The deformation of flux tubes in the solar wind with applications to the structure of magnetic clouds and CMEsTwo dimensional magnetohydrodynamic simulations of the distortion of a magnetic flux tube, accelerated through ambient solar wind plasma, are presented. Vortices form on the trailing edge of the flux tube, and couple strongly to its interior. If the flux tube azimuthal field is weak, it deforms into an elongated banana-like shape after a few Alfven transit times. A significant azimuthal field component inhibits this distortion. In the case of magnetic clouds in the solar wind, it is suggested that the shape observed at 1 AU was determined by distortion of the cloud in the inner heliosphere. Distortion of the cloud beyond 1 AU takes many days. It is estimated that effective drag coefficients slightly greater than unity are appropriate for modeling flux tube propagation. Synthetic magnetic field profiles as would be seen by a spacecraft traversing the cloud are presented.
Document ID
19950025496
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Cargill, Peter J. (Naval Research Lab. Washington, DC., United States)
Chen, James (Naval Research Lab. Washington, DC., United States)
Spicer, D. S. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Zalesak, S. T. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 16, 2013
Publication Date
December 1, 1994
Publication Information
Publication: ESA, Proceedings of 3rd SOHO Workshop on Solar Dynamic Phenomena and Solar Wind Consequences