Acceleration of the solar wind: effects of plasmoids

Details Acceleration of the solar wind: effects of plasmoids Acceleration of the solar wind: effects of plasmoids

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..385..205m&link_type=abstract

Scientific basis for robotic exploration close to the sun. AIP Conference Proceedings, Volume 385, pp. 205-210 (1997).

Other

Particle Emission, Solar Wind, Solar Wind Plasma, Sources Of Solar Wind, Magnetohydrodynamics And Plasmas

Scientific paper

Magnetic plasmoids in the solar corona and wind are subject to outward Lorentz forces in regions where the ambient magnetic field is decreasing outwards. We compute velocity profiles V(r) for a spherically symmetric solar wind containing plasmoids. In regions where the plasmoids occupy a progressively larger fraction of the solar wind, the wind accelerates rapidly, with radial gradients as much as 4-5 times steeper than the maximum gradient in an isothermal wind. Reconnection causes plasmoids eventually to lose their identity, and when the plasmoid fraction becomes small, the velocity profile becomes almost flat, with radial gradients shallower than in the isothermal wind by factors of about 2.

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