可拓学及其研究动态

文章对可拓学进行了简要的综述和介绍，阐述了可拓学的发展与当前的研究状况，提出了该领域研究中存在的问题，介绍了新的研究进展情况。     

GRB observed by IBIS/PICsIT in the MeV energy range

We present the preliminary results of a systematic search for GRB and other transients in the publicly available data for the IBIS/PICsIT (0.2–10 MeV) detector on board INTEGRAL. Lightcurves in 2–8 energy bands with time resolution from 1 to 62.5 ms have been collected and an analysis of spectral and temporal characteristics has been performed. This is the nucleus of a forthcoming first catalog of GRB observed by PICsIT.     

Formation of Giant Planets– An Attempt in Matching Observational Constraints

We present models of giant planet formation, taking into account migration and disk viscous evolution. We show that migration can significantly reduce the formation timescale bringing it in good agreement with typical observed disk lifetimes. We then present a model that produces a planet whose current location, core mass and total mass are comparable with the one of Jupiter. For this model, we calculate the enrichments in volatiles and compare them with the one measured by the Galileo probe. We show that our models can reproduce both the measured atmosphere enrichments and the constraints derived by Guillot et al. (2004), if we assume the accretion of planetesimals with ices/rocks ratio equal to 4, and that a substantial amount of CO₂ was present in vapor phase in the solar nebula, in agreement with ISM measurements.     

Dynamics of Coronal Loop Oscillations Recent Improvements and Computational Aspects

We will discuss the observed, heavily damped transversal oscillations of coronal loops. These oscillations are often modeled as transversal kink oscillations in a cylinder. Several features are added to the classical cylindrical model. In our models we include loop curvature, longitudinal density stratification, and highly inhomogeneous radial density profiles. In this paper, we will first give an overview of recently obtained results, both analytically and numerically. After that, we shed a light on the computational aspects of the modeling process. In particular, we will focus on the parallellization of the numerical codes.     

The Origin of Mercury’s Internal Magnetic Field

Mariner 10 measurements proved the existence of a large-scale internal magnetic field on Mercury. The observed field amplitude, however, is too weak to be compatible with typical convective planetary dynamos. The Lorentz force based on an extrapolation of Mariner 10 data to the dynamo region is 10⁻⁴ times smaller than the Coriolis force. This is at odds with the idea that planetary dynamos are thought to work in the so-called magnetostrophic regime, where Coriolis force and Lorentz force should be of comparable magnitude. Recent convective dynamo simulations reviewed here seem to resolve this caveat. We show that the available convective power indeed suffices to drive a magnetostrophic dynamo even when the heat flow though Mercury’s core–mantle boundary is subadiabatic, as suggested by thermal evolution models. Two possible causes are analyzed that could explain why the observations do not reflect a stronger internal field. First, toroidal magnetic fields can be strong but are confined to the conductive core, and second, the observations do not resolve potentially strong small-scale contributions. We review different dynamo simulations that promote either or both effects by (1) strongly driving convection, (2) assuming a particularly small inner core, or (3) assuming a very large inner core. These models still fall somewhat short of explaining the low amplitude of Mariner 10 observations, but the incorporation of an additional effect helps to reach this goal: The subadiabatic heat flow through Mercury’s core–mantle boundary may cause the outer part of the core to be stably stratified, which would largely exclude convective motions in this region. The magnetic field, which is small scale, strong, and very time dependent in the lower convective part of the core, must diffuse through the stagnant layer. Here, the electromagnetic skin effect filters out the more rapidly varying high-order contributions and mainly leaves behind the weaker and slower varying dipole and quadrupole components (Christensen in Nature 444:1056–1058, 2006). Messenger and BepiColombo data will allow us to discriminate between the various models in terms of the magnetic fields spatial structure, its degree of axisymmetry, and its secular variation.     

我校大学生心理健康状况不容乐观

本文用SCL－90症状自评量表方法，对我校三个年级的部分班级进行了测查。分析表明：我院大学生的心理健康状况不容乐观。本文还对学生管理现状提出了进一步改进建议。     

Line blanketed non-LTE atmosphere models for Wolf-Rayet stars

A standard non-LTE Wolf-Rayet star atmosphere model is compared with an identical model but including line-blanketing. The structures of the two models are presented in detail and the implications of blanketed models for spectroscopic analyses are discussed.     

企业应变能力及其传递矩阵研究

论述了企业应变能力的结构，内容及各层次间应变的特征，以应变能力在各责任单位之间的传递过程作了描述，用传递矩阵方法研究了应变能力在企业四个层次上的目标与保证关系，建立了一套实用的评价、诊断的定量指标体系。     

晚清修律对封建正统法律思想的改易

自汉朝以来，以儒家法律思想为主的封建正统法律思想在中国法律史上一直处于独尊独尚的地位。然而，清廷统治的最后十年，一场史无前例的变法修律，却首开吸收西方资产阶级法律思想入律之先河，第一次对封建正统法律思想的根本原则，基本内容等进行了突破、改易。尽管这些突破是有限的，但它足以表明晚清修律终于结束了两千多年来封建正统法律思想的垄断统治，终于使中国古代法律冲破了旧的樊篱，迈上了近现代型的历史轨道，为新的法律思想的发展完善开拓出了广阔的空间。     

“自准”赝像及识别

置平面镜于凸透镜后,则凸透镜前焦平面上的物成像于该物平面上,即“自准”成像.满足其它条件也能成像于物平面.分析不同条件下像的形成及其特点,并给出识别自准成像的判据.