Titlebook: Informatik — Wirtschaft — Gesellschaft; 23. GI — Jahrestagun Horst Reichel Conference proceedings 1993 Springer-Verlag Berlin Heidelberg 19

银河

书目名称Informatik — Wirtschaft — Gesellschaft影响因子(影响力)




书目名称Informatik — Wirtschaft — Gesellschaft影响因子(影响力)学科排名




书目名称Informatik — Wirtschaft — Gesellschaft网络公开度




书目名称Informatik — Wirtschaft — Gesellschaft网络公开度学科排名




书目名称Informatik — Wirtschaft — Gesellschaft被引频次




书目名称Informatik — Wirtschaft — Gesellschaft被引频次学科排名




书目名称Informatik — Wirtschaft — Gesellschaft年度引用




书目名称Informatik — Wirtschaft — Gesellschaft年度引用学科排名




书目名称Informatik — Wirtschaft — Gesellschaft读者反馈




书目名称Informatik — Wirtschaft — Gesellschaft读者反馈学科排名

会犯错误

passively, in virtually all coronal disturbances. The purpose of this paper is to put into perspective the various roles magnetic fields can play in both exciting and guiding these observed transient phenomena. A discussion of our present theoretical concepts relevant to this subject can be convenie

法官

B. Shriversisted of A. Boischot, A. Bruzek, J. T. Jefferies, G. Newkirk, T. Takakura, and V. V. Zhelez­ nyakov. We are indebted to the Local Organizing Commettee, chaired by S. F. Smerd and including R. G. Giovanelli, R. E. Loughhead, N. G. Seddon, K. V. Sheridan, and J. P. Wild, for advice in preparing this

Cognizance

W. Wahlster observations con­ firmed the basic validity of a theoretical model, first proposed by E. N. Parker, predicting a continuous, rapid expansion of the solar corona. The subsequent decade has seen a tremendous growth in both the breadth and sophistication of solar wind observations; the properties of t

进步

Klaus Lenky discussion of the physics of the interplanetary plasma. We have already seen that the models of Parker, based on the assumption of steady, spherically-symmetric fluid motion, correctly predicted the basic characteristics of the solar wind. The adoption of this same simplifying assumption in the fo

intellect

Insensate

Britta Schinzelobservations, which contain a last part of the maximum phase of the solar cycle 22, it was possible to obtain almost every aspect of solar activity at 17 GHz. They include two X-class flares, tens of M-class flares, hundreds of flares from the very initial phase through the late decay phase, or from

Accede

Frieder Nakeobservations, which contain a last part of the maximum phase of the solar cycle 22, it was possible to obtain almost every aspect of solar activity at 17 GHz. They include two X-class flares, tens of M-class flares, hundreds of flares from the very initial phase through the late decay phase, or from

正式通知

EREO/COR1 data obtained during a deep minimum of solar activity in February 2008 (Carrington Rotation CR 2066) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from 1.5 to 4 R. using a tomography method. With this, we qualitatively deduced structure

leniency