Fermi detection of a luminous γ-ray pulsar in a globular cluster

We report on the Fermi Large Area Telescope's detection of γ-ray (>100 mega-electron volts) pulsations from pulsar J1823-3021A in the globular cluster NGC 6624 with high significance (~7 σ). Its γ-ray luminosity, L(γ) = (8.4 ± 1.6) × 10(34) ergs per second, is the highest observed for any millisecond pulsar (MSP) to date, and it accounts for most of the cluster emission. The nondetection of the cluster in the off-pulse phase implies that it contains <32 γ-ray MSPs, not ~100 as previously estimated. The γ-ray luminosity indicates that the unusually large rate of change of its period is caused by its intrinsic spin-down. This implies that J1823-3021A has the largest magnetic field and is the youngest MSP ever detected and that such anomalous objects might be forming at rates comparable to those of the more normal MSPs.     

60Co γ射线辐照选育阿维链霉菌及辐射效应研究

[目的]采用60Coγ射线辐照选育阿维链霉菌,筛选B1a产量提高的突变菌株。[方法]用60Coγ射线作为诱变源,在辐照剂量200～1 600 Gy、剂量率10 Gy/min的条件下对一株未经任何诱变的微生物农药阿维菌素菌株Av2进行了诱变改良;对该菌株的致死率、突变率、菌落形态变化与60Coγ射线辐照剂量的关系进行了探讨,其中初筛采用抑菌圈法,复筛采用摇瓶培养发酵,阿维菌素含量测定采用高效液相色谱法。[结果]在800 Gy辐射剂量下得到了Av2-m212、Av2-m245和Av2-m286 3株高效突变菌,其Bla产量分别比原始菌株提高了36%、41%和46%,均属于皱缩型菌株。高于30%的正突变菌均在800 Gy辐射剂量下产生,该剂量点是致死率和正突变率趋于平稳的交叉点。辐照后皱缩型和火山型突变菌有正突变菌,其他形态菌株均为负突变。[结论]60Coγ射线在阿维菌素产生菌的诱变筛选中起到了重要作用,是一种非常有效的微生物诱变育种方法。     

γ射线与EMS单一及复合处理对烤烟种子活力的诱变效应

为探讨γ射线与EMS对烤烟诱变的适宜剂量,以K346、NC82和云85等3个品种的风干种子为材料,设置10个~(60)Co-γ射线剂量梯度和11个EMS浓度梯度及其组合共计330个处理,研究了γ射线与EMS单一及复合处理对烤烟种子活力的影响.结果表明,γ射线、EMS、品种及其两两互作等因素均对种子活力指数有极显著影响.3个品种对γ射线的辐射敏感性顺序为云85＞K346＞NC82,烟草γ射线诱变适宜剂量为300～350 Gy;3个品种对EMS的诱变敏感性顺序为云85＞K346≈NC82;烟草EMS诱变适宜浓度为0.35%;γ射线与EMS复合诱变敏感性顺序为云85＞K346≈NC82,复合处理中γ射线对活力指数的损伤效应大于EMS.     

60Co-γ射线辐射对芦荟生理指标的影响

探讨了6 0 Co- γ射线不同剂量辐射对芦荟生理指标的影响。试验结果表明 :淀粉以 10Gy辐射处理值最高 ,2 0Gy辐射处理最低 ;蛋白质以未辐射处理值最高 ;可溶性糖、SOD比活力、POD比活力、CAT比活力均以 2 0Gy辐射处理最高 ;PPO比活力与辐射剂量之间存在极显著正相关。芦荟的生理生化功能以 2 0Gy辐射处理的表现较为适中。     

Particle accelerators in the hot spots of radio galaxy 3C 445, imaged with the VLT

Hot spots (HSs) are regions of enhanced radio emission produced by supersonic jets at the tip of the radio lobes of powerful radio sources. Obtained with the Very Large Telescope (VLT), images of the HSs in the radio galaxy 3C 445 show bright knots embedded in diffuse optical emission distributed along the post-shock region created by the impact of the jet into the intergalactic medium. The observations reported here confirm that relativistic electrons are accelerated by Fermi-I acceleration processes in HSs. Furthermore, both the diffuse emission tracing the rims of the front shock and the multiple knots demonstrate the presence of additional continuous re-acceleration processes of electrons (Fermi-II).     

Discovery of a compact radio component in the center of supernova 1986J

Very-long-baseline interferometry observations have revealed a bright, compact radio component near the center of the expanding shell of supernova 1986J. The component, not present in earlier images, has an inverted radio spectrum different from that of the shell. Such an inversion has not been seen in the spectrum of any other supernova. The new component is likely radio emission associated either with accretion onto a black hole or with the nebula formed around an energetic young neutron star in the center of SN 1986J, which would directly link either a black hole or a neutron star to a modern supernova.     

γ-射线辐照对植物保护性酶活性和MDA含量的影响

综述了在生长发育和储藏保鲜过程中不同剂量γ-射线处理对植物体内保护性酶活性和MDA含量的影响,并且在辐照保鲜中保护性酶活性和MDA含量的变化。     

Hydrogen 21-centimeter emission from a galaxy at cosmological distance

We have detected the neutral atomic hydrogen (HI) emission line at a cosmologically significant distance [redshift (z) = 0.18] in the rich galaxy cluster Abell 2218 with the Westerbork Synthesis Radio Telescope. The HI emission originates in a spiral galaxy 2.0 h65(-1) megaparsecs from the cluster core. No other significant detections have been made in the cluster, suggesting that the mechanisms that remove neutral gas from cluster galaxies are efficient. We infer that fewer than three gas-rich galaxies were accreted by Abell 2218 over the past 10(9) years. This low accretion rate is qualitatively consistent with low-density cosmological models in which clusters are largely assembled at z > 1.     

不同辐射剂量对果蔗种芽苗期生长的影响

采用 30 Gy、5 0 Gy、70 Gy三种等级的 6 0 Co射线对果蔗种芽进行辐射处理 ,结果果蔗苗期生长受到不同程度的影响 ,表现为出苗率、移栽成活率、分蘖率低 ,果蔗植株生长、叶片生长慢。并且随着辐射剂量的增加 ,影响程度随之加重 ;6个果蔗品种对 6 0 Co辐射敏感性不一 ,白鳝蔗对 6 0 Co辐射敏感性较弱 ,同安果蔗、白玉蜜蔗较强     

豆腐干类风味制品试制与质量控制技术的研究

[目的]建立地方特色豆腐干制品常温非制冷保藏的技术。[方法]以生产过程中的减菌消毒措施降低起始菌数目,点浆环节加入优选的食品防腐剂,与熟制、真空包装6、0Coγ射线辐照加工相结合,进行综合控菌。[结果]将清洗、加热灭菌、防止二次污染以及消毒等减菌措施综合运用,可降低豆腐干产品的起始细菌数;如该类产品保质期只要求在常温下5 d之内,可采用在点浆工序中加入丙酸钙（2.5 g/kg）及实施真空包装即可;如保质期要求在常温下30 d,可采用剂量为6 kGy的60Coγ射线对其真空包装制品作辐照处理即可,而其熟制品在同样条件下可放置90 d,产品风味保持良好。[结论]控制起始菌技术与熟制、真空包装6、0Coγ射线辐照加工相结合,进行综合控菌,可实现豆腐干风味制品常温非制冷保藏90 d的目标。     

Fast variability of tera-electron volt gamma rays from the radio galaxy M87

The detection of fast variations of the tera-electron volt (TeV) (10(12) eV) gamma-ray flux, on time scales of days, from the nearby radio galaxy M87 is reported. These variations are about 10 times as fast as those observed in any other wave band and imply a very compact emission region with a dimension similar to the Schwarzschild radius of the central black hole. We thus can exclude several other sites and processes of the gamma-ray production. The observations confirm that TeV gamma rays are emitted by extragalactic sources other than blazars, where jets are not relativistically beamed toward the observer.     

γ射线对舞毒蛾虫卵处理效果的研究

为检验物理灭虫的效果,以林木害虫舞毒蛾(Lymantria dispar)虫卵为试验材料,用不同剂量的γ射线照射舞毒蛾虫卵,研究照射后幼虫孵化率的宏观变化情况和经过台盼蓝活体染色后幼虫细胞的微观变化情况.结果表明,随着γ射线辐照剂量的增加,幼虫孵化率逐渐降低,幼虫细胞的死亡数量逐渐上升;总体上看,宏观试验和微观试验所得...     

IRAS 14348-1447, an Ultraluminous Pair of Colliding, Gas-Rich Galaxies: The Birth of a Quasar?

Ground-based observations of the object IRAS 14348-1447, which was discovered with the Infrared Astronomical Satellite, show that it is an extremely luminous colliding galaxy system that emits more than 95 percent of its energy at far-infrared wavelengths. IRAS 14348-1447, which is receeding from the sun at 8 percent of the speed of light, has a bolometric luminosity more than 100 times larger than that of our galaxy, and is therefore as luminous as optical quasars. New optical, infrared, and spectroscopic measurements suggest that the dominant luminosity source is a dustenshrouded quasar. The fuel for the intense activity is an enormous supply of molecular gas. Carbon monoxide emission has been detected at a wavelength of 2.6 millimeters by means of a new, more sensitive receiver recently installed on the 12-meter telescope of the National Radio Astronomy Observatory. IRAS 14348-1447 is the most distant and luminous source of carbon monoxide line emission yet detected. The derived mass of interstellar molecular hydrogen is 6 x 10(10) solar masses. This value is approximately 20 times that of the molecular gas content of the Milky Way and is similar to the largest masses of atomic hydrogen found in galaxies. A large mass of molecular gas may be a prerequisite for the formation of quasars during strong galactic collisions.     

Tracing black hole mergers through radio lobe morphology

Binary supermassive black holes are produced by galactic mergers as the black holes from the two galaxies fall to the center of the merged system and form a bound pair. The two black holes will eventually coalesce in an enormous burst of gravitational radiation. Here we show that the orientation of a black hole's spin axis would change dramatically even in a minor merger, leading to a sudden flip in the direction of any associated jet. We identify the winged or X-type radio sources with galaxies in which this has occurred. The inferred coalescence rate is similar to the overall galaxy merger rate, implying that of the order of one merger event per year could be detected by gravitational wave interferometers.     

A Transient Radio Source near the Center of the Milky Way Galaxy

In late December 1990, a new radio source appeared near the center of our galaxy rivaling the intensity of Sgr A(*) (the compact radio source at the galactic center). Following its first detection, the flux density of the galactic center transient (GCT) increased rapidly to a maximum 1 month later, and then declined gradually with a time scale of about 3 months. Surprisingly, the GCT maintained a steep radio spectrum during both its rising and decay phases. The neutral hydrogen (HI) absorption shows similar absorption to that in front of Sgr A(*); this indicates that the GCT lies near the galactic center. Furthermore, both HI and OH observations show an additional deep absorption at +20 kilometers per second with respect to the local standard of rest. Thus, the GCT is either embedded in or located behind a molecular cloud moving with that velocity. The cloud can be seen on infrared images. Its opacity is shown to be inadequate to conceal a supernova near the galactic center. It is argued that the GCT was probably transient radio emission from synchrotron-radiating plasma associated with an x-ray binary system.     

Discovery of new variable radio sources in the nucleus of the nearby galaxy messier 82

Widespread variability has been discovered in a large population of radio sources close to the nucleus of an active galaxy. The galaxy, Messier 82 (M82), and others similar to it show evidence for enhanced nuclear activity and unusually strong far-infrared emission. The observational data, obtained with the National Radio Astronomy Observatory's Very Large Array in New Mexico over the past 3 years, provide the first direct "look" at a starburst-the phenomenon of sudden, rapid star formation which occurs near the nucleus of a small fraction of galaxies. Nearly all the brightest of about 40 radio sources in M82' s nucleus decreased in intensity over 2.7 years up to October 1983. One source, which in February 1981 was ten times as bright as our Galaxy's most luminous supernova remnant, turned off within only a few months. Most of the other ten strongest sources are declining so rapidly that they will fade into the background within 30 years. Thus, new supernovae are expected to appear in M82' s nucleus every few years. The discovery has revealed the "engine room" of the mysterious activity in M82 and, by implication, similar active galaxies which have disturbed nuclei and which are unusually luminous in the far infrared. An estimate of the rate of energy input by the radio-visible supernovae closely matches the far-infrared luminosities which were recently measured for M82 and other similar galaxies.     

应用γ-射线辐照降解羽毛的研究

分别采用0,100,200,300,400,500,600 kGy剂量的γ-射线对羽毛进行辐照处理,探索了不同剂量γ-射线辐照直接降解羽毛的可行性以及辐照剂量对羽毛水解率和可溶性蛋白回收率的影响。结果表明:γ-射线可在一定程度上直接降解羽毛,但降解率比较低;与碱法降解相结合,在辐照剂量为240 kGy时羽毛的降解率最高可达34.92%,但羽毛中的可溶性蛋白也受到破坏,含量为20.05%;在辐照剂量为100 kGy时羽毛的降解率为28.12%低于240kGy剂量辐照时的降解率,但可溶性蛋白含量较高(30.12%)。因此确定γ-射线辐照直接降解羽毛的最佳辐照剂量为100~240 kGy.     

Upper limit of 3.3 astronomical units to the diameter of the galactic center radio source sgr a*

Sagittarius (Sgr) A(*) is a unique radio source located at the center of our galaxy. The radiation from Sgr A(*) may be generated in matter accreting onto a massive black hole. In observations at long wavelengths, the apparent angular size of Sgr A(*) decreases in the manner expected for emission from a point source scattered by electron density fluctuations along the line of sight. Measurements at a wavelength of 7 millimeters with the nearly completed Very Long Baseline Array indicate a size of 0.7 milliarc seconds, which is consistent with an extrapolation from results at longer wavelengths. The true size of Sgr A(*) must be less than 0.4 milliarc seconds, or 3.3 astronomical units. The inferred black hole mass is less than 1.5 x 10(6) solar masses according to a recent model for the emission.     

Neutral hydrogen survey of andromeda galaxy

A neutral hydrogen survey of the Andromeda galaxy (M31) has been conducted with the 260-foot (80m) Ohio State University radio telescope. The neutral hydrogen is concentrated in the spiral arm regions, with but relatively small amounts near the center of the galaxy. Similar deficiencies have been found near the center of M33 and our galaxy, suggesting similar evolutionary processes in the three galaxies.     

Evidence for black holes

Black holes are common objects in the universe. Each galaxy contains large numbers-perhaps millions-of stellar-mass black holes, each the remnant of a massive star. In addition, nearly every galaxy contains a supermassive black hole at its center, with a mass ranging from millions to billions of solar masses. This review discusses the demographics of black holes, the ways in which they interact with their environment, factors that may regulate their formation and growth, and progress toward determining whether these objects really warp spacetime as predicted by the general theory of relativity.