Hostname: page-component-745bb68f8f-d8cs5 Total loading time: 0 Render date: 2025-01-13T05:54:58.625Z Has data issue: false hasContentIssue false
  • English
  • Français

Properties of Magnetohydrodynamic Turbulence in the Solar Wind

Published online by Cambridge University Press:  14 August 2015

M. Dobrowolny ,
A. Mangeney  and
P.L. Veltri
M. Dobrowolny
Affiliation:
(Laboratorio Plasma Spazio, CNR, Frascati, Italy)
A. Mangeney
Affiliation:
(Observatoire de Meudon, Paris, France)
P.L. Veltri
Affiliation:
(Dipartimento di Fisica, Università della Calabria, Italy)

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

The observations of MHD turbulence in the solar wind indicate that this is in a state characterized, to a good degree by the absence of non linear interactions. It is argued that this is a general property of incompressible MHD turbulence in a magnetized plasma.

Type
Part II. Coronal and Interplanetary Responses to Long Time Scale Phenomena
Information
Symposium - International Astronomical Union , Volume 91: Solar and Interplanetary Dynamics , 1980 , pp. 143 - 146
Copyright
Copyright © Reidel 1980 

References

Belcher, J.W., and Davis, L.: 1971, J. Geophys. Res. 76, pp. 3534–3563.CrossRefGoogle Scholar
Burlaga, L.F. and Turner, J.M.: 1976, J. Geophys. Res. 81, pp. 73–77.CrossRefGoogle Scholar
Dobrowolny, M., Mangeney, A. and Veltri, P.L.: 1979, to be published in Astron. and Astrophys.Google Scholar
Hollweg, J.V.: 1978, Solar Phys. 56, pp. 305–333.CrossRefGoogle Scholar
Kraichnan, R.H.: 1965, Phys. of Fluids 8, pp. 1385–1387.CrossRefGoogle Scholar
Osterbrock, D.E.: 1961, Astrophys. J. 134, pp. 347–388.CrossRefGoogle Scholar