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Acceleration of the Solar Wind: A New View

Published online by Cambridge University Press:  14 August 2015

V.H. Hansteen  and
E. Leer
V.H. Hansteen
Affiliation:
Institute of Theoretical AstrophysicsPB 1029 Blindern, 0315 Oslo, Norway
E. Leer
Affiliation:
Institute of Theoretical AstrophysicsPB 1029 Blindern, 0315 Oslo, Norway

Extract

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The last few years have seen the development of solar wind models characterized by high coronal proton temperatures, low electron temperatures and low densities in the inner corona. In addition the emphasis on “additional” acceleration via Alfvén waves has been muted and been replaced by models where the acceleration is essentially complete within 1OR0. This work has, in part, been spurred by Ulysses observations of the high speed wind and by the expectations of the observations to be made by the various instruments on the SOHO satellite. In this paper we show how these new models differ from earlier ones.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 2: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part B), 1997 , 1998 , pp. 838 - 841
Copyright
Copyright © Kluwer 1998

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