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。     

一种低副瓣宽零点的自适应波束形成算法

自适应波束形成算法能自动地将波束的主瓣对准期望用户信号的来波方向,零陷对准干扰信号的来波方向;但是常规的自适应算法形成的干扰零限比较尖锐,副瓣容易产生畸变,在干扰、天线平台快速移动的情况下,其性能将会严重下降。本文基于对权值的范数约束和对零点的最小二乘线性约束优化,提出了一种降低副瓣电平并且加宽零点的自适应波束形成算法。理论分析和计算机仿真结果证明了新算法的有效性     

一种低副瓣宽零点的自适应波束形成算法

自适应波束形成算法能自动地将波束的主瓣对准期望用户信号的来波方向,零陷对准干扰信号的来波方向;但是常规的自适应算法形成的干扰零限比较尖锐,副瓣容易产生畸变,在干扰、天线平台快速移动的情况下,其性能将会严重下降.基于对权值的范数约束和对零点的最小二乘线性约束优化,提出了一种降低副瓣电平并且加宽零点的自适应波束形成算法.理论分析和计算机仿真结果证明了新算法的有效性.     

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。     

极低逾渗阈值的导电聚苯胺纳米复合膜

直接将改进的微乳液聚合法合成的纳米聚苯胺分别与聚乙烯醇和聚丙烯酰胺进行溶液共混复合,浇铸成纳米聚苯胺复合膜,研究了聚苯胺的加入量对复合膜的电导率的影响.所得复合膜的电导率符合逾渗规律,且导电膜的逾渗阈值极低,为0.04%左右,其中PVA纳米复合膜出现了双逾渗行为.加入极少量的聚苯胺即可使膜的导电率发生突跃,使其从绝缘体转变成半导体或导体.逾渗阈值下的复合膜不仅力学性能良好,而且透明性接近于纯基体膜,当膜中的聚苯胺质量分数为0.1%时,PVA复合膜对300～700 nm波长的可见光的透过率为70%～84%.     

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.     

OFDM系统中一种改进的低复杂度自适应比特功率分配算法

针对正交频分复用(orthogonal frequency division multiplexing,OFDM)系统在进行自适应比特功率分配时存在过高复杂度的问题,提出了一种基于边缘自适应(margin adaptive,MA)准则的改进低复杂度自适应比特功率分配算法.与贪婪(Greedy)算法相比,提出的改进算法通过预分配和迭代分配2部分来降低算法的计算量.改进算法先在预分配中根据信道条件预先分配部分比特,在迭代分配中通过增大内存开销的方法减少Greedy算法中计算和比较每个子信道功率增量的次数,从而降低算法的复杂度.仿真结果表明,在相同的仿真环境下算法的自适应分配效果和Greedy算法的自适应分配效果基本一致,同时该算法和Greedy算法具有几乎相同的误比特性能.且随着子信道数量的增加,与Greedy算法相比,该算法的运行时间更短,进而说明所提出的算法具有较低的复杂度.     

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.     

An experimental study of premixed laminar methane/oxygen/argon flames doped with hydrogen at low pressure with synchrotron photoionization

Laminar premixed stoichiometric methane/hydrogen/oxygen/argon flames were investigated with tunable synchrotron vacuum ultraviolet （VUV） photoionizaUon and molecular-beam sampling mass spectrometry techniques. The methane/hydrogen fuel blends with hydrogen volumetric fraction of 0, 20%, 40%, 60% and 80% were studied. All observed flame species, including stable intermediates and radicals in the flames, were detected by measuring photoionization mass spectra and photoionization efficiency （PIE） spectra. Mole fraction profiles of major species and intermediates were derived by scanning burner at some selected photon energies near ionization thresholds. The influence of hydrogen addition on mole fraction of major species and intermediates was analyzed. The results show that the major species mole fraction of CO, CO2 and CH4 decreases with the increase of hydrogen fraction. The mole fraction of intermediates measured in this experiment decreases remarkably with the increase of hydrogen fraction. This would be due to the increase of H and OH radicals by hydrogen addition and the high diffusivity and activity of H radical promoting the chemical reaction. In addition, the increase of H/C ratio with the increase of hydrogen fraction also leads to the decrease of the mole fraction of carbon-related intermediates and contributes to the decrease of unburned and incomplete combustion products.