The onset of planet formation in brown dwarf disks

The onset of planet formation in protoplanetary disks is marked by the growth and crystallization of sub-micrometer-sized dust grains accompanied by dust settling toward the disk mid-plane. Here, we present infrared spectra of disks around brown dwarfs and brown dwarf candidates. We show that all three processes occur in such cool disks in a way similar or identical to that in disks around low- and intermediate-mass stars. These results indicate that the onset of planet formation extends to disks around brown dwarfs, suggesting that planet formation is a robust process occurring in most young circumstellar disks.     

The mass of dwarf planet Eris

The discovery of dwarf planet Eris was followed shortly by the discovery of its satellite, Dysnomia, but the satellite orbit, and thus the system mass, was not known. New observations with the Keck Observatory and the Hubble Space Telescopes show that Dysnomia has a circular orbit with a radius of 37,350 +/- 140 (1-sigma) kilometers and a 15.774 +/- 0.002 day orbital period around Eris. These orbital parameters agree with expectations for a satellite formed out of the orbiting debris left from a giant impact. The mass of Eris from these orbital parameters is 1.67 x 10(22) +/- 0.02 x 10(22) kilograms, or 1.27 +/- 0.02 that of Pluto.     

A transient radio jet in an erupting dwarf nova

Astrophysical jets seem to occur in nearly all types of accreting objects, from supermassive black holes to young stellar objects. On the basis of x-ray binaries, a unified scenario describing the disc/jet coupling has evolved and been extended to many accreting objects. The only major exceptions are thought to be cataclysmic variables: Dwarf novae, weakly accreting white dwarfs, show similar outburst behavior to x-ray binaries, but no jet has yet been detected. Here we present radio observations of a dwarf nova in outburst showing variable flat-spectrum radio emission that is best explained as synchrotron emission originating in a transient jet. Both the inferred jet power and the relation to the outburst cycle are analogous to those seen in x-ray binaries, suggesting that the disc/jet coupling mechanism is ubiquitous.     

ROSAT X-ray detection of a young brown dwarf in the chamaeleon I dark cloud

Photometry and spectroscopy of the object Cha Halpha 1, located in the Chamaeleon I star-forming cloud, show that it is a approximately 10(6)-year-old brown dwarf with spectral type M7.5 to M8 and 0.04 +/- 0.01 solar masses. Quiescent x-ray emission was detected in a 36-kilosecond observation with 31.4 +/- 7.7 x-ray photons, obtained with the Rontgen Satellite (ROSAT), with 9final sigma detection significance. This corresponds to an x-ray luminosity of 2.57 x 10(28) ergs per second and an x-ray to bolometric luminosity ratio of 10(-3.44). These are typical values for late M-type stars. Because the interior of brown dwarfs may be similar to that of convective late-type stars, which are well-known x-ray sources, x-ray emission from brown dwarfs may indicate magnetic activity.     

A search for companions to nearby brown dwarfs: the binary DENIS-P J1228.2-1547

Hubble Space Telescope imaging observations of two nearby brown dwarfs, DENIS-P J1228.2-1547 and Kelu 1, made with the near-infrared camera and multiobject spectrometer (NICMOS), show that the DENIS object is resolved into two components of nearly equal brightness with a projected separation of 0.275 arc second (5 astronomical units for a distance of 18 parsecs). This binary system will be able to provide the first dynamical measurement of the masses of two brown dwarfs in only a few years. Upper limits to the mass of any unseen companion in Kelu 1 yield a planet of 7 Jupiter masses aged 0. 5 x 10(9) years, which would have been detected at a separation larger than about 4 astronomical units. This example demonstrates that giant planets could be detected by direct imaging if they exist in Jupiter-like orbits around nearby young brown dwarfs.     

Discovery of a low-mass brown dwarf companion of the young nearby star G 196-3

A substellar-mass object in orbit at about 300 astronomical units from the young low-mass star G 196-3 was detected by direct imaging. Optical and infrared photometry and low- and intermediate-resolution spectroscopy of the faint companion, hereafter referred to as G 196-3B, confirm its cool atmosphere and allow its mass to be estimated at 25-10+15 Jupiter masses. The separation between the objects and their mass ratio suggest the fragmentation of a collapsing cloud as the most likely origin for G 196-3B, but alternatively it could have originated from a protoplanetary disc that has been dissipated. Whatever the formation process was, the young age of the primary star (about 100 million years) demonstrates that substellar companions can form on short time scales.     

High-pressure and high-temperature experiments on core-mantle segregation in the accreting Earth

The abundances of siderophile elements in the Earth's silicate mantle are too high for the mantle to have been in equilibrium with iron in the core if equilibrium occurred at low pressures and temperatures. It has been proposed that this problem may be solved if equilibrium occurred at high pressures and temperatures. Experimental determination of the distribution of siderophile elements between liquid metal and liquid silicate at 100 kilobar and 2000 degrees C demonstrates that it is unlikely that siderophile element abundances were established by simple metal-silicate equilibrium, which indicates that the segregation of the core from the mantle was a complex process.     

A gaseous metal disk around a white dwarf

The destiny of planetary systems through the late evolution of their host stars is very uncertain. We report a metal-rich gas disk around a moderately hot and young white dwarf. A dynamical model of the double-peaked emission lines constrains the outer disk radius to just 1.2 solar radii. The likely origin of the disk is a tidally disrupted asteroid, which has been destabilized from its initial orbit at a distance of more than 1000 solar radii by the interaction with a relatively massive planetesimal object or a planet. The white dwarf mass of 0.77 solar mass implies that planetary systems may form around high-mass stars.     

Characterization of dwarf mutants and molecular mapping of a dwarf locus in soybean

Plant height is one of the most important traits in soybean. The semi-dwarf soybean cultivars could improve the ability of lodging resistance to obtain higher yield. To broaden the dwarfism germplasm resources in soybean, 44 dwarf mutants were identified from a gamma rays mutagenized M_-2 population. Two of these mutants, Gmdwf1(Glycine max dwarf 1) and Gmdwf2(Glycine max dwarf 2), were investigated in this study. Genetic analysis showed that both mutants were inherited in a recessive manner and their mutated regions were delimited to a 2.610-Mb region on chromosome 1 by preliminary mapping. Further fine mapping study proved that the two mutants had a common deletion region of 1.552 Mb in the target region, which was located in a novel locus site without being reported previously. The dwarfism of Gmdwf1 could not be rescued by gibberellin(GA) and brassinolide(BR) treatments, which indicated that the biosynthesis of these hormones was not deficient in Gmdwf1.     

Nitrite, an electron donor for anoxygenic photosynthesis

We report a previously unknown process in which anoxygenic phototrophic bacteria use nitrite as an electron donor for photosynthesis. We isolated a purple sulfur bacterium 98% identical to Thiocapsa species that stoichiometrically oxidizes nitrite to nitrate in the light. Growth and nitrate production strictly depended on both light and nitrite. This is the first known microbial mechanism for the stoichiometric oxidation of nitrite to nitrate in the absence of oxygen and the only known photosynthetic oxidation in the nitrogen cycle. This work demonstrates nitrite as the highest-potential electron donor for anoxygenic photosynthesis known so far.     

新疆褐牛体重与体尺指标的相关及回归分析

为探讨新疆褐牛体重与体尺指标间的相关性及构建不同生长阶段的回归方程,为新疆褐牛选育提供直接而有效的方法,以伊犁地区2011—2019年6月龄、12月龄、18月龄、24月龄新疆褐牛为对象,测定4个生长阶段的4个体尺指标和体重并进行相关性分析和逐步线性回归分析.新疆褐牛不同生长阶段体重和体尺指标间存在着极显著的(P<0.0...     

Stellar feedback in dwarf galaxy formation

Dwarf galaxies pose substantial challenges for cosmological models. In particular, current models predict a dark-matter density that is divergent at the center, which is in sharp contrast with observations that indicate a core of roughly constant density. Energy feedback, from supernova explosions and stellar winds, has been proposed as a major factor shaping the evolution of dwarf galaxies. We present detailed cosmological simulations with sufficient resolution both to model the relevant physical processes and to directly assess the impact of stellar feedback on observable properties of dwarf galaxies. We show that feedback drives large-scale, bulk motions of the interstellar gas, resulting in substantial gravitational potential fluctuations and a consequent reduction in the central matter density, bringing the theoretical predictions in agreement with observations.     

水稻黑条矮缩病矮化程度与产量关系研究

对不同时期发病的黑条矮缩病病株矮化程度进行了调查,结果发现不同发病时期的矮化程度存在显著差异,据此将不同时期的病株分为5类。在此基础上对不同类型植株的单株产量、有效分蘖、穗长、秕谷率和千粒重等重要指标进行了考察,采用DPS软件对试验结果进行了相关性和差异显著性分析。数据分析表明,随着病情加重,植株产量、有效分蘖、穗长和千粒重明显下降,秕谷率则显著上升,且不同类型间考察指标达到了显著水平。     

Procion brown: an intracellular dye for light and electron microscopy

Procion browvn has been used to inject lamprey giant interneutros. The dye is opaque to both light and electrons, and imparts a pink color to the neuron in situ during iontophoresis. It has the advantage over cobaltolus chloride that postinjection treatment with ammonium sulfide is eliminated and the integrity of the surrounding neuropil is ensured.     

糜子矮秆突变体“819”矮秆基因的遗传学分析

为揭示糜子矮秆突变体“819”矮秆基因的遗传规律,为后续定位矮秆突变基因提供理论基础,研究调查了糜子矮秆突变体“819”与高秆材料J12,以及它们杂交产生的674个F₂代个体的株高、穗长、穗颈长、分蘖数、茎节数、二级枝梗长度1、二级枝梗长度2、二级枝梗长度3、二级枝梗间距1、二级枝梗间距2共10个性状,进一步利用方差分析、卡方检验、相关及回归分析、主成分分析对这些性状进行研究。结果表明,糜子矮秆突变体“819”的矮秆性状是由单基因控制的隐性性状;株高与穗长、穗颈长、分蘖数、茎节数、二级枝梗长度1、二级枝梗长度2、二级枝梗长度3、二级枝梗间距1呈极显著正相关(P<0.01),与二级枝梗间距2呈显著正相关(P<0.05);株高(Y)对其他农艺性状的回归方程为:Y=-18.446+1.491X₁+1.222X₂+6.827X₄+1.319X₇+0.746X₈,回归方程的拟合度为0.811,回归方程经显著性检验达到极显著水平(P<0.01),可以利用回归方程对株高进行预测;糜子F₂群体的10个性状进行主成分分析获得3个主成分,这3个主成分的累积贡献率高达72.656%,3个主成分分别被命名为长度因子、茎节数因子、枝梗间距因子。研究结果为矮秆基因定位、矮秆后代的评价选择提供了依据。     

中国水稻黑条矮缩病研究进展

水稻黑条矮缩病是水稻重要的病毒病,对水稻生产造成严重损失。该病由灰飞虱传播的水稻黑条矮缩病毒引起。本文综述了近年来中国水稻黑条矮缩病病原基因组结构和功能、传毒介体、病害流行以及防治等方面的最新研究进展,为中国水稻黑条矮缩病的综合防控提供依据。     

稻褐飞虱对噻嗪酮抗性的检测技术

建立了适合于测定褐飞虱对噻嗪酮敏感性的稻茎浸渍法及相对敏感毒力基线。用该方法检测的结果表明：１９９６年安庆、江浦,１９９７年南宁种群对噻嗪酮为早期抗性（抗性倍数为３．０￣３．５）;１９９６年由南向北敏感性有下降趋势,而１９９７年该趋势不明显。还对抗性监测方法及抗生治理进行了讨论。     

南方水稻黑条矮缩病毒S6编码一个沉默抑制子

 【目的】分析南方水稻黑条矮缩病毒（SRBSDV）基因组S6编码的SP6蛋白的抑制子活性,明确SRBSDV是否编码RNA沉默抑制子来干扰植物的沉默。【方法】将分别含有SP6与GFP质粒的农杆菌共浸润转GFP基因的16c本氏烟纯合系,观察SP6对局部沉默和系统沉默的抑制作用;将含有SP6,GFP和dsGFP质粒的农杆菌三者共浸润,观察SP6对由dsRNA引起的沉默的抑制作用;在同一植株不同部位接种GFP和SP6,观察SP6对RNA沉默信号传导的影响;通过马铃薯X病毒（Potato virus X,PVX）在本氏烟上表达SP6,观察SP6是否能增强PVX的致病性。【结果】SP6能抑制由GFP正义RNA介导的沉默,但其抑制作用较弱,仅能延缓局部沉默和系统沉默的产生。SP6能灭活RNA沉默信号,阻止沉默信号的长距离传导,回复GFP的沉默,但不能抑制由dsRNA引起的沉默。利用PVX在本氏烟上表达SP6能增强PVX的致病性。【结论】SP6是病毒编码的RNA沉默抑制子,在RNA沉默的起始和信号传导阶段起作用。