Diffuse Extreme-Ultraviolet Emission from the Coma Cluster: Evidence for Rapidly Cooling Gases at Submegakelvin Temperatures

The central region of the Coma cluster of galaxies was observed in the energy band from 0.065 to 0.245 kiloelectron volts by the Deep Survey telescope aboard the Extreme Ultraviolet Explorer. A diffuse emission halo of angular diameter approximately 30 arc minutes was detected. The extreme-ultraviolet (EUV) emission level exceeds that expected from the x-ray temperature gas in Coma. This halo suggests the presence of two more phases in the emitting gas, one at a temperature of approximately 2 x 10(6) kelvin and the other at approximately 8 x 10(5) kelvin. The latter phase cools rapidly and, in steady state, would have produced cold matter with a mass of approximately 10(14) solar masses within the EUV halo. Although a similar EUV enhancement was discovered in the Virgo cluster, this detection in Coma applies to a noncooling flow system.     

Radiohalos in a radiochronological and cosmological perspective

New photographic evidence, data on halo ring sizes, and x-ray fluorescence analyses provide unambiguous evidence that polonium halos exist as a separate and distinct class apart from uranium halos. Because of the short half-lives of the polonium isotopes involved, it is not clear how polonium halos may be explained on the basis of currently accepted cosmological models of Earth formation.     

A Lunar Occultation of the Dust-Scattering Halo Around GX 5-1 Observed with ROSAT

The x-ray source GX 5-1 in the galactic bulge has been observed with the position-sensitive proportional counter onboard the R?ntgen satellite (ROSAT) during and after a lunar occultation. Extended emission around the source was unambiguously discovered while the central source was behind the lunar rim. This emission is interpreted as a dust-scattering halo around GX 5-1 that has a fractional intensity of 28 percent, implying a grain column density between GX 5-1 and Earth of approximately 3 x 10(10) per square centimeter. The halo derived from imaging during the ROSAT all-sky survey is identical to that obtained from the lunar occultation, thus demonstrating that the ROSAT x-ray mirror scattering has not changed as compared with the mirror properties as measured in preflight calibrations.     

Scheiner's Halo: Evidence for Ice Ic in the Atmosphere

Refraction of sunlight at the angle of minimum deviation between octahedral faces of crystals of ice Ic in the upper atmosphere could produce a halo around the sun or the moon at 27.46 degrees . Crystals of hexagonal ice having low-index faces cannot produce a halo of this radius. It is therefore suggested that Scheiner's halo, which has been reported at least four times since 1629 at 28 degrees from the sun, is due to ice Ic. If this is correct, it is apparently the first evidence that ice Ic occurs naturally and that liquid water can freeze to ice Ic.     

Kinematic evidence for an old stellar halo in the Large Magellanic Cloud

The oldest and most metal-poor Milky Way stars form a kinematically hot halo, which motivates the two major formation scenarios for our galaxy: extended hierarchical accretion and rapid collapse. RR Lyrae stars are excellent tracers of old and metal-poor populations. We measured the kinematics of 43 RR Lyrae stars in the inner regions of the nearby Large Magellanic Cloud (LMC) galaxy. The velocity dispersion equals 53 +/- 10 kilometers per second, which indicates that a kinematically hot metal-poor old halo also exists in the LMC. This result suggests that our galaxy and smaller late-type galaxies such as the LMC have similar early formation histories.     

Direct detection of galactic halo dark matter

The Milky Way galaxy contains a large, spherical component which is believed to harbor a substantial amount of unseen matter. Recent observations indirectly suggest that as much as half of this "dark matter" may be in the form of old, very cool white dwarfs, the remnants of an ancient population of stars as old as the galaxy itself. We conducted a survey to find faint, cool white dwarfs with large space velocities, indicative of their membership in the galaxy's spherical halo component. The survey reveals a substantial, directly observed population of old white dwarfs, too faint to be seen in previous surveys. This newly discovered population accounts for at least 2 percent of the halo dark matter. It provides a natural explanation for the indirect observations, and represents a direct detection of galactic halo dark matter.     

Genesis of the heaviest elements in the Milky Way Galaxy

We review the origin and evolution of the heavy elements, those with atomic numbers greater than 30, in the early history of the Milky Way. There is a large star-to-star bulk scatter in the concentrations of heavy elements with respect to the lighter metals, which suggests an early chemically unmixed and inhomogeneous Galaxy. The relative abundance patterns among the heavy elements are often very different from the solar system mix, revealing the characteristics of the first element donors in the Galaxy. Abundance comparisons among several halo stars show that the heaviest neutron-capture elements (including barium and heavier) are consistent with a scaled solar system rapid neutron-capture abundance distribution, whereas the lighter such elements do not conform to the solar pattern. The stellar abundances indicate an increasing contribution from the slow neutron-capture process (s-process) at higher metallicities in the Galaxy. The detection of thorium in halo and globular cluster stars offers a promising, independent age-dating technique that can put lower limits on the age of the Galaxy.     

Radiohalos: some unique lead isotope ratios and unknown alpha radioactivity

Previously unreported lead isotope ratios, that is, values for the lead-206/lead-207 ratio ranging from about 20 to 60, primarily radiogenic in origin but unsupported by uranium decay, have been determined in the inclusions of certain polonium halos by means of ion microprobe techniques. Evidence for radiogenic lead-208 unsupported by thorium decay may also be inferred from the existence of a composite polonium halo type with rings from the radioactive precursors of lead-208. Several new dwarf halo sizes, seem to indicate the existence of unknown, very low-energy alpha-emitters. Furthermore, the three-ring "X halo" also provides evidence for an unknown series of genetically related alpha-emitters with energies in the range from 3 to 7 million electron volts.     

The central galaxy in abell 2029: an old supergiant

A mosaic of images shows the extended structure of the cD galaxy that resides at the center of the rich cluster of galaxies Abell 2029. After correcting for the scattered light of nearby stars and galaxies, the faint halo of this giant can be traced out to a distance of more than 1 megaparsec, making it one of the largest and most luminous galaxies known. The smoothness of this halo suggests that it was formed early in the history of the cluster.     

The dark halo of the milky Way

Most of the matter in the Milky Way is invisible to astronomers. Precise numbers are elusive, but it appears that the dark component is 20 times as massive as the visible disk of stars and gas. This dark matter is distributed in space differently than the stars, forming a vast, diffuse halo, more spherical than disklike, which occupies more than 1000 times the volume of the disk of stars. The composition of this dark halo is unknown, but it may comprise a mixture of ancient, degenerate dwarf stars and exotic, hypothetical elementary particles.     

利用抽样函数实现螺线聚焦管道中的束晕-混沌控制研究

根据束晕-混沌控制策略方法,利用具有非线性、收敛性的抽样函数构造控制器,对初始条件遵从K-V 分布的离子束进行了控制研究。结果表明,加控制后束晕强度因子变为零,束均方根半径、束横向动量平方和的平均值和束横向平均发射度比控制前都明显减小。利用该方法可实现束晕-混沌的有效控制。     

Three-dimensional polarimetric imaging of coronal mass ejections

We present three-dimensional reconstructions of coronal mass ejections (CMEs), which were obtained through polarization analysis of single-view images recorded with the use of the Large Angle and Spectrometric Coronagraph (LASCO) C2 coronagraph on board the Solar and Heliospheric Observatory (SOHO) spacecraft. Analysis of a loop-like CME shows a complex three-dimensional structure centered at 40 degrees from the plane of the sky, moving radially at 250 kilometers/second. Reconstruction of two halo CMEs suggests that these events are expanding loop arcades.     

利用抽样函数实现螺线聚焦管道中的束晕-混沌控制研究

根据束晕-混沌控制策略方法,利用具有非线性、收敛性的抽样函数构造控制器,对初始条件遵从K-V分布的离子束进行了控制研究。结果表明,加控制后束晕强度因子变为零,束均方根半径、束横向动量平方和的平均值和束横向平均发射度比控制前都明显减小。利用该方法可实现束晕-混沌的有效控制。     

种衣剂和叶面肥处理对绿豆晕疫病防治效果及生长的影响

[目的]研究田间绿豆晕疫病的防治方案。[方法]研究不同种衣剂和叶面肥组合对绿豆晕疫病田间防治效果和绿豆生长的影响。[结果]种衣剂拌种并喷施叶面肥对绿豆田间晕疫病的防治效果最好,病株率仅为3.0%,防治效果达91.4%,并且3组处理绿豆植株的株高、主茎分枝数、主茎节数、单株荚数、荚长、荚粒数、籽粒大小、单株粒重和百粒重等重要表型性状均高于对照组,3组处理的产量分别为1 126.20、1 213.80和1 194.60 kg/hm~2,也均显著高于对照组。[结论]种衣剂拌种和喷施叶面肥能有效控制田间绿豆晕疫病的发生和危害,提高绿豆产量。     

The 46{degrees} Halo and Its Arcs

Ice crystals in the form of right hexagonal prisms have faces that form 90 degrees prisms. Light rays were traced through these prism faces by computer calculation, and the light patterns that would be produced in the sky for a particular distribution of crystal orientations were simulated. Crystals with random orientations produce a 46 degrees halo. Hexagonal plate crystals with nearly horizontal end faces produce circumzenithal and circumhorizontal arcs. Hexagonal column crystals with horizontal axes produce supralateral and infralateral arcs. Plate crystals spinning about a horizontal axis that is a face diagonal of the crystal produce a series of arcs touching the 46 degrees halo. Each of these effects was simulated for several elevations of the sun.     

冠状彩晕的模拟实验分析

不同云层中正六角柱状冰晶对称轴取向不同,面内沿各向分布,使非主截面内光线的最小偏向角不同,验曲线,推证出冠状彩晕的形状．太阳上方冰晶对称轴平行于地面且在平行于地面的层形成了冠状彩晕;用充水三棱镜模拟冰三棱镜做出实     

Comet kohoutek: ultraviolet images and spectrograms

Emissions of atomic oxygen (1304 angstroms), atomic carbon (1657 angstroms), and atomic hydrogen (1216 angstroms) from Comet Kohoutek were observed with ultraviolet cameras carried on a sounding rocket on 8 January 1974. Analysis of the Lyman alpha halo at 1216 angstroms gave an atomic hydrogen production rate of 4.5 x 10(29) atoms per second.     

玉米弯孢菌叶斑病菌致病力分化测定

以8个黑龙江省主栽玉米品种为鉴别寄主,对不同来源的玉米弯孢菌叶斑病菌[新月弯孢菌Curvularialunata(Wakker)Boed.]菌株进行了致病力分化测定。结果表明,不同菌株间存在明显的致病性差异,不同菌株在相同寄主上能产生不同类型的病斑,病斑大小、形状、边缘颜色、晕圈大小存在较大差异,说明菌株间有明显的致病力分化现象。     

A reservoir of ionized gas in the galactic halo to sustain star formation in the Milky Way

Without a source of new gas, our Galaxy would exhaust its supply of gas through the formation of stars. Ionized gas clouds observed at high velocity may be a reservoir of such gas, but their distances are key for placing them in the galactic halo and unraveling their role. We have used the Hubble Space Telescope to blindly search for ionized high-velocity clouds (iHVCs) in the foreground of galactic stars. We show that iHVCs with 90 ≤ |v(LSR)| ? 170 kilometers per second (where v(LSR) is the velocity in the local standard of rest frame) are within one galactic radius of the Sun and have enough mass to maintain star formation, whereas iHVCs with |v(LSR)| ? 170 kilometers per second are at larger distances. These may be the next wave of infalling material.     

Fossil alpha-recoil analysis of certain variant radioactive halos

The distribution of alpha-radioactivity in the vicinity of uranium and of certain variant radioactive halos in biotite was investigated by the fossil alpharecoil method. Within the limits of the method I could not confirm a previously proposed hydrothermal mechanism for the origin of certain variant halo types due to polonium isotopes.