中国东北黑土地研究进展与展望

东北黑土区是世界四大片黑土区之一,它以高有机质和高肥力而著称,不仅是东北农业发展的基础,也是中国的粮仓,在保障国家粮食安全中具有举足轻重的地位。针对东北黑土自身的特色和面临的问题,首先描述了东北黑土地形成的条件及自然黑土的属性特征;其次阐述了黑土被开垦后农田化过程中土壤属性和肥力的演化情况,土壤有机质大幅度下降,土壤肥力降低,已严重影响到东北黑土地农业的可持续发展;在此基础上分析了黑土区耕作土壤不同保护途经及其对土壤肥力的影响机制;最后展望了未来黑土地理论研究的侧重点：应加大新技术、新方法和跨学科交叉理论的研究,培育更适合东北黑土地气候条件的高产优质作物品种,并结合目前黑土地保护的技术调控模式,优化作物种植模式,提升作物品质和产量,提高黑土区农业的综合生产力和竞争力、保证黑土区农业的永续利用。     

近200年来全球地震活动与月相及地球自公转的关系分析

对1811-2008年近200年来全球地震活动与月相、日地距离、地球自转速度这三个天文因素的统计分析表明,月相不论与全球地震还是全球大地震之间似乎无统计关系,全球地震的发生与日地距离似乎无统计关系。本文还进一步对全球M≥7．5的大地震进行了统计,结果表明M≥7．5的大地震与地球处于近日点似乎有一定的关系,但关系不太明显。全球除了8．0〉M≥7．0的地震基本上符合发震的自然概率外,在M≥9．0、9．0〉M≥8．0、6．0〉M≥5．0、4．0〉M≥3．0这些震级段地震发生的机率在地球自转减速期比较小,在地球自转加速期发生的机率比较大,似乎地球自转速度的变化对全球地震活动有一定的促发作用,但不明显。     

哈雷彗星观测报告

1986年3月16日至4月19日,中国南极考察队二次越冬队在南极洲乔治王岛中国南极长城站执行了哈雷彗星观测任务。在为期34天的时间里共进行了8次观测,拍摄到大尺度照片9张,并详细地记录了观测过程。     

Visible and near-infrared spectrophotometry of the Deep Impact ejecta of Comet 9P/Tempel 1

We have obtained optical spectrophotometry of the evolution of Comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field Spectrograph (SNIFS) at the UH 2.2-m telescope, as well as simultaneous optical and infrared spectra using the Lick Visible-to-Near-Infrared Imaging Spectrograph (VNIRIS). The spatial distribution and temporal evolution of the “violet band” CN (0-0) emission and of the 630 nm [OI] emission was studied. We found that CN emission centered on the nucleus increased in the 2 h after impact, but that this CN emission was delayed compared to the light curve of dust-scattered sunlight. The CN emission also expanded faster than the cloud of scattering dust. The emission of [OI] at 630 nm rose similarly to the scattered light, but then remained nearly constant for several hours after impact. On the day following the impact, both CN and [OI] emission concentrated on the comet nucleus had returned nearly to pre-impact levels. We have also searched for differences in the scattering properties of the dust ejected by the impact compared to the dust released under normal conditions. Compared to the pre-impact state of the comet, we find evidence that the color of the comet was slightly bluer during the post-impact rise in brightness. Long after the impact, in the following nights, the comet colors returned to their pre-impact values. This can be explained by postulating a change to a smaller particle size distribution in the ejecta cloud, in agreement with the findings from mid-infrared observations, or by postulating a large fraction of clean ice particles, or by a combination of these two.     

Differential Rotation Driven by Precession

The tidal force in the Earth–Moon system exerted on the Earth's equatorial bulge results in the Earth's precession. It was proposed a long time ago that the strong shear flow driven by the precession of the Earth may power the Earth's dynamo in its liquid core. We present a nonlinear analytical study investigating how the Poincaré force in a rotating, precessing spherical system drives a large-amplitude differential rotation which plays a major role in the modern theory of the geodynamo. The analysis is based on a perturbation approach in terms of the small Poincaré force parameter. It is found that the amplitude of the precession-driven differential rotation is consistent with that estimated from the geomagnetic secular variation.     

On the fluid and viscoelastic deformations of the planets

The shape of the Earth and of planets depends on the exciting forces and on the rheology of the medium. From the equilibrium equation, we present the main modelisations of the viscous and inviscid fluids and we essentially describe the characteristics of linear viscoelastic deformations, for the Maxwell viscoelastic model of rheology. We use the elastic, viscoelastic and fluid Love numbers in order to investigate the associated relaxation modes. For these various kinds of rheology of the planets interior, we compute the geoid and the topography induced by an internal mass distribution. Finally, we show the importance of this viscoelastic deformation calculations in the study of the celestial body rotations.     

On the r-mode spectrum of relativistic stars in the low-frequency approximation

The axial modes for non-barotropic relativistic rotating neutron stars with uniform angular velocity are studied, using the slow-rotation formalism together with the low-frequency approximation, first investigated by Kojima. The time-independent form of the equations leads to a singular eigenvalue problem, which admits a continuous spectrum. We show that for     , it is nevertheless also possible to find discrete mode solutions (the r modes). However, under certain conditions related to the equation of state and the compactness of the stellar model, the eigenfrequency lies inside the continuous band and the associated velocity perturbation is divergent; hence these solutions have to be discarded as being unphysical. We corroborate our results by explicitly integrating the time-dependent equations. For stellar models admitting a physical r-mode solution, it can indeed be excited by arbitrary initial data. For models admitting only an unphysical mode solution, the evolutions do not show any tendency to oscillate with the respective frequency. For higher values of l it seems that in certain cases there are no mode solutions at all.