Astronomy and Astrophysics – Astronomy
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.6704r&link_type=abstract
American Astronomical Society Meeting 204, #67.04; Bulletin of the American Astronomical Society, Vol. 36, p.783
Astronomy and Astrophysics
Astronomy
Scientific paper
We present modeling results on the initiation and evolution of the coronal mass ejection which occurred on 1998 May 2 in NOAA AR8210. This is done within the framework of a global model of the solar magnetic field as it was observed by the Wilcox Solar Observatory. Our calculations are fully three-dimensional and involve compressible magnetohydrodynamics. We begin by first producing a steady-state solar wind for Carrington Rotation 1935/6. The solar eruption is initiated by slowly evolving the boundary conditions until a critical point is reached where the configuration loses mechanical equilibrium. As this point, the field erupts, and a flux rope is ejected away from the Sun, reaching a maximum speed in excess of 1,000 km/s. The shock that forms in front of the rope reaches a fast-mode Mach number in excess of 4 and a compression ratio greater than 3 by the time it has traveled a distance of 5 solar radii from the surface. Thus, by constructing a fully three-dimensional numerical model, which incorporates magnetic field data and a loss-of-equilibrium mechanism, we have been able to demonstrate that a shock can develop close to the Sun sufficiently strong to account for the energization of solar particles. For this event, diffusive-shock-acceleration theory predicts a distribution of solar energetic protons with a cut-off energy of about 10 GeV.
Forbes Terry G.
Gombosi Tamas I.
Lee Martin A.
Roussev Ilia I.
Sokolov Igor V.
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