Flux cancellation and coronal mass ejections

Time dependent magnetohydrodynamic computations of the flux cancellation mechanism are presented. Previous authors have discussed this mechanism as a possible cause for the formation of prominences and the trigger for prominence eruptions and coronal mass ejections (CMEs). This paper shows that flux cancellation in an energized two-and-one-half-dimensional helmet streamer configuration first leads to the formation of stable flux rope structures. When a critical threshold of flux reduction is exceeded, the configuration erupts violently. Significant amounts of stored magnetic energy are released through magnetic reconnection. The ejected flux rope propagates out into the solar wind and forms an interplanetary shock wave. A similar eruption occurs for a three-dimensional calculation where the ends of the flux rope field lines are anchored to the Sun. The flux cancellation mechanism unifies the processes of prominence formation, prominence eruption, and CME initiation, and thus provides an attractive hypothesis for explaining the cause of these dynamic events.Time dependent magnetohydrodynamic computations of the flux cancellation mechanism are presented. Previous authors have discussed this mechanism as a possible cause for the formation of prominences and the trigger for prominence eruptions and coronal mass ejections (CMEs). This paper shows that flux cancellation in an energized two-and-one-half-dimensional helmet streamer configuration first leads to the formation of stable flux rope structures. When a critical threshold of flux reduction is exceeded, the configuration erupts violently. Significant amounts of stored magnetic energy are released through magnetic reconnection. The ejected flux rope propagates out into the solar wind and forms an interplanetary shock wave. A similar eruption occurs for a three-dimensional calculation where the ends of the flux rope field lines are anchored to the Sun. The flux cancellation mechanism unifies the processes of prominence formation, prominence eruption, and CME initiation, and thus provides an attractive hypothe...

[1]  Petrus C. H. Martens,et al.  Formation and eruption of solar prominences , 1989 .

[2]  J. Linker,et al.  Magnetohydrodynamic modeling of prominence formation within a helmet streamer , 2001 .

[3]  R. Tousey.  First Results from Skylab. , 1973 .

[4]  A. Hundhausen,et al.  Sizes and locations of coronal mass ejections - SMM observations from 1980 and 1984-1989 , 1993 .

[5]  A. Hundhausen.  Coronal Mass Ejections , 1997 .

[6]  J. Aly.  How much energy can be stored in a three-dimensional force-free magnetic field? , 1991 .

[7]  M. Kundu,et al.  Radio Physics of the Sun , 1980 .

[8]  Bernhard Haisch,et al.  Nonpotential features observed in the magnetic field of an active region , 1987 .

[9]  E. Hildner,et al.  The outer solar corona as observed from Skylab - Preliminary results , 1974 .

[10]  L. Driel-Gesztelyi,et al.  What is the source of the magnetic helicity shed by CMEs? The long-term helicity budget of AR 7978 , 2002 .

[11]  A. Hundhausen,et al.  Observation of a coronal transient from 1.2 to 6 solar radii , 1985 .

[12]  J. Aly.  On some properties of force-free magnetic fields in infinite regions of space , 1984 .

[13]  T. Forbes,et al.  A catastrophe mechanism for coronal mass ejections , 1991 .

[14]  J. Linker,et al.  Disruption of a helmet streamer by photospheric shear , 1995 .

[15]  J. Linker,et al.  Stability of Algorithms for Waves with Large Flows , 1999 .

[16]  T. Forbes.  A review on the genesis of coronal mass ejections , 2000 .

[17]  E. Priest,et al.  On the maximum energy release in flux-rope models of Eruptive Flares , 1994 .

[18]  B. Low.  Coronal mass ejections, magnetic flux ropes, and solar magnetism , 2001 .

[19]  P. Lamy,et al.  The Large Angle Spectroscopic Coronagraph (LASCO) , 1995 .

[20]  M. Hagyard.  Observed nonpotential magnetic fields and the inferred flow of electric currents at a location of repeated flaring , 1987 .

[21]  R. Canfield,et al.  The morphology of flare phenomena, magnetic fields, and electric currents in active regions. I - Introduction and methods , 1993 .

[22]  D. Schnack,et al.  Magnetohydrodynamic modeling of the global solar corona , 1999 .

[23]  R. E. Marshak,et al.  Interplanetary Dynamical Processes , 1963 .

[24]  R. Canfield,et al.  The morphology of flare phenomena, magnetic fields, and electric currents in active regions. II: NOAA active region 5747 (1989 october) , 1993 .

[25]  Jon A. Linker,et al.  Disruption of Coronal Magnetic Field Arcades , 1994 .

[26]  J. Linker,et al.  Magnetohydrodynamic modeling of the solar corona during Whole Sun Month , 1999 .

[27]  Carolus J. Schrijver,et al.  Solar surface magnetism , 1994 .

[28]  J. Luciani,et al.  A Twisted Flux Rope Model for Coronal Mass Ejections and Two-Ribbon Flares , 2000, The Astrophysical journal.

[29]  S. Martin,et al.  The cancellation of magnetic flux. II - In a decaying active region , 1985 .

[30]  J. Linker,et al.  Including the Transition Region in Models of the Large-Scale Solar Corona , 2001 .

[31]  P. Démoulin,et al.  The Effect of Curvature on Flux-Rope Models of Coronal Mass Ejections , 1998 .

[32]  E. Hildner,et al.  The High Altitude Observatory Coronagraph/Polarimeter on the Solar Maximum Mission , 1980 .

[33]  S. Antiochos.  The magnetic topology of solar eruptions , 1998, astro-ph/9806030.

[34]  The Dynamic Formation of Prominence Condensations , 1998, astro-ph/9808199.

[35]  J. Linker,et al.  Magnetic Field Topology in Prominences , 2002 .