Theoretical Investigations of Mechanisms for SolarEruptions

The book's main content is from Dr. Jun Lin'sdissertation submitted to the University of NewHampshire in partial fulfillment of the requirementsfor the PhD degree in physics in September 2001.Some theoretical models of solar eruptions derivedfrom previous works that involve a loss ofequilibrium of the coronal magnetic field arepresented. These models consist of a magnetic fluxrope nested within an arcade of magnetic loop.Before the eruption, the flux rope floats in thecorona under a balance between magnetic compressionand tension forces. When an eruption occurs, themagnetic compression exceeds the magnetic tensionand causes the flux rope to be thrown outwards, awayfrom the Sun. Three important factors which impactthe occurrence and evolution of the eruptiveprocesses are investigated. These factors aremagnetic reconnection, new emerging flux, and thelarge scale curvature of the flux rope. The resultssuggest that the catastrophic loss of equilibriumin the coronal magnetic configuration plays animportant role in triggering the eruption, andreconnection in the current sheet created by thecatastrophe helps the process to eveolve smoothly.

Autorentext

Degree: PhD in Physics
Major: Solar physics
Affiliation (since 2005):Yunnan Astronomical Observatory,
Email: jlin@ynao.ac.cn
B. S., Nanjing Univ., 1981
M. S., Nanjing UNiv., 1985
Ph. D., Univ. of New Hampshire, 2001
2001-2005, Harvard-Smithsonian CfA

Klappentext

The book's main content is from Dr. Jun Lin's
dissertation submitted to the University of New
Hampshire in partial fulfillment of the requirements
for the PhD degree in physics in September 2001.
Some theoretical models of solar eruptions derived
from previous works that involve a loss of
equilibrium of the coronal magnetic field are
presented. These models consist of a magnetic flux
rope nested within an arcade of magnetic loop.
Before the eruption, the flux rope floats in the
corona under a balance between magnetic compression
and tension forces. When an eruption occurs, the
magnetic compression exceeds the magnetic tension
and causes the flux rope to be thrown outwards, away
from the Sun. Three important factors which impact
the occurrence and evolution of the eruptive
processes are investigated. These factors are
magnetic reconnection, new emerging flux, and the
large scale curvature of the flux rope. The results
suggest that the catastrophic loss of equilibrium
in the coronal magnetic configuration plays an
important role in triggering the eruption, and
reconnection in the current sheet created by the
catastrophe helps the process to eveolve smoothly.