Formation of giant planets by fragmentation of protoplanetary disks

The evolution of gravitationally unstable protoplanetary gaseous disks has been studied with the use of three-dimensional smoothed particle hydrodynamics simulations with unprecedented resolution. We have considered disks with initial masses and temperature profiles consistent with those inferred for the protosolar nebula and for other protoplanetary disks. We show that long-lasting, self-gravitating protoplanets arise after a few disk orbital periods if cooling is efficient enough to maintain the temperature close to 50 K. The resulting bodies have masses and orbital eccentricities similar to those of detected extrasolar planets.     

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 formation of substellar objects induced by the collision of protostellar disks

Simulations of a close encounter between two protostars, each surrounded by a relatively massive disk, resulted in the ejection of some of the disk material into a tidal tail. A portion of the tail condensed into an object with a mass in the range of 5 to 10 jovian masses. This mechanism may explain the existence of the single objects of substellar mass that have recently been discovered.     

Three-layered atmospheric structure in accretion disks around stellar-mass black holes

Modeling of the x-ray spectra of the Galactic superluminal jet sources GRS 1915+105 and GRO J1655-40 reveals a three-layered atmospheric structure in the inner region of their accretion disks. Above the cold and optically thick disk with a temperature of 0.2 to 0.5 kiloelectron volts, there is a warm layer with a temperature of 1.0 to 1.5 kiloelectron volts and an optical depth around 10. Sometimes there is also a much hotter, optically thin corona above the warm layer, with a temperature of 100 kiloelectron volts or higher and an optical depth around unity. The structural similarity between the accretion disks and the solar atmosphere suggests that similar physical processes may be operating in these different systems.     

Organic molecules and water in the planet formation region of young circumstellar disks

The chemical composition of protoplanetary disks is expected to hold clues to the physical and chemical processes that influence the formation of planetary systems. However, characterizing the gas composition in the planet formation region of disks has been a challenge to date. We report here that the protoplanetary disk within 3 astronomical units of AA Tauri possesses a rich molecular emission spectrum in the mid-infrared, indicating a high abundance of simple organic molecules (HCN, C2H2, and CO2), water vapor, and OH. These results suggest that water is abundant throughout the inner disk and that the disk supports an active organic chemistry.     

Star formation around supermassive black holes

The presence of young massive stars orbiting on eccentric rings within a few tenths of a parsec of the supermassive black hole in the galactic center is challenging for theories of star formation. The high tidal shear from the black hole should tear apart the molecular clouds that form stars elsewhere in the Galaxy, and transport of stars to the galactic center also appears unlikely during their lifetimes. We conducted numerical simulations of the infall of a giant molecular cloud that interacts with the black hole. The transfer of energy during closest approach allows part of the cloud to become bound to the black hole, forming an eccentric disk that quickly fragments to form stars. Compressional heating due to the black hole raises the temperature of the gas up to several hundred to several thousand kelvin, ensuring that the fragmentation produces relatively high stellar masses. These stars retain the eccentricity of the disk and, for a sufficiently massive initial cloud, produce an extremely top-heavy distribution of stellar masses. This potentially repetitive process may explain the presence of multiple eccentric rings of young stars in the presence of a supermassive black hole.     

山羊胚胎原始生殖细胞的分离与培养

选择受精后30～50d的关中奶山羊胎儿为材料,参照小鼠原始生殖细胞(PGCs)分离得到了山羊的PGCs,将其分别培养在STO饲养层上,或与同源山羊成纤维细胞(GEF)及山羊睾丸支持细胞(GSCs)共培养。结果表明,3种方法均能获得类EG细胞。分离得到的类EG细胞在STO饲养层上仅传4代;培养在GEF上的效果最差,传至第3代时丢失;而在GSCs上培养的效果最好,可传6代。     

牛原始生殖细胞的分离与培养

从4～15周龄的牛胎儿生殖嵴中分离得到牛原始生殖细胞,以STO(一种建系的小鼠胎儿成纤维细胞)及MEF(小鼠胎儿成纤维细胞)为饲养层抑制分化培养,其中1个细胞系传至4代。研究发现,STO较MEF更有利于牛类EG细胞的分离与培养,体长小于5cm的胎儿适合牛EG细胞分离与克隆。同时观察到这些细胞在体外进行自发性分化,可形成上皮样细胞、神经样细胞和成纤维样细胞。     

随书光(磁)盘的管理与开发

通过对几种图书馆随书光 (磁 )盘管理方法的利弊分析 ,提出了一种随书光 (磁 )盘网络化管理的方法 ,以提高其利用率。     

第28期鸡胚原始生殖细胞的冷冻保存与体外培养研究

利用Ficoll密度梯度离心,提取鸡胚第28期(孵化132h)性腺中的原始生殖细胞(PGCs),用不同的冷冻保护液,对PGCs采用分离后直接冷冻保存和体外培养24h后冷冻保存2种方法,以筛选合适的冷冻保护体系。结果发现,分离提纯后直接进行冷冻保存的PGCs,存活率最高为(87.07±1.29)%;体外培养24h后进行冷冻的PGCs,存活率最高为(44.08±1.19)%。对复苏后的PGCs进行体外培养结果发现,分离提纯后直接进行冷冻的PGCs,在体外培养过程中具有形成细胞克隆的能力,且可传代和进行体外分化;而体外培养24h后进行冷冻的PGCs,复苏后在体外培养过程中不能形成细胞克隆,且在体外培养40h左右死亡。     

Diverse and contrasting effects of habitat fragmentation

Different components of an ecosystem can respond in very different ways to habitat fragmentation. An archipelago of patches, representing different levels of fragmentation, was arrayed within a successional field and studied over a period of 6 years. Ecosystem processes (soil mineralization and plant succession) did not vary with the degree of subdivision, nor did most measures of plant and animal community diversity. However, fragmentation affected vertebrate population dynamics and distributional patterns as well as the population persistence of clonal plant species. The results highlight the dangers of relying on broad community measures in lieu of detailed population analyses in studies of fragmented habitats.     

农业劳动力特征、土地细碎化与农机社会化服务

近年来随着农村劳动力的转移就业,我国农业劳动力数量不断下降,老龄化和女性化趋势明显。农业机械化是应对农村人口变化的关键,在此背景下研究了农机社会化服务对农户农业劳动力变化的补充以及相关的制约因素。基于江苏和安徽省调查数据,利用Probit模型实证分析了农业劳动力特征以及耕地细碎化对农机社会化服务采用的影响。结果表明,在耕地环节和收割环节分别有70.54%和66.83%的农户会全部采用农机社会化服务。老龄户和女性户由于体力、技术等原因会更加偏向于采用农机社会化服务;耕地细碎化则阻碍了农机服务的采用。因此,为进一步促进我国农业机械化发展,提出政府应该不断完善农机社会化服务体系建设,在有条件的地区对土地进行规整降低细碎化程度的政策建议。     

作物幼苗根际土壤MB－S的初步研究

采用根际袋培养技术研究了大豆、玉米、油菜和水稻幼苗（６０ｄ）根际ＭＢ－Ｓ（ＭｉｃｒｏｂｉａｌＢｉｏｍａｓｓ－Ｓｕｌｆｕｒ）的根际效应及硫肥对根际ＭＢ－Ｓ的影响。结果表明：不施Ｓ,根际土壤ＭＢ－Ｓ在２１．６～２３．９ｍｇＳｋｇ－１（土）;油菜和水稻施Ｓ处理根际土壤ＭＢ－Ｓ为２２～２５ｍｇＳｋｇ－１（土）。作物根际土壤中ＭＢ－Ｓ含量比无作物处理提高了６５％～１３０％。非根际土壤ＭＢ－Ｓ在１２．５～１５．４ｍｇＳｋｇ－１（土）,比无作物处理高７％～３３％。根际土壤ＭＢ－Ｓ是非根际土壤的１．７～２倍。水稻根际ＭＢ－Ｓ含量一般比旱作物高。与对照（无作物处理）相比根际ＭＢ－Ｓ增加百分数,水稻稍大于油菜,但明显低于大豆和玉米。硫肥施用对根际土壤ＭＢ－Ｓ的影响不大。作物根际土壤ＭＢ－Ｓ含量与其无机Ｓ呈直线正相关;与其有机硫呈直线负相关。在旱作物中根际土壤ＭＢ－Ｓ与土壤有机碳呈负相关,但在水稻中则相反。作物体含硫量与根际土壤ＭＢ－Ｓ含量呈负相关     

Carbynes: carriers of primordial noble gases in meteorites

Five carbynes (triply bonded allotropes of carbon) have been found by electron diffraction in the Allende and Murchison carbonaceous chondrites: carbon VI, VIII, X, XI, and (tentatively) XII. From the isotopic composition of the associated noble-gas components, it appears that the carbynes in Allende (C3V chondrite) are local condensates from the solar nebula, whereas at least two carbynes in Murchison (C2 chondrite) are of exotic, presolar origin. They may be dust grains that condensed in stellar envelopes and trapped isotopically anomalous matter from stellar nucleosynthesis.