Ejection of magnetic fields from the sun - Acceleration of a solar wind containing diamagnetic plasmoids

Details Ejection of magnetic fields from the sun - Acceleration of a solar wind containing diamagnetic plasmoids Ejection of magnetic fields from the sun - Acceleration of a solar wind containing diamagnetic plasmoids

Feb 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...265..468p&link_type=abstract

Astrophysical Journal, Part 1, vol. 265, Feb. 1, 1983, p. 468-482.

Astronomy and Astrophysics

Astrophysics

61

Diamagnetism, Magnetohydrodynamics, Solar Magnetic Field, Solar Wind, Gas Pressure, Magnetic Field Configurations, Solar Corona, Solar X-Rays, Ultraviolet Spectra

Scientific paper

A solar wind model that uses magnetic fields expelled by small-scale magnetic reconnection as a driving force in addition to that provided by the gas pressure is developed. The occurrence of reconnection is postulated as a mechanism for expelling magnetic flux brought up through the solar surface as suggested by the X-ray bright points and explosive events in the transition region as observed by Brueckner (1980). For an elliptical bubble, it is shown that the net force exerted by the magnetic field assumes a particularly simple form depending only on the plasmoid's temperature, its mass, and the radial gradient of the logarithm of the undisturbed ambient field strength. It is also found that as the percentage of the total mass flux carried by the diamagnetic component is increased, the velocity of the wind is correspondingly increased significantly. It is believed that this effect could be important in explaining the high velocities at 1 AU observed in the high-speed streams.

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