基于活动网络图的工作流建模工具的设计与实现

在描述工作流过程的模型中,基于活动网络图工作流模型的可读性最好。它对于工作流过程的描述非常直观,是最自然的过程表达方式。本文首先分析了工作流管理联盟(WfMC)提出的工作流过程定义的元模型,然后给出了一种基于活动网络图的工作流过程模型,并采用面向对象的程序设计方法,完成了工作流过程建模工具的开发。     

面向人机交互式软件的测试模型建模方法

从测试用例自动生成和自动执行的角度来探讨如何对人机交互软件建立测试模型。采用UML活动图模型来描述软件的人机交互过程。为了能够从活动图模型中生成一组确定的可执行的测试用例，给出了一组规则来细化基于活动图的测试模型所表达的语义，同时也对活动图做了一些扩展，以支持基于模型的测试用例自动生成及其自动执行。给出的建模方法，能够减少某些冗余的测试用例。     

浅谈实施作业管理的意义和效果

对实施作业管理的意义和效果进行阐述。指出作业管理可使企业产品成本信息更为准确，并有利于提高生产效率，降低库存，有利于企业资源的优化配置和战略发展。     

Closing address

Impressions from the workshop are summarized. Difficulties within the present observational and theoretical context are outlined and directions for fruitful future work are indicated. The workshop subtitle, the interface between MHD and plasma physics, still appears to be a goal for the future, though some encouraging results have been reported at this workshop.     

1996-2002年太阳耀斑的统计分析

分析了1996-2002年南北半球的太阳黑子相对数和南北半球太阳X射线耀斑级别(简称Imp)≥M1．0的太阳X射线耀斑的特征和不对称性．分析结果表明，南北半球的太阳耀斑活动的程度交替上升，在2001年7月以前北半球的太阳耀斑活动强于南半球，2001年7月开始耀斑活动逐渐以南半球为主．本文还逐月分析了1996—2001年南北半球的耀斑指数．2000年7月为第23周太阳指数最大的一个月，与第23周太阳黑子相对数最大月均值吻合．     

太阳活动对EUV辐射在大气中吸收过程的影响

本文利用A-E卫星在太阳活动21周峰年间观测到的EUV辐射资料,高层大气成分的吸收截面,以及MSIS-86热层大气模式,研究了EUV辐射在大气中的吸收过程;在透射比为1/e和0.1/100时分别计算了透射高度随波长及太阳活动的变化。在波长范围50—1050内对37个波段分别求出了透射高度随太阳天顶角的变化。结果表明,当太阳活动增强时各波段的透射高度均升高,而且透射比越大则透射高度随太阳活动的变化也越剧烈。当透射比为一定时,太阳天顶角越大则透射高度随太阳活动的变化也越大。除此之外还存在一个相反效应,即太阳活动会使Chapman函数变小,这反过来又促使透射高度降低。这两种效应的综合作用结果可较好地解释某些电离层观测中的日没效应。     

“Oblique” Bernstein modes in solar preflare plasma: Generation of second harmonics

Process of second harmonics generation due to development of corresponding instability has been investigated for pure electron weakly oblique Bernstein mode. This mode was supposed to be modified by taking into account the influence of pair Coulomb collisions and weak large-scale electric field in flare loop. Investigated area was located near the loop foot-point in the “lower–middle” chromosphere of active region. It has been shown, that for the Fontenla–Avrett–Loeser model of solar atmosphere the investigated process of second harmonics generation starts at the extremely low threshold values of subdreicer electric field, well before the beginning of “preheating” phase of flare process.     

The relationship between inductive electric field and flares

We observationally deduce the inductive electric field in the photosphere for the first time from the horizontal velocities computed by local correlation tracking (LCT) technique and the vector magnetic fields derived from vector magnetograms. We study the relationship between E and powerful flares (X-class) of four active regions (ARs): NOAA 10720, 10486, 9077 and 8100. It is found that the kernels of flares are roughly located near the inversion lines where maxima of E are observed. Our results show that E relates to the accumulation of non-potentiality in the photosphere and the transportation of non-potentiality from the photosphere to the corona.