Dynamical evolution of a coronal streamer-bubble system. 1: A self-consistent planar magnetohydrodynamic simulation

Details Dynamical evolution of a coronal streamer-bubble system. 1: A self-consistent planar magnetohydrodynamic simulation Dynamical evolution of a coronal streamer-bubble system. 1: A self-consistent planar magnetohydrodynamic simulation

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..157..325w&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 157, no. 1-2, p. 325-248

Physics

49

Magnetohydrodynamics, Simulation, Size Distribution, Solar Corona, Solar Magnetic Field, Solar Physics, Sun, Bubbles, Mathematical Models, Nonequilibrium Flow, Quasi-Steady States, Time Dependence

Scientific paper

We present a self-consistent, time-dependent magnetohydrodynamic (MHD) description of a dipolar configuration helmet streamer in which a magnetic bubble structure has been introduced into the closed field region of the helmet streamer. A numerical model is used to study the magnetohydrodynamic evolution of this streamer- bubble system. We find two distinct behaviors characterized by the size of the magnetic bubble: (1) if the bubble's radius is less than or equal to 0.15 Rc (where Rc is the characteristic length of the helmet streamer), the numerical solution describes a quasi-equilibrium state, and this coronal streamer-bubble structure is stable; and (2) if the bubble's radius is equal to or larger than 0.25 Rc, the numerical solution describes a non-equilibrium state and, after a period of slow evolution, this coronal streamer bubble structure becomes unstable and breaks up dynamically. In the case of the dipolar configuration helmet streamer, Rc is the solar radius. We identify the non-equilibrium solution as a loss of equilibrium of this coronal magnetic structure. Its subsequent dynamic development may be a candidate for some of the commonly observed coronal mass ejections (CMEs).

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