社会关系嵌入与产业转移的区位选择——宁波服装业案例研究

从企业社会关系网络嵌入的视角,以宁波服装企业和机构为访谈调研对象,追寻众多宁波服装企业早期发展的历史,研究上海与宁波两地基于历史原因形成的社会关系嵌入——"红帮师傅"对上海服装业转移中区位选择的影响。研究发现,上海国有服装企业中宁波籍"红帮师傅",是理解上海服装企业在向外转移加工业务的过程中为何选择宁波服装企业的关键因素。在宁波服装业的早期发展阶段,"红帮师傅"充当了宁波服装企业与上海服装企业建立业务联系的桥梁,不仅将自己所在服装企业的加工业务介绍给宁波的服装企业,还利用自己的社会网络,将上海其它服装企业引荐给宁波服装企业,使宁波服装企业从上海获得了大量的加工业务。另外,"红帮师傅"还亲自或引荐其它服装技师为宁波的服装企业提供必要的技术指导。对理解非经济因素对产业转移区位选择的影响提供了一个有意义的实证案例,为欠发达地区吸引发达地区的产业转移提供了一种新的思路。     

郑州承接产业转移示范区机制创新研究

郑州市积极承接产业转移对于加快郑州都市区建设、打造中原经济区核心增长极、充分发挥郑州引领区域发展的重心作用、强化郑州的龙头作用和示范带动作用、提升郑州全国区域性中心城市地位具有重大战略意义。目前郑州市承接产业转移还存在着一系列深层次矛盾和突出问题,需要进一步机制创新,加快郑州承接产业转移示范区建设。     

河南省打造内陆开放高地研究

从河南省对外开放态势入手,较详细地分析了近年来尤其是"十一五"期间外部因素对河南省经济发展所起到的促进作用。在此基础上,结合中原经济区建设的新形势,提出为了更好地利用外部因素,需要打造内陆开放高地。根据河南省的优势,河南省内陆开放高地的打造应从以下几个方面展开:承接产业转移,形成产业集聚高地;加快综合保税区建设,形成开放制度创新高地;提高外资利用质量,形成利用外资高地;打造服务外包示范城市,形成服务外包高地。     

产业有序转移与区域产业协调发展——基于广东产业有序转移的经验

阐明了产业有序转移、区域产业协调发展的内涵,构建了产业有序转移对区域产业协调发展作用机制的分析框架。根据这个分析框架,从理论和广东产业转移经验两个方面进一步揭示了产业有序转移促进区域产业协调发展的机制。结果表明,产业有序转移是在政府有效干预下所形成的有利于区域产业协调发展的一种产业转移形式。产业有序转移通过诱致或促进区域产业结构优化调整、区际产业合理分工、区际产业关联互动,以及提高区域产业发展总体效率等路径,促进区域产业协调发展。     

基于全球转移的乐器制造业价值链空间分布——以钢琴制造业为例

作为一个发展成熟的全球性产业,乐器制造业也正经历着快速的发展和演变。鉴于作为乐器之王的钢琴在乐器中的地位,本文以钢琴为例,研究全球乐器产业的转移及价值活动分布。研究认为,钢琴制造业了5次全球转移,即西欧内部的转移、由欧洲向美国的转移、由美国向西欧和日本的转移、由日本向东亚的转移和由韩国向东亚的转移,形成了当前的全球价值分布格局,即全球钢琴制造业价值量分布整体上呈现阶梯状分布的格局,以欧美为第一阶梯,日本和韩国为第二阶梯,中国为第三阶梯。在研发、核心产品设计及品牌等的核心竞争力上表现更是如此。基于上述研究,论文最后对我国的乐器制造业发展提出了一些思考。     

Analysis of thermal emission from the nightside of Venus at 1.51 and 1.55 μm

We present radiative transfer modelling of thermal emission from the nightside of Venus in two ‘spectral window’ regions at 1.51 and 1.55 μm. The first discovery of these windows, reported by Erard et al. [Erard, S., Drossart, P., Piccioni, G., 2009. J. Geophys. Res. Planets 114, doi:10.1029/2008JE003116. E00B27], was achieved using a principal component analysis of data from the VIRTIS instrument on Venus Express. These windows are spectrally narrow, with a full-width at half-maximum of ∼20 nm, and less bright than the well-known 1.7 and 2.3 μm spectral windows by two orders of magnitude.In this note we present the first radiative transfer analysis of these windows. We conclude that the radiation in these windows originates at an altitude of 20-35 km. As is the case for the other infrared window regions, the brightness of the windows is affected primarily by the optical depth of the overlying clouds; in addition, the 1.51 μm radiance shows a very weak sensitivity to water vapour abundance.     

Effects of scattering and dust grain size on the temperature structure of protoplanetary discs: a three-layer approach

The temperature in the optically thick interior of protoplanetary discs is essential for the interpretation of millimetre observations of the discs, for the vertical structure of the discs, for models of the disc evolution and the planet formation, and for the chemistry in the discs. Since large icy grains have a large albedo even in the infrared, the effect of scattering of the diffuse radiation in the discs on the interior temperature should be examined. We have performed a series of numerical radiation transfer simulations, including isotropic scattering by grains with various typical sizes for the diffuse radiation as well as for the incident stellar radiation. We also have developed an analytic model including isotropic scattering to understand the physics concealed in the numerical results. With the analytic model, we have shown that the standard two-layer approach is valid only for grey opacity (i.e. grain size ≳10 μm) even without scattering. A three-layer interpretation is required for grain size ≲10 μm. When the grain size is 0.1–10 μm, the numerical simulations show that the isotropic scattering reduces the temperature of the disc interior. This reduction is nicely explained by the analytic three-layer model as a result of the energy loss by scatterings of the incident stellar radiation and of the warm diffuse radiation in the disc atmosphere. For grain size ≳10 μm (i.e. grey scattering), the numerical simulations show that the isotropic scattering does not affect the interior temperature. This is nicely explained by the analytic two-layer model; the energy loss by scattering in the disc atmosphere is exactly offset by the 'green-house effect' due to the scattering of the cold diffuse radiation in the interior.     

Introducing a hybrid radiative transfer method for smoothed particle hydrodynamics

A new means of incorporating radiative transfer into smoothed particle hydrodynamics (SPH) is introduced, which builds on the success of two previous methods – the polytropic cooling approximation as devised by Stamatellos et al. and flux-limited diffusion. This hybrid method preserves the strengths of its individual components, while removing the need for atmosphere matching or other boundary conditions to marry optically thick and optically thin regions. The code uses a non-trivial equation of state to calculate temperatures and opacities of SPH particles, which captures the effects of H₂ dissociation, H⁰ ionization, He⁰ and He⁺ ionization, ice evaporation, dust sublimation, molecular absorption, bound-free and free–free transitions and electron scattering. The method is tested in several scenarios, including (i) the evolution of a  0.07 M_⊙  protoplanetary disc surrounding a  0.5 M_⊙  star; (ii) the collapse of a  1 M_⊙  protostellar cloud and (iii) the thermal relaxation of temperature fluctuations in a static homogeneous sphere.     

SN 1994W: an interacting supernova or two interacting shells?

We present a multi-epoch quantitative spectroscopic analysis of the Type IIn supernova (Type IIn SN) 1994W, an event interpreted by Chugai et al. as stemming from the interaction between the ejecta of a SN and a  0.4 M_⊙  circumstellar shell ejected 1.5 yr before core collapse. During the brightening phase, our models suggest that the source of optical radiation is not unique, perhaps associated with an inner optically thick cold dense shell and outer optically thin shocked material. During the fading phase, our models support a single source of radiation, an hydrogen-rich optically thick layer with a near-constant temperature of ∼7000 K that recedes from a radius of  4.3 × 10¹⁵  at a peak to  2.3 × 10¹⁵ cm  40 d later. We reproduce the hybrid narrow-core broad-wing line profile shapes of SN 1994W at all times, invoking an optically thick photosphere exclusively (i.e. without any external optically thick shell). In SN 1994W, slow expansion makes scattering with thermal electrons a key escape mechanism for photons trapped in optically thick line cores, and allows the resulting broad incoherent electron-scattering wings to be seen around narrow-line cores. In SNe with larger expansion velocities, the thermal broadening due to incoherent scattering is masked by the broad profile and the dominant frequency redshift occasioned by bulk motions. Given the absence of broad lines at all times and the very low ⁵⁶Ni yields, we speculate whether SN 1994W could have resulted from an interaction between two ejected shells without core collapse. The high conversion efficiency of kinetic to thermal energy may not require a SN-like energy budget for SN1994W.