1,…,n-1｝,并给出它们生成元之间的关系以及它们的乘法表T＝（ ti ,j ）和 H＝（ hi ,j ）,同时得出对偶基复杂度的上界。     

国有企业效率低下的原因分析

我国国有企业效率普遍偏低，造成这一现象的原因主要有：经济体制、经济形势发生了深刻的变化；经济改革中存在某些失误以及国有企业承担了过高的改革成本；政企不分和国有企业产权制度存在缺陷。其中最根本的原因在于产权制度的缺陷。     

具有年龄结构的SIRS流行病模型的分析

建立和研究一类具有非终身免疫并带有年龄结构的SIRS流行病模型平衡解的存在性与稳定性。在总人口规模不变的假设下,运用微分方程和积分方程的理论和方法得到了决定疾病消亡与否的基本再生数R0的表达式;证明了当R0<1时无病平衡点是全局渐近稳定的,当R0>1时此时至少存在一个地方病平衡点,并在一定的条件下证明了该地方病平衡点的局部渐近稳定性。     

一种X波段低插损5位数控衰减器设计

该文基于IBM 0.18μm Si Ge Bi CMOS工艺,采用混合结构设计了一种可用于X波段相控阵的5位数控衰减器.通过电路分析和计算,确定了电路中的元件参数,通过对NMOS开关进行仿真分析,得到了最优尺寸.阐述了一种插损补偿技术,即在输入输出端引入串联电感来降低电路的插损并且优化端口匹配.仿真结果显示,该衰减器的插损小于5.0 d B;所有状态的相移小于7°;输入端口回波损耗小于-15.7 d B,输出端口回波损耗小于-16.65 d B.     

低信噪比弱信号提取算法研究

采用从强背景噪声中提取话音信号的自适应噪声抵消技术———最小均方误差(LMS)入手,对该算法的性能进行了分析,针对其收敛速度慢、提取信号频带窄的缺点,提出了改进的有动量因子的自适应最小均方误差算法(MLMS).仿真结果表明,该方法对于解决弱信号提取问题有一定效果.     

提高动态性能的齿轮优化设计

本文提出了以齿轮副的动态性能作为目标函数,以其中的连续参数作为设计变量,并对啮合过程中的最大动载荷加以限制的优化设计方法.经这种方法设计的齿轮,其动载荷及振动加速度的均方根值,在各种转速下均比常规设计的小得多.     

庞加莱指数在一个带有接种疫苗的SIS流行病模型中的应用

给出一个带有接种疫苗的SIS流行病模型,并对它进行了分析,得出该模型有3个稳定点,其中1个无病平衡点及2个染病平衡点.     

偏差计数型位置伺服系统的最优控制模型

1.引言偏差计数型位置伺服系统结构简单、快速性好、定位精度高,在数字伺服领域被广为应用。若对该系统速度内环作简化处理,整个系统可按二阶系统考虑。其等效结构框图如图1。     

无标度网络上具有2个染病者仓室的SIR模型分析

在无标度网络中建立和分析具有2个染病者仓室的SIR模型,首先计算得到基本再生数R0;证明了当R01时,无病平衡点是全局渐近稳定的;当R01时,存在唯一的地方病平衡点且疾病是持续性传染病.其次研究和比较网络上的2种免疫,得到在平均免疫率相同的条件下,目标免疫比随机免疫更有效.最后利用数值分析验证了主要结论.     

具有ω型燃烧室的缸内流动特性的研究

用PDA对活塞顶具有ω型燃烧室的缸内二维紊流场进行了测量,讨论了气门偏置、燃烧室偏心、挤流以及活塞运动速度对平均速度和紊流强度的影响,结果表明:在进气过程中缸内气流是翻滚式的流动,而在压缩过程中则是朝向燃烧室的汇合流动.     

光学法诊断发动机燃烧过程的实验研究

研制了一个用于发动机燃烧过程监测和分析的光电测量系统，包括一个以镀膜蓝宝石棒为传感头的光纤燃烧传感器，一套以光电倍增管ＰＭＴ为光探测器的检测电路和一套数据采集分析系统．应用这个系统在一台汽油机上进行了实际测量．实验表明，光学法可以准确地测出发动机燃烧过程的时间参数，从光强变化曲线可以得到混合气均匀性和燃烧循环波动之间的关系